text:
@article{dekleerIoVolcanicActivity2019,
	title = {Io’s {Volcanic} {Activity} from {Time} {Domain} {Adaptive} {Optics} {Observations}: 2013–2018},
	volume = {158},
	issn = {1538-3881},
	shorttitle = {Io’s {Volcanic} {Activity} from {Time} {Domain} {Adaptive} {Optics} {Observations}},
	url = {https://iopscience.iop.org/article/10.3847/1538-3881/ab2380},
	doi = {10.3847/1538-3881/ab2380},
	abstract = {We present measurements of the near-infrared brightness of Io’s hot spots derived from 2 to 5 μm imaging with adaptive optics on the Keck and Gemini N telescopes. The data were obtained on 271 nights between 2013 August and the end of 2018, and include nearly 1000 detections of over 75 unique hot spots. The 100 observations obtained between 2013 and 2015 have been previously published in de Kleer \& de Pater the observations since the start of 2016 are presented here for the ﬁrst time, and the analysis is updated to include the full ﬁve-year data set. These data provide insight into the global properties of Io’s volcanism. Several new hot spots and bright eruptions have been detected, and the preference for bright eruptions to occur on Io’s trailing hemisphere noted in the 2013–2015 data is strengthened by the larger data set and remains unexplained. The program overlapped in time with Sprint-A/EXCEED and Juno observations of the Jovian system, and correlations with transient phenomena seen in other components of the system have the potential to inform our understanding of the impact of Io’s volcanism on Jupiter and its neutral/plasma environment.},
	language = {en},
	number = {1},
	urldate = {2019-07-31},
	journal = {AJ},
	author = {de Kleer, Katherine and de Pater, Imke and Molter, Edward M. and Banks, Elizabeth and Davies, Ashley Gerard and Alvarez, Carlos and Campbell, Randy and Aycock, Joel and Pelletier, John and Stickel, Terry and Kacprzak, Glenn G. and Nielsen, Nikole M. and Stern, Daniel and Tollefson, Joshua},
	month = jun,
	year = {2019},
	pages = {29},
	file = {de Kleer et al. - 2019 - Io’s Volcanic Activity from Time Domain Adaptive O.pdf:/Users/fb90/Zotero/storage/ESFNTPFK/de Kleer et al. - 2019 - Io’s Volcanic Activity from Time Domain Adaptive O.pdf:application/pdf;de Kleer et al. - 2019 - Io’s Volcanic Activity from Time Domain Adaptive O.pdf:/Users/fb90/Zotero/storage/YZGX35DM/de Kleer et al. - 2019 - Io’s Volcanic Activity from Time Domain Adaptive O.pdf:application/pdf}
}

@inproceedings{oren1994,
	address = {New York, NY, USA},
	series = {{SIGGRAPH} '94},
	title = {Generalization of {Lambert}'s reflectance model},
	isbn = {978-0-89791-667-7},
	url = {https://doi.org/10.1145/192161.192213},
	doi = {10.1145/192161.192213},
	abstract = {Lambert's model for body reflection is widely used in computer graphics. It is used extensively by rendering techniques such as radiosity and ray tracing. For several real-world objects, however, Lambert's model can prove to be a very inaccurate approximation to the body reflectance. While the brightness of a Lambertian surface is independent of viewing direction, that of a rough surface increases as the viewing direction approaches the light source direction. In this paper, a comprehensive model is developed that predicts body reflectance from rough surfaces. The surface is modeled as a collection of Lambertian facets. It is shown that such a surface is inherently non-Lambertian due to the foreshortening of the surface facets. Further, the model accounts for complex geometric and radiometric phenomena such as masking, shadowing, and interreflections between facets. Several experiments have been conducted on samples of rough diffuse surfaces, such as, plaster, sand, clay, and cloth. All these surface demonstrate significant deviation from Lambertian behavior. The reflectance measurements obtained are in strong agreement with the reflectance predicted by the model.},
	urldate = {2020-02-05},
	booktitle = {Proceedings of the 21st annual conference on {Computer} graphics and interactive techniques},
	publisher = {Association for Computing Machinery},
	author = {Oren, Michael and Nayar, Shree K.},
	month = jul,
	year = {1994},
	keywords = {BRDF, Lambert's model, moon reflectance, reflection models, rough surfaces},
	pages = {239--246},
	file = {Oren and Nayar - 1994 - Generalization of Lambert's reflectance model.pdf:/Users/fb90/Zotero/storage/22TP8PKG/Oren and Nayar - 1994 - Generalization of Lambert's reflectance model.pdf:application/pdf}
}

@article{mallama1991,
	title = {Light curve model for the {Galilean} satellites during {Jovian} eclipse},
	volume = {92},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/001910359190055X},
	doi = {10.1016/0019-1035(91)90055-X},
	language = {en},
	number = {2},
	urldate = {2020-02-05},
	journal = {Icarus},
	author = {Mallama, Anthony},
	month = aug,
	year = {1991},
	pages = {324--331},
	file = {Mallama - 1991 - Light curve model for the Galilean satellites duri.pdf:/Users/fb90/Zotero/storage/V4XCMCVX/Mallama - 1991 - Light curve model for the Galilean satellites duri.pdf:application/pdf}
}

@misc{zotero-3174,
	title = {The 2014-2015 {Brazilian} mutual phenomena campaign for the {Jovian} satellites and improved results for the 2009 events {\textbar} {Elsevier} {Enhanced} {Reader}},
	url = {https://reader.elsevier.com/reader/sd/pii/S0032063319302880?token=512CC56B066268D2B29C519A9928247C630FBAD67D846586BF542794387BCB7AAED569458B5253367CFE78E3752AA170},
	language = {en},
	urldate = {2020-02-05},
	doi = {10.1016/j.pss.2019.104736},
	file = {Snapshot:/Users/fb90/Zotero/storage/7PTZRZG8/S0032063319302880.html:text/html;The 2014-2015 Brazilian mutual phenomena campaign .pdf:/Users/fb90/Zotero/storage/RKKSYVD4/The 2014-2015 Brazilian mutual phenomena campaign .pdf:application/pdf}
}

@article{arlot2014,
	title = {The {PHEMU09} catalogue and astrometric results of the observations of the mutual occultations and eclipses of the {Galilean} satellites of {Jupiter} made in 2009},
	volume = {572},
	issn = {0004-6361, 1432-0746},
	url = {http://www.aanda.org/10.1051/0004-6361/201423854},
	doi = {10.1051/0004-6361/201423854},
	abstract = {Context. In 2009, the Sun and the Earth passed through the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. It was the equinox on Jupiter. This occurrence made mutual occultations and eclipses between the satellites possible. Experience has shown that the observations of such events provide accurate astrometric data able to bring new information on the dynamics of the Galilean satellites. Observations are made under the form of photometric measurements, but need to be made through the organization of a worldwide observation campaign maximizing the number and the quality of the data obtained.},
	language = {en},
	urldate = {2020-02-05},
	journal = {A\&A},
	author = {Arlot, J.-E. and Emelyanov, N. and Varfolomeev, M. I. and Amossé, A. and Arena, C. and Assafin, M. and Barbieri, L. and Bolzoni, S. and Bragas-Ribas, F. and Camargo, J. I. B. and Casarramona, F. and Casas, R. and Christou, A. and Colas, F. and Collard, A. and Combe, S. and Constantinescu, M. and Dangl, G. and De Cat, P. and Degenhardt, S. and Delcroix, M. and Dias-Oliveira, A. and Dourneau, G. and Douvris, A. and Druon, C. and Ellington, C. K. and Estraviz, G. and Farissier, P. and Farmakopoulos, A. and Garlitz, J. and Gault, D. and George, T. and Gorda, S. Yu. and Grismore, J. and Guo, D. F. and Herald, D. and Ida, M. and Ishida, M. and Ivanov, A. V. and Klemt, B. and Koshkin, N. and Le Campion, J. F. and Liakos, A. and Liao, S. L. and Li, S. N. and Loader, B. and Lopresti, C. and Lo Savio, E. and Marchini, A. and Marino, G. and Masi, G. and Massallé, A. and Maulella, R. and McFarland, J. and Miyashita, K. and Napoli, C. and Noyelles, B. and Pauwels, T. and Pavlov, H. and Peng, Q. Y. and Perelló, C. and Priban, V. and Prost, J. and Razemon, S. and Rousselle, J. P. and Rovira, J. and Ruisi, R. and Ruocco, N. and Salvaggio, F. and Sbarufatti, G. and Shakun, L. and Scheck, A. and Sciuto, C. and da Silva Neto, D. N. and V Sinyaeva, N. and Sofia, A. and Sonka, A. and Talbot, J. and Tang, Z. H. and Tejfel, V. G. and Thuillot, W. and Tigani, K. and Timerson, B. and Tontodonati, E. and Tsamis, V. and Unwin, M. and Venable, R. and Vieira-Martins, R. and Vilar, J. and Vingerhoets, P. and Watanabe, H. and Yin, H. X. and Yu, Y. and Zambelli, R.},
	month = dec,
	year = {2014},
	pages = {A120},
	file = {Arlot et al. - 2014 - The PHEMU09 catalogue and astrometric results of t.pdf:/Users/fb90/Zotero/storage/C8QS67MT/Arlot et al. - 2014 - The PHEMU09 catalogue and astrometric results of t.pdf:application/pdf}
}

@article{dias-oliveira2013,
	title = {Analysis of 25 mutual eclipses and occultations between the {Galilean} satellites observed from {Brazil} in 2009},
	volume = {432},
	issn = {0035-8711},
	url = {https://academic.oup.com/mnras/article/432/1/225/1117425},
	doi = {10.1093/mnras/stt447},
	abstract = {Abstract.  The light curves of mutual eclipses and occultations between the natural satellites of a planet allow us to obtain high-precision position and relati},
	language = {en},
	number = {1},
	urldate = {2020-02-05},
	journal = {Mon Not R Astron Soc},
	author = {Dias-Oliveira, A. and Vieira-Martins, R. and Assafin, M. and Camargo, J. I. B. and Braga-Ribas, F. and da Silva Neto, D. N. and Gaspar, H. S. and Pires dos Santos, P. M. and Domingos, R. C. and Boldrin, L. a. G. and Izidoro, A. and Carvalho, J. P. S. and Sfair, R. and Sampaio, J. C. and Winter, O. C.},
	month = jun,
	year = {2013},
	pages = {225--242},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/FK2UVP7Z/Dias-Oliveira et al. - 2013 - Analysis of 25 mutual eclipses and occultations be.pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/FD4YSANV/1117425.html:text/html}
}

@article{dekleer2017,
	title = {Multi-phase volcanic resurfacing at {Loki} {Patera} on {Io}},
	volume = {545},
	issn = {0028-0836, 1476-4687},
	url = {http://www.nature.com/articles/nature22339},
	doi = {10.1038/nature22339},
	language = {en},
	number = {7653},
	urldate = {2020-02-05},
	journal = {Nature},
	author = {de Kleer, K. and Skrutskie, M. and Leisenring, J. and Davies, A. G. and Conrad, A. and de Pater, I. and Resnick, A. and Bailey, V. and Defrère, D. and Hinz, P. and Skemer, A. and Spalding, E. and Vaz, A. and Veillet, C. and Woodward, C. E.},
	month = may,
	year = {2017},
	pages = {199--202},
	file = {de Kleer et al. - 2017 - Multi-phase volcanic resurfacing at Loki Patera on.pdf:/Users/fb90/Zotero/storage/YL65Z6BW/de Kleer et al. - 2017 - Multi-phase volcanic resurfacing at Loki Patera on.pdf:application/pdf}
}

@article{rathbun2004,
	series = {Special {Issue}: {Io} after {Galileo}},
	title = {Mapping of {Io}'s thermal radiation by the {Galileo} photopolarimeter–radiometer ({PPR}) instrument},
	volume = {169},
	issn = {0019-1035},
	url = {http://www.sciencedirect.com/science/article/pii/S0019103504000235},
	doi = {10.1016/j.icarus.2003.12.021},
	abstract = {Between 1999 and 2002, the Galileo spacecraft made 6 close flybys of Io during which many observations of Io's thermal radiation were made with the photopolarimeter–radiometer (PPR). While the NIMS instrument could measure thermal emission from hot spots with T{\textgreater}200 K, PPR was the only Galileo instrument capable of mapping the lower temperatures of older, cooling lava flows, and the passive background. We tabulate all data taken by PPR of Io during these flybys and describe some scientific highlights revealed by the data. The data include almost complete coverage of Io at better than 250 km resolution, with extensive regional coverage at higher resolutions. We found a modest poleward drop in nighttime background temperatures and evidence of thermal inertia variations across the surface. Comparison of high spatial resolution temperature measurements with observed daytime SO2 gas pressures on Io provides evidence for local cold trapping of SO2 frost on scales smaller than the 60 km resolution of the PPR data. We also calculated the power output from several hot spots and estimated total global heat flow to be about 2.0–2.6 Wm−2. The low-latitude diurnal temperature variations for the regions between obvious hot spots are well matched by a laterally-inhomogeneous thermal model with less than 1 Wm−2 endogenic heat flow.},
	language = {en},
	number = {1},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Rathbun, J. A. and Spencer, J. R. and Tamppari, L. K. and Martin, T. Z. and Barnard, L. and Travis, L. D.},
	month = may,
	year = {2004},
	keywords = {Infrared observations, Io, Surfaces, Thermal histories, Volcanism},
	pages = {127--139},
	file = {ScienceDirect Full Text PDF:/Users/fb90/Zotero/storage/JNFP3DR5/Rathbun et al. - 2004 - Mapping of Io's thermal radiation by the Galileo p.pdf:application/pdf;ScienceDirect Snapshot:/Users/fb90/Zotero/storage/UYXEFGNY/S0019103504000235.html:text/html}
}

@article{davies2015,
	title = {Map of {Io}’s volcanic heat flow},
	volume = {262},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103515003474},
	doi = {10.1016/j.icarus.2015.08.003},
	abstract = {We present a map of Io’s volcanic heat ﬂow. Io’s high heat ﬂow is a result of intense tidal heating, which generates widespread volcanic activity. The surface expression of ongoing volcanic activity constrains the location and magnitude of tidal dissipation within Io. Tidal heating models place heating either at relatively shallow (aesthenosphere) levels, or deep in the mantle. It was thought that actual tidal heating could be approximated using a combination of these end-member models. Io’s volcanic heat ﬂow has now been mapped in sufﬁcient detail to compare with the models. Our maps show that the distribution of heat ﬂow is not matched by current models of deep nor shallow tidal heating, nor by any combination of these two models. We ﬁnd relatively low heat ﬂow at sub-jovian (0°W) and anti-jovian (180°W) longitudes, at odds with the pure aesthenospheric heating model. Furthermore, there are large swaths of Io’s surface where there is poor correlation between the number of hot spots in an area and the power emitted. We have previously accounted for \%54\% of Io’s observed heat ﬂow. We now show that Io’s anomalously warm poles, possibly the result of heat ﬂow from deep-mantle heating, would yield the ‘‘missing” energy (48 TW) if the polar surfaces are at temperatures of \$90 K to \$95 K and cover latitudes above \$43° to \$48° respectively. This possibility implies a ratio of deep to shallow heating of about 1:1. However, explaining regional variations in surface volcanic activity requires more detailed modeling of the location and magnitude of the internal tidal dissipation and the consequences of mantle convection and advection within Io. Future model predictions can be compared to our heat ﬂow map.},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Davies, Ashley Gerard and Veeder, Glenn J. and Matson, Dennis L. and Johnson, Torrence V.},
	month = dec,
	year = {2015},
	pages = {67--78},
	file = {Davies et al. - 2015 - Map of Io’s volcanic heat flow.pdf:/Users/fb90/Zotero/storage/W254VRSQ/Davies et al. - 2015 - Map of Io’s volcanic heat flow.pdf:application/pdf}
}

@article{dekleer2016,
	title = {Time variability of {Io}'s volcanic activity from near-{IR} adaptive optics observations on 100 nights in 2013–2015},
	volume = {280},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103516303104},
	doi = {10.1016/j.icarus.2016.06.019},
	abstract = {Jupiter’s moon Io is a dynamic target, exhibiting extreme and time-variable volcanic activity powered by tidal forcing from Jupiter. We have conducted a campaign of high-cadence observations of Io with the goal of characterizing its volcanic activity. Between Aug 2013 and the end of 2015, we imaged Io on 100 nights in the near-infrared with adaptive optics on the Keck and Gemini N telescopes, which resolve emission from individual volcanic hot spots. During our program, we made over 400 detections of 48 distinct hot spots, some of which were detected 30+ times. We use these observations to derive a timeline of global volcanic activity on Io, which exhibits wide variability from month to month. The timelines of thermal activity at individual volcanic centers have geophysical implications, and will permit future characterization by others. We evaluate hot spot detection limits and give a simple parameterization of the minimum detectable intensity as a function of emission angle, which can be applied to other analyses. We detected three outburst eruptions in August 2013, but no other outburst-scale events were observed in the subsequent ∼90 observations. Either the cluster of events in August 2013 was a rare occurrence, or there is a mechanism causing large events to occur closely-spaced in time. We also detected large eruptions (though not of outburst scale) within days of one another at Kurdalagon Patera and Sethlaus/Gabija Paterae in 2015. As was also seen in the Galileo dataset, the hot spots we detected can be separated into two categories based on their thermal emission: those that are persistently active for 1 year or more at moderate intensity, and those that are only brieﬂy active, are time-variable, and often reach large intensities. A small number of hot spots in the latter category appear and subside in a matter of days, reaching particularly high intensities; although these are not bright enough to qualify as outbursts, their thermal signatures follow the same pattern, suggesting that a similar mechanism may be responsible for these events though at a smaller scale.},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {de Kleer, Katherine and de Pater, Imke},
	month = dec,
	year = {2016},
	pages = {378--404},
	file = {de Kleer and de Pater - 2016 - Time variability of Io's volcanic activity from ne.pdf:/Users/fb90/Zotero/storage/X582C794/de Kleer and de Pater - 2016 - Time variability of Io's volcanic activity from ne.pdf:application/pdf}
}

@article{dekleer2016a,
	title = {Spatial distribution of {Io}’s volcanic activity from near-{IR} adaptive optics observations on 100 nights in 2013–2015},
	volume = {280},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103516303098},
	doi = {10.1016/j.icarus.2016.06.018},
	abstract = {The extreme and time-variable volcanic activity on Jupiter’s moon Io is the result of periodic tidal forcing. The spatial distribution of Io’s surface heat ﬂux provides an important constraint on models for tidal heat dissipation, yielding information on interior properties and on the depth at which the tidal heat is primarily dissipated. We analyze the spatial distribution of 48 hot spots based on more than 400 total hot spot detections in adaptive optics images taken on 100 nights in 2013–2015 (data presented in de Kleer and de Pater [2016] Time variability of Io’s volcanic activity from near-IR adaptive optics 13 observations on 100 nights in 2013–2015). We present full surface maps of Io at multiple near-infrared wavelengths for three epochs during this time period, and show that the longitudinal distribution of hot spots has not changed signiﬁcantly since the Galileo mission.},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {de Kleer, Katherine and de Pater, Imke},
	month = dec,
	year = {2016},
	pages = {405--414},
	file = {de Kleer and de Pater - 2016 - Spatial distribution of Io’s volcanic activity fro.pdf:/Users/fb90/Zotero/storage/2UJTC9YT/de Kleer and de Pater - 2016 - Spatial distribution of Io’s volcanic activity fro.pdf:application/pdf}
}

@article{gutierrez2016,
	title = {Occultation {Observations} of {Io}'s {Hot} {Spots} in 2014},
	volume = {23},
	url = {http://adsabs.harvard.edu/abs/2016AGUFM.P23C2183G},
	abstract = {We present ground-based observations and analysis of Io in the near-infrared during Spring 2014 taken with the imager on the CSHELL instrument of NASA's Infrared Telescope Facility (IRTF). Images of Io were taken during reappearance from Jupiter occultation into eclipse, therefore the derived fluxes originate entirely from hotspot volcanism. The eight nights of observations were all obtained in L' band
(3.8-microns) from February to May 2014. The images do not resolve individual hotspots; however by analyzing the light curve and fitting an occultation model to the data we are able to determine the spectral flux and location of distinct hotspots. Loki Patera, and Janus Patera and/or Kanehekili Fluctus are the most likely candidates for detected hotspots across all of the nights. We compare the absolute flux densiti of the individual volcanoes over this period to observe decreases in brightness over the four month time period. This analysis contributes to the decadal timelines of Loki Patera's and Janus Patera/Kanehekili Fluctus's volcanic variability.},
	urldate = {2020-02-04},
	journal = {AGU Fall Meeting Abstracts},
	author = {Gutierrez, S. and De Pater, I. and de Kleer, K. and Rathbun, J. A. and Spencer, J. R.},
	month = dec,
	year = {2016},
	keywords = {2756 Planetary magnetospheres, MAGNETOSPHERIC PHYSICSDE: 6219 Io, PLANETARY SCIENCES: SOLAR SYSTEM OBJECTSDE: 6220 Jupiter, PLANETARY SCIENCES: SOLAR SYSTEM OBJECTSDE: 8450 Planetary volcanism, VOLCANOLOGY},
	pages = {P23C--2183},
	file = {2954.pdf:/Users/fb90/Zotero/storage/U47BQXY9/2954.pdf:application/pdf}
}

@article{spencer1990,
	title = {Discovery of hotspots on lo using disk-resolved infrared imaging},
	volume = {348},
	language = {en},
	author = {Spencer, R and Shure, M A and Ressler, M E and Goguent, D and Sinton, W M and Toomey, D W},
	year = {1990},
	pages = {4},
	file = {Spencer et al. - 1990 - Discovery of hotspots on lo using disk-resolved in.pdf:/Users/fb90/Zotero/storage/48DRCFIS/Spencer et al. - 1990 - Discovery of hotspots on lo using disk-resolved in.pdf:application/pdf}
}

@article{spencer1994,
	title = {Io {Hot} {Spots} in 1991: {Results} from {Europa} {Occultation} {Photometry} and {Infrared} {Imaging}},
	volume = {107},
	issn = {0019-1035},
	shorttitle = {Io {Hot} {Spots} in 1991},
	url = {http://www.sciencedirect.com/science/article/pii/S0019103584710165},
	doi = {10.1006/icar.1994.1016},
	abstract = {During the winter of 1991 an unusually favorable series of occultations of Io by Europa took place. We obtained infrared photometry of four of these events at the United Kingdom Infrared Telescope at wavelengths of 5.0 or 3.4 μm, in order to investigate the nature and distribution of volcanism on Io by observing the occultation of the volcanic hot spots by the limb of Europa. Observations at 3.4 μm on 1991/01/08 detected a possible small hot spot in the northern hemisphere. Observations at 5.0 μm on 1991/02/27 detected and resolved the major hot spot Loki, which had a diameter of 170 km and had three times its Voyager 1 flux, and also detected the Voyager hot spot Pele at about half its Voyager 1 flux. A 5.0-μm occultation of Pele on 1991/03/06, when Loki was not occulted, indicated no significant flux change since the week before. Infrared images of Io obtained at the NASA Infrared Telescope Facility between October 1990 and April 1991 show that the Europa occultations occurred during a period of unusually high activity at Loki. Loki showed very little thermal emission in observations between 1990/10/12 and 1990/11/27, but increased in flux by a factor of 10 in 32 days by 1991/12/29. Loki then remained bright in all observations until 1991/03/26, but had begun to fade on 1991/04/09. Such rapid variations in flux over such a large area are remarkable. Multiwavelength observations indicate that Loki increased in temperature during the brightening, and that materials hotter than 630 K were exposed at Loki. The possible "Pele-type" volcanoes Surt and Aten, unlike Pele, were not detected, with 3.8 μm flux upper limits of about 8 GW μm-1 str-1.},
	language = {en},
	number = {1},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Spencer, John R. and Clark, Beth E. and Woodney, Laura M. and Sinton, William M. and Toomey, D.},
	month = jan,
	year = {1994},
	pages = {195--208},
	file = {main.pdf:/Users/fb90/Zotero/storage/XAANQK8Q/main.pdf:application/pdf;ScienceDirect Snapshot:/Users/fb90/Zotero/storage/DNTMT84N/S0019103584710165.html:text/html}
}

@article{kirchoff2011,
	title = {Global distribution of volcanic centers and mountains on {Io}: {Control} by asthenospheric heating and implications for mountain formation},
	volume = {301},
	issn = {0012821X},
	shorttitle = {Global distribution of volcanic centers and mountains on {Io}},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0012821X10007132},
	doi = {10.1016/j.epsl.2010.11.018},
	abstract = {Jupiter's moon Io possesses numerous tectonic mountains in addition to its ubiquitous volcanoes and volcanic features. Remarkably, a distinct global anticorrelation exists between the spatial distribution of mountains and volcanic centers on Io. This relationship indicates an explicit connection between volcanism and mountain formation, even though the mountains are tectonic in origin (predominantly upthrusted crustal blocks). Spherical harmonic analysis shows the distribution of mountains and volcanic centers have statistically signiﬁcant power at degree 2; this result is especially striking for the volcanic center distribution, and directly implicates models of asthenospheric tidal heating. The latter predict enhanced heat ﬂux along the equator in a degree-two pattern that matches observations. Mountain formation on Io appears to be a form of dominantly vertical tectonism unique in the modern Solar System: continual burial by widespread volcanism drives the crust inward, which leads to strong compression, and at discrete locations, mountains. Correlation coefﬁcients between the volcanic and mountain distributions indicate statistically meaningful anticorrelation at low spectral degrees (l = 1, 2, 4, and 6); the anticorrelation is especially signiﬁcant between the longitudinal (sectorial) l = 2 components when considered on their own. We compare this anticorrelation with published models that link volcano and mountain formation. While consistent in part with l = 2 convection models, which predict such an anticorrelation (in principle), such low degree anticorrelations are also (if not more) compatible with mountain formation due to, or inﬂuenced by, thermal expansion of Io's crust, and deep compression and thrust faulting in regions of lower than average volcanic heat-piping. Positive correlations between mountain and volcanic center distributions at high spectral degree may reﬂect structural links between a good fraction of mountain blocks and adjacent volcanic paterae, whereas the anticorrelation at low degree implies that most volcanic features (which are far more numerous overall) form independently of mountains.},
	language = {en},
	number = {1-2},
	urldate = {2020-02-04},
	journal = {Earth and Planetary Science Letters},
	author = {Kirchoff, Michelle R. and McKinnon, William B. and Schenk, Paul M.},
	month = jan,
	year = {2011},
	pages = {22--30},
	annote = {They use spherical harmonics to describe pre-determined locations of volcanos and mountains by expanding the scalar field of their positions (delta functions) in terms of spherical harmonics up to certain degree. They don't fit for the spherical harmonic coefficients.
Then they use the SH representation of the volcanos and mountains to  measure anti-correlation in their positions.},
	file = {Kirchoff et al. - 2011 - Global distribution of volcanic centers and mounta.pdf:/Users/fb90/Zotero/storage/AMW5SS6S/Kirchoff et al. - 2011 - Global distribution of volcanic centers and mounta.pdf:application/pdf}
}

@article{kleer2019,
	title = {Variability in {Io}'s {Volcanism} on {Timescales} of {Periodic} {Orbital} {Changes}},
	volume = {46},
	issn = {0094-8276, 1944-8007},
	url = {https://onlinelibrary.wiley.com/doi/abs/10.1029/2019GL082691},
	doi = {10.1029/2019GL082691},
	abstract = {The widespread volcanism on the Jovian moon Io is powered by tidal heating, yet we lack a deep understanding of how this distinctive heating process affects the locations, timing, or intensities of Io's eruptions. We show that the quasiperiodic behavior of the volcano Loki Patera in 1987–2018 matches the timescales for the evolution of Io's eccentricity and semimajor axis ({\textasciitilde}480 and {\textasciitilde}460 days). If this orbital forcing is driving Loki Patera's variability, a low‐pass geophysical ﬁlter such as poroelastic ﬂow, or a resonant ampliﬁcation of Io's wobble, could account for the importance of these long‐period orbital variations despite their small amplitudes. The peak volcanic response is predicted to roughly coincide with Io's maximum eccentricity, consistent with the observations. High‐cadence observations over the next several years have the potential to conclusively discriminate between orbital versus geophysical control of Loki Patera's variability. Plain Language Summary Tidal heating is one of the central processes that generates heat in the interiors of planets and moons and is in part responsible for the existence of subsurface oceans and geological activity on moons in the outer solar system. Under this process, the amount of heating that occurs, and the stresses in the crust, vary periodically with the periodic tidal ﬂexing. As a result, we might expect that any geological activity powered by tidal heating, such as volcanic eruptions on Jupiter's tidally heated moon Io, would also vary periodically. Indeed, the water geysers on Saturn's moon Enceladus vary in strength over the course of Enceladus' orbit around Saturn due to tides opening and closing ﬁssures. Io takes only 1.77 days to orbit Jupiter, but its orbit is also slowly changing in time with a period of {\textasciitilde}480 days. We compare the variability of Io's volcanoes with the evolution of its orbit and ﬁnd that the quasiperiodic behavior of Loki Patera, the most powerful volcano on Io, follows a similar pattern as the orbital changes. We explore whether this volcano could be brightening and fading in response to changes in the heating and stresses produced by tides in its interior and what implications this has for the geophysical processes in Io's interior.},
	language = {en},
	number = {12},
	urldate = {2020-02-04},
	journal = {Geophys. Res. Lett.},
	author = {Kleer, Katherine and Nimmo, Francis and Kite, Edwin},
	month = jun,
	year = {2019},
	pages = {6327--6332},
	file = {Kleer et al. - 2019 - Variability in Io's Volcanism on Timescales of Per.pdf:/Users/fb90/Zotero/storage/YP736XBR/Kleer et al. - 2019 - Variability in Io's Volcanism on Timescales of Per.pdf:application/pdf}
}

@article{dekleer,
	title = {Io as a {Template} for {Volcanic} {Signatures} on {Exoplanets}},
	abstract = {Exoplanets in eccentric orbits or those orbiting very close to their host stars may host molten rock at their surfaces and silicate or sulfuric atmospheres. As the only Solar System world whose surface and atmosphere are dominated by the products of volcanic activity, Jupiter’s moon Io demonstrates a range of signatures indicative of volcanism and provides a template for connecting such signatures to the volcanic activity that produces them. This presentation will review recent results from ground- and space-based observations targeting Io’s volcanism and its various products and signatures, and will discuss the relevance of these results to searches for evidence of volcanism on extrasolar planets and moons.},
	language = {en},
	author = {de Kleer, Katherine},
	pages = {2},
	file = {de Kleer - Io as a Template for Volcanic Signatures on Exopla.pdf:/Users/fb90/Zotero/storage/XEMB6AS5/de Kleer - Io as a Template for Volcanic Signatures on Exopla.pdf:application/pdf}
}

@article{kaltenegger2010,
	title = {{DETECTING} {VOLCANISM} {ON} {EXTRASOLAR} {PLANETS}},
	volume = {140},
	issn = {0004-6256, 1538-3881},
	url = {http://stacks.iop.org/1538-3881/140/i=5/a=1370?key=crossref.e0a0160e82d36b4982de83d42e2b19d7},
	doi = {10.1088/0004-6256/140/5/1370},
	abstract = {The search for extrasolar rocky planets has already found the ﬁrst transiting rocky super-Earth, Corot 7b, with a surface temperature that allows for magma oceans. Here, we investigate whether we could distinguish rocky planets with recent major volcanism by remote observation. We develop a model for volcanic eruptions on an Earth-like exoplanet based on the present-day Earth and derive the observable features in emergent and transmission spectra for multiple scenarios of gas distribution and cloud cover. We calculate the observation time needed to detect explosive volcanism on exoplanets in primary as well as secondary eclipse and discuss the likelihood of observing volcanism on transiting Earth-sized to super-Earth-sized exoplanets. We ﬁnd that sulfur dioxide from large explosive eruptions does present a spectral signal that is remotely detectable especially for secondary eclipse measurements around the closest stars and ground-based telescopes, and report the frequency and magnitude of the expected signatures. The transit probability of a planet in the habitable zone decreases with distance from the host star, making small, nearby host stars the best targets.},
	language = {en},
	number = {5},
	urldate = {2020-02-04},
	journal = {The Astronomical Journal},
	author = {Kaltenegger, L. and Henning, W. G. and Sasselov, D. D.},
	month = nov,
	year = {2010},
	pages = {1370--1380},
	file = {Kaltenegger et al. - 2010 - DETECTING VOLCANISM ON EXTRASOLAR PLANETS.pdf:/Users/fb90/Zotero/storage/AK4RLEFY/Kaltenegger et al. - 2010 - DETECTING VOLCANISM ON EXTRASOLAR PLANETS.pdf:application/pdf}
}

@article{dekleer2017a,
	title = {Io’s {Loki} {Patera}: {Modeling} of three brightening events in 2013–2016},
	volume = {289},
	issn = {00191035},
	shorttitle = {Io’s {Loki} {Patera}},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103516306443},
	doi = {10.1016/j.icarus.2017.01.038},
	abstract = {Loki Patera is one of the most dramatically time-variable volcanic features on Io, exhibiting episodic brightening events every 1–3 years that may produce over 15\% of Io’s global heat ﬂow. We observed three such brightening events with adaptive optics imaging at the Keck and Gemini N telescopes over the course of 70 nights of observation in 2013–2016. The high cadence and multi-wavelength nature of the observations provides constraints on models for activity at Loki Patera. The Matson et al. (2006) model for Loki Patera as an overturning basaltic magma sea is adapted to ﬁt the observations of all three events. In particular, we adjust the details of the overturn progression, and modify the lava thermal properties to include dependencies on temperature and porosity, to improve the ﬁt to the data. The preferred models ﬁnd overturn front propagation velocities of 1.2–1.7 km/day, corresponding to resurfacing rates of 1500–2200 m2/s. The time intervals of 440–540 days between successive events are roughly consistent with the 540-day period calculated by Rathbun et al. (2002) for events prior to 2001. The best coverage was obtained for the 2016 brightening; model ﬁts to this event require a lava bulk thermal conductivity of 0.55–0.75 W/m/K, with the best ﬁt obtained for a value of ∼0.7 W/m/K and an average porosity that decreases during cooling. For all three events, the overturn front appears to propagate around the patera in the clockwise direction, opposite to what has been inferred for past brightening events. There is evidence that the overturn may be more complex than a single propagating wave, perhaps involving multiple simultaneous resurfacing waves as well as portions of the patera that are active even after the nominal bright phase has ended. The measured intensities are anomalously low when Loki Patera is viewed at high emission angles, suggestive of topographic shadowing due to a raised area or the edge of the depression in which the magma sea resides.},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {de Kleer, Katherine and de Pater, Imke},
	month = jun,
	year = {2017},
	pages = {181--198},
	file = {de Kleer and de Pater - 2017 - Io’s Loki Patera Modeling of three brightening ev.pdf:/Users/fb90/Zotero/storage/DALKFSLQ/de Kleer and de Pater - 2017 - Io’s Loki Patera Modeling of three brightening ev.pdf:application/pdf}
}

@misc{zotero-3195,
	title = {Variability and geologic associations of volcanic activity on {Io} in 2001-2016 {\textbar} {Elsevier} {Enhanced} {Reader}},
	url = {https://reader.elsevier.com/reader/sd/pii/S0019103517305018?token=55D03F2165F44819CA938EC1E92A3D0D7D0E6F4B812D8C48C396A6C89104D36DC173D547BE944268390924DD06AF7ECE},
	language = {en},
	urldate = {2020-02-04},
	doi = {10.1016/j.icarus.2018.04.007},
	file = {Snapshot:/Users/fb90/Zotero/storage/APPEQF73/S0019103517305018.html:text/html;Variability and geologic associations of volcanic .pdf:/Users/fb90/Zotero/storage/9V2WYXRY/Variability and geologic associations of volcanic .pdf:application/pdf}
}

@article{retherford2019,
	title = {Io’s {Atmosphere} {Silhouetted} by {Jupiter} {Ly} \textit{α}},
	volume = {158},
	issn = {1538-3881},
	url = {https://iopscience.iop.org/article/10.3847/1538-3881/ab3c4c},
	doi = {10.3847/1538-3881/ab3c4c},
	abstract = {We report results from a new technique for mapping Io’s SO2 vapor distribution. The Space Telescope Imaging Spectrograph (STIS) instrument on the Hubble Space Telescope observed Io during four Jupiter transit events to obtain medium resolution far-UV spectral images near the Lyα wavelength of 121.6 nm. Jupiter’s bright Lyα dayglow provides a bright, mostly uniform background light source for opacity measurements, much like during a stellar occultation or transiting exoplanet event. Peaks in the photoabsorption cross-sections for sulfur dioxide occur near 122 nm, with resulting absorptions raising the altitude where a tangential line-of-sight opacity of ∼1 occurs. This method of measuring column densities along lines of sight above the limb uses detailed image simulations and complements Lyα reﬂectance imaging and other methods for measuring Io’s SO2 gas on the disk. Our reported near-terminator limb observations with STIS conﬁrm the ﬁndings from previous Lyα disk reﬂectance imaging that Io’s polar SO2 density is an order of magnitude lower than found at the equator. We provide constraints for additional attenuation by atmospheric hydrogen atoms produced by charge exchange reactions between magnetospheric protons and Io’s atmosphere. Searches for plume-related features provided no deﬁnitive enhancements within the signal quality, ruling out unusually high levels of activity for Pele and Tvashtar.},
	language = {en},
	number = {4},
	urldate = {2020-02-04},
	journal = {AJ},
	author = {Retherford, K. D. and Roth, L. and Becker, T. M. and Feaga, L. M. and Tsang, C. C. C. and Jessup, K. L. and Grava, C.},
	month = sep,
	year = {2019},
	pages = {154},
	file = {Retherford et al. - 2019 - Io’s Atmosphere Silhouetted by Jupiter Ly iαi.pdf:/Users/fb90/Zotero/storage/RSM6HZNR/Retherford et al. - 2019 - Io’s Atmosphere Silhouetted by Jupiter Ly iαi.pdf:application/pdf}
}

@article{rathbun2014,
	title = {Io’s active volcanoes during the {New} {Horizons} era: {Insights} from {New} {Horizons} imaging},
	volume = {231},
	issn = {00191035},
	shorttitle = {Io’s active volcanoes during the {New} {Horizons} era},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103513005113},
	doi = {10.1016/j.icarus.2013.12.002},
	abstract = {In February 2007, the New Horizons spacecraft ﬂew by the Jupiter system, obtaining images of Io, the most volcanically active body in the Solar System. The Multicolor Visible Imaging Camera (MVIC), a four-color (visible to near infrared) camera, obtained 17 sets of images. The Long-Range Reconnaissance Imager (LORRI), a high-resolution panchromatic camera, obtained 190 images, including many of Io eclipsed by Jupiter. We present a complete view of the discrete point-like emission sources in all images obtained by these two instruments. We located 54 emission sources and determined their brightnesses. These observations, the ﬁrst that observed individual Ionian volcanoes on short timescales of seconds to minutes, demonstrate that the volcanoes have stable brightnesses on these timescales. The active volcanoes Tvashtar (63N, 124W) and E. Girru (22N, 245W) were observed by both LORRI and MVIC, both in the near-infrared (NIR) and methane (CH4) ﬁlters. Tvashtar was additionally observed in the red ﬁlter, which allowed us to calculate a color temperature of approximately 1200 K. We found that, with some exceptions, most of the volcanoes frequently active during the Galileo era continued to be active during the New Horizons ﬂyby. We found that none of the seven volcanoes observed by New Horizons multiple times over short timescales showed substantial changes on the order of seconds and only one, E. Girru exhibited substantial variation over minutes to days, increasing by 25\% in just over an hour and decreasing by a factor of 4 over 6 days. Observations of Tvashtar are consistent with a current eruption similar to previously observed eruptions and are more consistent with the thermal emission of a lava ﬂow than the ﬁre fountains inferred from the November 1999 observations. These data also present new puzzles regarding Ionian volcanism. Since there is no associated surface change or low albedo feature that could be identiﬁed nearby, the source of the emission from E. Girru is a mystery. Furthermore, the in-eclipse glows we observe over many paterae are likely to be gas emission from interaction with the magnetosphere, but the details of that process are not clear.},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Rathbun, J.A. and Spencer, J.R. and Lopes, R.M. and Howell, R.R.},
	month = mar,
	year = {2014},
	pages = {261--272},
	file = {Rathbun et al. - 2014 - Io’s active volcanoes during the New Horizons era.pdf:/Users/fb90/Zotero/storage/GK5U2DF3/Rathbun et al. - 2014 - Io’s active volcanoes during the New Horizons era.pdf:application/pdf}
}

@article{rathbun2018,
	title = {The {Global} {Distribution} of {Active} {Ionian} {Volcanoes} and {Implications} for {Tidal} {Heating} {Models}},
	volume = {156},
	issn = {1538-3881},
	url = {http://stacks.iop.org/1538-3881/156/i=5/a=207?key=crossref.659198d388c2489861a59f772a1f1628},
	doi = {10.3847/1538-3881/aae370},
	abstract = {Tidal heating is the major source of heat in the outer solar system. Because of its strong tidal interaction with Jupiter and the other Galilean satellites, Io is incredibly volcanically active. We use the directly measured volcanic activity level of Io’s volcanoes as a proxy for surface heat ﬂow and compare it to tidal heating model predictions. Volcanic activity is a better proxy for heat ﬂow than simply the locations of volcanic constructs. We determine the volcanic activity level using three data sets: the Galileo Photopolarimeter Radiometer (PPR), Galileo Near-Infrared Mapping Spectrometer (NIMS), and New Horizons LEISA. We also present a systematic reanalysis of the Galileo NIMS observations to determine the 3.5 μm brightness of 51 active volcanoes. We ﬁnd that potential differences in volcanic style between high and low latitudes make high-latitude observations unreliable for distinguishing between tidal heating models. Observations of Io’s polar areas, such as those by Juno, are necessary to unambiguously understand Io’s heat ﬂow. However, all three of the data sets examined show a relative dearth of volcanic brightness near 180 W (anti-Jovian point) and the equator, and the only data set with good observations of the sub-Jovian point (LEISA) also shows a lack of volcanic brightness in that region. These observations are more consistent with the mantle-heating model than the asthenospheric-heating model. Furthermore, all three of the data sets are consistent with fourfold symmetry in longitude and peak heat ﬂow at mid-latitudes, which best matches with the combined heating case of Tackley et al.},
	language = {en},
	number = {5},
	urldate = {2020-02-04},
	journal = {AJ},
	author = {Rathbun, Julie A. and Lopes, Rosaly M. C. and Spencer, John R.},
	month = oct,
	year = {2018},
	pages = {207},
	file = {Rathbun et al. - 2018 - The Global Distribution of Active Ionian Volcanoes.pdf:/Users/fb90/Zotero/storage/HKAU5VNS/Rathbun et al. - 2018 - The Global Distribution of Active Ionian Volcanoes.pdf:application/pdf}
}

@article{cantrall2018,
	title = {Variability and geologic associations of volcanic activity on {Io} in 2001–2016},
	volume = {312},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103517305018},
	doi = {10.1016/j.icarus.2018.04.007},
	abstract = {Since the end of the Galileo epoch, ground-based observations have been crucial for the continued monitoring and characterization of volcanic activity on Jupiter’s moon, Io. We compile and analyze observations from the Keck and Gemini North telescopes between 2001 and 2016, including new and published observations from 2003, 2004, 2005, 2007, 2008, 2009, 2011, 2012, 2013, and 2016. A total of 88 distinct hot spot sites were detected over the 15-year period, 82 of which were detected multiple times, and 24 of which were not detected by Galileo at thermal infrared wavelengths (1–5 μm). A variety of analytical methods are utilized to investigate the detections of active volcanism as a surface expression of interior heating. Geologic associations of hot spots, including patera type, lava ﬂow type, and proximity to mountainous regions, are made using the USGS-published global geologic map of Io (Williams, 2011). We also provide a summary of outburst-scale events, along with the slightly less bright but more frequent, mini-outbursts described by de Kleer and de Pater (2016a).},
	language = {en},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Cantrall, Clayton and de Kleer, Katherine and de Pater, Imke and Williams, David A. and Davies, Ashley Gerard and Nelson, David},
	month = sep,
	year = {2018},
	pages = {267--294},
	file = {Cantrall et al. - 2018 - Variability and geologic associations of volcanic .pdf:/Users/fb90/Zotero/storage/M8SFQ5DA/Cantrall et al. - 2018 - Variability and geologic associations of volcanic .pdf:application/pdf}
}

@article{veeder1994,
	title = {Io's heat flow from infrared radiometry: 1983–1993},
	volume = {99},
	issn = {2156-2202},
	shorttitle = {Io's heat flow from infrared radiometry},
	url = {https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/94JE00637},
	doi = {10.1029/94JE00637},
	abstract = {We report the following results from a decade of infrared radiometry of Io: (1) The average global heat flow is more than ∼2.5 W m−2, (2) large warm (≤200 K) volcanic regions dominate the global heat flow, (3) small high-temperature (≥300 K) “hotspots” contribute little to the average heat flow, (4) thermal anomalies on the leading hemisphere contribute about half of the heat flow, (5) a substantial amount of heat is radiated during Io's night, (6) high-temperature (≥600 K) “outbursts” occurred during ∼4\% of the nights we observed, (7) “Loki” is the brightest, persistent, infrared emission feature, and (8) some excess emission is always present at the longitude of Loki, but its intensity and other characteristics change between apparitions. Observations of Io at M (4.8 μm), 8.7 μm, N (10 μm), and Q (20 μm) with the Infrared Telescope Facility presented here were collected during nine apparitions between 1983 and 1993. These measurements provide full longitudinal coverage as well as an eclipse observation and the detection of two outbursts. Reflected sunlight, passive thermal emission, and radiation from thermal anomalies all contribute to the observed flux densities. We find that a new thermophysical model is required to match all the data. Two key elements of this model are (1) a “thermal reservoir” unit which lowers daytime temperatures, and (2) the “thermal pedestal effect” which shifts to shorter wave-lengths the spectral emission due to the reradiation of solar energy absorbed by the thermal anomalies. The thermal anomalies are modeled with a total of 10 source components at five locations. Io's heat flow is the sum of the power from these components.},
	language = {en},
	number = {E8},
	urldate = {2020-02-06},
	journal = {Journal of Geophysical Research: Planets},
	author = {Veeder, Glenn J. and Matson, Dennis L. and Johnson, Torrence V. and Blaney, Diana L. and Goguen, Jay D.},
	year = {1994},
	pages = {17095--17162},
	file = {Snapshot:/Users/fb90/Zotero/storage/2NG4ELNA/94JE00637.html:text/html;Submitted Version:/Users/fb90/Zotero/storage/CCF8RY8F/Veeder et al. - 1994 - Io's heat flow from infrared radiometry 1983–1993.pdf:application/pdf}
}

@article{spencer1994a,
	title = {Io {Hot} {Spots} in 1991: {Results} from {Europa} {Occultation} {Photometry} and {Infrared} {Imaging}},
	volume = {107},
	issn = {0019-1035},
	shorttitle = {Io {Hot} {Spots} in 1991},
	url = {http://www.sciencedirect.com/science/article/pii/S0019103584710165},
	doi = {10.1006/icar.1994.1016},
	abstract = {During the winter of 1991 an unusually favorable series of occultations of Io by Europa took place. We obtained infrared photometry of four of these events at the United Kingdom Infrared Telescope at wavelengths of 5.0 or 3.4 μm, in order to investigate the nature and distribution of volcanism on Io by observing the occultation of the volcanic hot spots by the limb of Europa. Observations at 3.4 μm on 1991/01/08 detected a possible small hot spot in the northern hemisphere. Observations at 5.0 μm on 1991/02/27 detected and resolved the major hot spot Loki, which had a diameter of 170 km and had three times its Voyager 1 flux, and also detected the Voyager hot spot Pele at about half its Voyager 1 flux. A 5.0-μm occultation of Pele on 1991/03/06, when Loki was not occulted, indicated no significant flux change since the week before. Infrared images of Io obtained at the NASA Infrared Telescope Facility between October 1990 and April 1991 show that the Europa occultations occurred during a period of unusually high activity at Loki. Loki showed very little thermal emission in observations between 1990/10/12 and 1990/11/27, but increased in flux by a factor of 10 in 32 days by 1991/12/29. Loki then remained bright in all observations until 1991/03/26, but had begun to fade on 1991/04/09. Such rapid variations in flux over such a large area are remarkable. Multiwavelength observations indicate that Loki increased in temperature during the brightening, and that materials hotter than 630 K were exposed at Loki. The possible "Pele-type" volcanoes Surt and Aten, unlike Pele, were not detected, with 3.8 μm flux upper limits of about 8 GW μm-1 str-1.},
	language = {en},
	number = {1},
	urldate = {2020-02-06},
	journal = {Icarus},
	author = {Spencer, John R. and Clark, Beth E. and Woodney, Laura M. and Sinton, William M. and Toomey, D.},
	month = jan,
	year = {1994},
	pages = {195--208},
	file = {main.pdf:/Users/fb90/Zotero/storage/D98YYVHA/main.pdf:application/pdf;ScienceDirect Snapshot:/Users/fb90/Zotero/storage/TQU32RPH/S0019103584710165.html:text/html}
}

@article{rathbun2004a,
	title = {Io and {Loki} in 2003 as {Seen} from the {Infrared} {Telescope} {Facility} {Using} {Mutual} {Satellite} and {Jupiter} {Occultations}},
	volume = {35},
	url = {http://adsabs.harvard.edu/abs/2004LPI....35.1698R},
	abstract = {We observed Io on 16 nights in 2003 at the NASA IRTF using both Jupiter
occultations and mutual satellite occultations. Measurements of the Loki
hotspot continue to deviate from the previous decade's 540 day period.
No hotspots were detected during mutual occultations.},
	urldate = {2020-02-06},
	author = {Rathbun, J. A. and Ellis, C. T. and Johnson, S. T. and Spencer, J. R.},
	month = mar,
	year = {2004},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/M98B25QK/Rathbun et al. - 2004 - Io and Loki in 2003 as Seen from the Infrared Tele.pdf:application/pdf}
}

@book{2011,
	address = {Washington, D.C.},
	title = {Vision and {Voyages} for {Planetary} {Science} in the {Decade} 2013-2022},
	isbn = {978-0-309-22464-2},
	url = {http://www.nap.edu/catalog/13117},
	language = {en},
	urldate = {2020-02-06},
	publisher = {National Academies Press},
	month = dec,
	year = {2011},
	doi = {10.17226/13117},
	file = {2011 - Vision and Voyages for Planetary Science in the De.pdf:/Users/fb90/Zotero/storage/T6FYPTI9/2011 - Vision and Voyages for Planetary Science in the De.pdf:application/pdf}
}

@article{howell2016,
	title = {Jupiter and {Mutual} {Satellite} {Occultations} of {Io} from 1985 to 2015},
	volume = {48},
	url = {http://adsabs.harvard.edu/abs/2016DPS....4842921H},
	abstract = {Occultations of Io by Jupiter and by other satellites provide a long-term record of the brightness of individual volcanic hotspots. They also provide our highest spatial resolution observations of individual volcanic centers such as Loki. We are in the process of reanalyzing observations spanning the years 1985 through 2015 for submission to the NASA Planetary Data System. The Jupiter occultation observations have spatial resolution limited to roughly the Jupiter atmospheric scale height (22 km) but as these events occur every Io orbit we have data on over 100. They include observations from the NASA-IRTF, WIRO, Lowell, and other telescopes on Mauna Kea. Part of this data set originally revealed the semi-periodic nature of the activity at Loki (Rathbun et al. 2002). A series of mutual satellite occultations occurs only every six years but the sharp limb of the other satellite allows for much higher spatial resolution. The original analysis was limited by
inaccuracies in the satellite ephemerides but improvements now allow us to more reliably assign brightnesses to individual hotspots. They also allow improved image reconstructions of individual spots from mutual events. We will report on our tests of that better ephemeris, the improved assignment of hotspot brightnesses, and the reconstructed mutual event images.},
	urldate = {2020-02-07},
	author = {Howell, Robert R. and Rathbun, Julie A. and Spencer, John R.},
	month = oct,
	year = {2016},
	pages = {429.21}
}

@article{robert2017,
	title = {{CCD} astrometric observations of {Amalthea} and {Thebe} in the \textbf{{Gaia} era}},
	issn = {0035-8711, 1365-2966},
	url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx123},
	doi = {10.1093/mnras/stx123},
	abstract = {In the framework of the 2014–2015 campaign of mutual events, we observed Jupiter’s inner satellites Amalthea (JV) and Thebe (JXIV). We focused on estimating whether the positioning accuracy determined from direct astrometry could compete with that derived from photometric observations of eclipses, for dynamical purposes. We present the analysis of 35 observations of Amalthea and 19 observations of Thebe realized with the 1-m telescope at the Pic du Midi observatory during three nights in 2015, January and April. The images were reduced through an optimal process that includes image and spherical corrections using the Gaia-DR1 catalogue to provide the most accurate equatorial (RA, Dec.) positions. We compared the observed positions of both satellites with the theoretical positions from JPL JUP310 satellite ephemerides and from the IMCCE INPOP13c planetary ephemeris. The values of rms (O−C) in equatorial positions are ±112 mas for the Amalthea observations, or 330 km at Jupiter, and ±90 mas for the Thebe observations, or 270 km at Jupiter. Using the Gaia-DR1 catalogue allowed us to eliminate systematic errors due to the star references up to 120 mas, or 350 km at Jupiter, by comparison with the UCAC4 catalogue.},
	language = {en},
	urldate = {2020-02-07},
	journal = {Mon. Not. R. Astron. Soc.},
	author = {Robert, V. and Saquet, E. and Colas, F. and Arlot, J.-E.},
	month = jan,
	year = {2017},
	pages = {stx123},
	annote = {Says that occultation determined orbits are more precise than JPL Horizons and alternatives.},
	file = {Robert et al. - 2017 - CCD astrometric observations of Amalthea and Thebe.pdf:/Users/fb90/Zotero/storage/XNW2DH8J/Robert et al. - 2017 - CCD astrometric observations of Amalthea and Thebe.pdf:application/pdf}
}

@article{saquet2018,
	title = {The {PHEMU15} catalogue and astrometric results of the {Jupiter}'s {Galilean} satellite mutual occultation and eclipse observations made in 2014–2015},
	volume = {474},
	issn = {0035-8711, 1365-2966},
	url = {http://academic.oup.com/mnras/article/474/4/4730/4644838},
	doi = {10.1093/mnras/stx2957},
	abstract = {During the 2014–2015 mutual events season, the Institut de Me´canique Ce´leste et de Calcul des E´ phe´me´rides (IMCCE), Paris, France, and the Sternberg Astronomical Institute (SAI), Moscow, Russia, led an international observation campaign to record ground-based photometric observations of Galilean moon mutual occultations and eclipses. We focused on processing the complete photometric observations data base to compute new accurate astrometric positions. We used our method to derive astrometric positions from the light curves of the events.},
	language = {en},
	number = {4},
	urldate = {2020-02-07},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Saquet, E and Emelyanov, N and Robert, V and Arlot, J-E and Anbazhagan, P and Baillié, K and Bardecker, J and Berezhnoy, A A and Bretton, M and Campos, F and Capannoli, L and Carry, B and Castet, M and Charbonnier, Y and Chernikov, M M and Christou, A and Colas, F and Coliac, J-F and Dangl, G and Dechambre, O and Delcroix, M and Dias-Oliveira, A and Drillaud, C and Duchemin, Y and Dunford, R and Dupouy, P and Ellington, C and Fabre, P and Filippov, V A and Finnegan, J and Foglia, S and Font, D and Gaillard, B and Galli, G and Garlitz, J and Gasmi, A and Gaspar, H S and Gault, D and Gazeas, K and George, T and Gorda, S Y and Gorshanov, D L and Gualdoni, C and Guhl, K and Halir, K and Hanna, W and Henry, X and Herald, D and Houdin, G and Ito, Y and Izmailov, I S and Jacobsen, J and Jones, A and Kamoun, S and Kardasis, E and Karimov, A M and Khovritchev, M Y and Kulikova, A M and Laborde, J and Lainey, V and Lavayssiere, M and Le Guen, P and Leroy, A and Loader, B and Lopez, O C and Lyashenko, A Y and Lyssenko, P G and Machado, D I and Maigurova, N and Manek, J and Marchini, A and Midavaine, T and Montier, J and Morgado, B E and Naumov, K N and Nedelcu, A and Newman, J and Ohlert, J M and Oksanen, A and Pavlov, H and Petrescu, E and Pomazan, A and Popescu, M and Pratt, A and Raskhozhev, V N and Resch, J-M and Robilliard, D and Roschina, E and Rothenberg, E and Rottenborn, M and Rusov, S A and Saby, F and Saya, L F and Selvakumar, G and Signoret, F and Slesarenko, V Y and Sokov, E N and Soldateschi, J and Sonka, A and Soulie, G and Talbot, J and Tejfel, V G and Thuillot, W and Timerson, B and Toma, R and Torsellini, S and Trabuco, L L and Traverse, P and Tsamis, V and Unwin, M and Abbeel, F Van Den and Vandenbruaene, H and Vasundhara, R and Velikodsky, Y I and Vienne, A and Vilar, J and Vugnon, J-M and Wuensche, N and Zeleny, P},
	month = mar,
	year = {2018},
	pages = {4730--4739},
	file = {Saquet et al. - 2018 - The PHEMU15 catalogue and astrometric results of t.pdf:/Users/fb90/Zotero/storage/7M9FVJ59/Saquet et al. - 2018 - The PHEMU15 catalogue and astrometric results of t.pdf:application/pdf}
}

@article{nelson1996,
	title = {Compositional {Mapping} of {Jupiter}'s {Satellite} {Io} {Utilizing} {High} {Speed} {Multifilter} {Photometry} during {Mutual} {Satellite} {Occultations}, 1990–1991},
	volume = {123},
	issn = {00191035},
	url = {https://linkinghub.elsevier.com/retrieve/pii/S0019103596901797},
	doi = {10.1006/icar.1996.0179},
	language = {en},
	number = {2},
	urldate = {2020-02-11},
	journal = {Icarus},
	author = {Nelson, Robert M. and Wallis, Brad D. and Barker, Edwin S. and Horn, Linda J. and Smythe, William D. and Lane, Arthur L. and Hapke, Bruce W.},
	month = oct,
	year = {1996},
	pages = {568--577},
	file = {Nelson et al. - 1996 - Compositional Mapping of Jupiter's Satellite Io Ut.pdf:/Users/fb90/Zotero/storage/47GCRGPD/Nelson et al. - 1996 - Compositional Mapping of Jupiter's Satellite Io Ut.pdf:application/pdf}
}

@article{arlot,
	title = {Observations of the {Volcanoes} of lo, {Loki} and {Pele}, {Made} in 1991 at the {ES0} during an {Occultation} by {Europa}},
	language = {en},
	author = {Arlot, J E and Thuillot, W and Colas, F and Vu, D T},
	pages = {10},
	file = {Arlot et al. - Observations of the Volcanoes of lo, Loki and Pele.pdf:/Users/fb90/Zotero/storage/SP4XSXV7/Arlot et al. - Observations of the Volcanoes of lo, Loki and Pele.pdf:application/pdf}
}

@article{goguen1988,
	title = {Io hot spots: {Infrared} photometry of satellite occultations},
	volume = {76},
	issn = {00191035},
	shorttitle = {Io hot spots},
	url = {https://linkinghub.elsevier.com/retrieve/pii/0019103588900152},
	doi = {10.1016/0019-1035(88)90015-2},
	language = {en},
	number = {3},
	urldate = {2020-02-11},
	journal = {Icarus},
	author = {Goguen, J.D. and Sinton, W.M. and Matson, D.L. and Howell, R.R. and Dyck, H.M. and Johnson, T.V. and Brown, R.H. and Veeder, G.J. and Lane, A.L. and Nelson, R.M. and Mc Laren, R.A.},
	month = dec,
	year = {1988},
	pages = {465--484},
	file = {Goguen et al. - 1988 - Io hot spots Infrared photometry of satellite occ.pdf:/Users/fb90/Zotero/storage/NRSH7ZFV/Goguen et al. - 1988 - Io hot spots Infrared photometry of satellite occ.pdf:application/pdf}
}

@article{vasundhara2017,
	title = {Analysis of mutual events of {Galilean} satellites observed from {VBO} during 2014–2015},
	volume = {468},
	issn = {0035-8711, 1365-2966},
	url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx437},
	doi = {10.1093/mnras/stx437},
	abstract = {Results of analysis of 23 events of the 2014–2015 mutual event series from the Vainu Bappu Observatory are presented. Our intensity distribution model for the eclipsed/occulted satellite is based on the criterion that it simulates a rotational light curve that matches the ground-based light curve. Dichotomy in the scattering characteristics of the leading and trailing sides explains the basic shape of the rotational light curves of Europa, Ganymede and Callisto. In the case of Io, the albedo map (courtesy United States Geological Survey) along with global values of scattering parameters works well. Mean values of residuals in (O − C) along and perpendicular to the track are found to be −3.3 and −3.4 mas, respectively, compared to ‘L2’ theory for the seven 2E1/2O1 events. The corresponding rms values are 8.7 and 7.8 mas, respectively. For the ﬁve 1E3/1O3 events, the along and perpendicular to the track mean residuals are 5.6 and 3.2 mas, respectively. The corresponding rms residuals are 6.8 and 10.5 mas, respectively. We compare the results using the chosen model (Model 1) with a uniform but limb-darkened disc (Model 2). The residuals with Model 2 of the 2E1/2O1 and 1E3/1O3 events indicate a bias along the satellite track. The extent and direction of bias are consistent with the shift of the light centre from the geometric centre. Results using Model 1, which intrinsically takes into account the intensity distribution, show no such bias.},
	language = {en},
	number = {1},
	urldate = {2020-02-13},
	journal = {Monthly Notices of the Royal Astronomical Society},
	author = {Vasundhara, R. and Selvakumar, G. and Anbazhagan, P.},
	month = jun,
	year = {2017},
	pages = {501--508},
	file = {ms (1).pdf:/Users/fb90/Zotero/storage/ADPJM3WP/ms (1).pdf:application/pdf;Vasundhara et al. - 2017 - Analysis of mutual events of Galilean satellites o.pdf:/Users/fb90/Zotero/storage/HSTMYBEN/Vasundhara et al. - 2017 - Analysis of mutual events of Galilean satellites o.pdf:application/pdf}
}

@article{spencer1994b,
	title = {Io {Hot} {Spots} in 1991: {Results} from {Europa} {Occultation} {Photometry} and {Infrared} {Imaging}},
	volume = {107},
	issn = {0019-1035},
	shorttitle = {Io {Hot} {Spots} in 1991},
	url = {http://www.sciencedirect.com/science/article/pii/S0019103584710165},
	doi = {10.1006/icar.1994.1016},
	abstract = {During the winter of 1991 an unusually favorable series of occultations of Io by Europa took place. We obtained infrared photometry of four of these events at the United Kingdom Infrared Telescope at wavelengths of 5.0 or 3.4 μm, in order to investigate the nature and distribution of volcanism on Io by observing the occultation of the volcanic hot spots by the limb of Europa. Observations at 3.4 μm on 1991/01/08 detected a possible small hot spot in the northern hemisphere. Observations at 5.0 μm on 1991/02/27 detected and resolved the major hot spot Loki, which had a diameter of 170 km and had three times its Voyager 1 flux, and also detected the Voyager hot spot Pele at about half its Voyager 1 flux. A 5.0-μm occultation of Pele on 1991/03/06, when Loki was not occulted, indicated no significant flux change since the week before. Infrared images of Io obtained at the NASA Infrared Telescope Facility between October 1990 and April 1991 show that the Europa occultations occurred during a period of unusually high activity at Loki. Loki showed very little thermal emission in observations between 1990/10/12 and 1990/11/27, but increased in flux by a factor of 10 in 32 days by 1991/12/29. Loki then remained bright in all observations until 1991/03/26, but had begun to fade on 1991/04/09. Such rapid variations in flux over such a large area are remarkable. Multiwavelength observations indicate that Loki increased in temperature during the brightening, and that materials hotter than 630 K were exposed at Loki. The possible "Pele-type" volcanoes Surt and Aten, unlike Pele, were not detected, with 3.8 μm flux upper limits of about 8 GW μm-1 str-1.},
	language = {en},
	number = {1},
	urldate = {2020-02-04},
	journal = {Icarus},
	author = {Spencer, John R. and Clark, Beth E. and Woodney, Laura M. and Sinton, William M. and Toomey, D.},
	month = jan,
	year = {1994},
	pages = {195--208},
	file = {main.pdf:/Users/fb90/Zotero/storage/4WFVIJDF/main.pdf:application/pdf}
}

@article{morgado2016a,
	title = {Astrometry of mutual approximations between natural satellites. {Application} to the {Galilean} moons},
	volume = {460},
	issn = {0035-8711, 1365-2966},
	url = {https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw1244},
	doi = {10.1093/mnras/stw1244},
	abstract = {Typically we can deliver astrometric positions of natural satellites with errors in the 50–150 mas range. Apparent distances from mutual phenomena, have much smaller errors, less than 10 mas. However, this method can only be applied during the equinox of the planets. We developed a method that can provide accurate astrometric data for natural satellites – the mutual approximations. The method can be applied when any two satellites pass close by each other in the apparent sky plane. The fundamental parameter is the central instant t0 of the passage when the distances reach a minimum. We applied the method for the Galilean moons. All observations were made with a 0.6 m telescope with a narrow-band ﬁlter centred at 889 nm with width of 15 nm which attenuated Jupiter’s scattered light. We obtained central instants for 14 mutual approximations observed in 2014–2015. We determined t0 with an average precision of 3.42 mas (10.43 km). For comparison, we also applied the method for 5 occultations in the 2009 mutual phenomena campaign and for 22 occultations in the 2014–2015 campaign. The comparisons of t0 determined by our method with the results from mutual phenomena show an agreement by less than 1σ error in t0, typically less than 10 mas. This new method is particularly suitable for observations by small telescopes.},
	language = {en},
	number = {4},
	urldate = {2020-02-12},
	journal = {Mon. Not. R. Astron. Soc.},
	author = {Morgado, B. and Assafin, M. and Vieira-Martins, R. and Camargo, J. I. B. and Dias-Oliveira, A. and Gomes-Júnior, A. R.},
	month = aug,
	year = {2016},
	pages = {4086--4097},
	file = {Morgado et al. - 2016 - Astrometry of mutual approximations between natura.pdf:/Users/fb90/Zotero/storage/UU9NELNW/Morgado et al. - 2016 - Astrometry of mutual approximations between natura.pdf:application/pdf}
}

@article{arlota,
	title = {Astrometry through photometry},
	language = {en},
	author = {Arlot, J E},
	pages = {63},
	file = {Arlot - Astrometry through photometry.pdf:/Users/fb90/Zotero/storage/CB2ALGT3/Arlot - Astrometry through photometry.pdf:application/pdf}
}

@article{farr2018,
	title = {exocartographer: {A} {Bayesian} {Framework} for {Mapping} {Exoplanets} in {Reflected} {Light}},
	volume = {156},
	issn = {1538-3881},
	shorttitle = {exocartographer},
	url = {https://iopscience.iop.org/article/10.3847/1538-3881/aad775},
	doi = {10.3847/1538-3881/aad775},
	abstract = {Future space telescopes will directly image extrasolar planets at visible wavelengths. Time-resolved reﬂected light from an exoplanet encodes information about atmospheric and surface inhomogeneities. Previous research has shown that the light curve of an exoplanet can be inverted to obtain a low-resolution map of the planet, as well as constraints on its spin orientation. Estimating the uncertainty on 2D albedo maps has so far remained elusive. Here, we present exocartographer, a ﬂexible open-source Bayesian framework for solving the exocartography inverse problem. The map is parameterized with equal-area Hierarchical, Equal Area, and isoLatitude Pixelation (HEALPix) pixels. For a ﬁducial map resolution of 192 pixels, a four-parameter Gaussian process describing the spatial scale of albedo variations, and two unknown planetary spin parameters, exocartographer explores a 198-dimensional parameter space. To test the code, we produce a light curve for a cloudless Earth in a face-on orbit with a 90° obliquity. We produce synthetic white-light observations of the planet: ﬁve epochs of observations throughout the planet’s orbit, each consisting of 24 hourly observations with a photometric uncertainty of 1\% (120 data points). We retrieve an albedo map and—for the ﬁrst time—its uncertainties, along with spin constraints. The albedo map is recognizably of Earth, with a typical 90\% uncertainty of 0.14. The retrieved characteristic length scale is ∼9800 km. The obliquity is recovered to be {\textgreater}87°.9 at the 90\% credible level. Despite the uncertainty in the retrieved albedo map, we robustly identify a high-albedo region (the Sahara desert) and a large low-albedo region (the Paciﬁc Ocean).},
	language = {en},
	number = {4},
	urldate = {2020-06-29},
	journal = {AJ},
	author = {Farr, Ben and Farr, Will M. and Cowan, Nicolas B. and Haggard, Hal M. and Robinson, Tyler},
	month = sep,
	year = {2018},
	pages = {146},
	file = {Farr et al. - 2018 - exocartographer A Bayesian Framework for Mapping .pdf:/Users/fb90/Zotero/storage/4HUXEH95/Farr et al. - 2018 - exocartographer A Bayesian Framework for Mapping .pdf:application/pdf}
}

@article{rauscher2018,
	title = {A {More} {Informative} {Map}: {Inverting} {Thermal} {Orbital} {Phase} and {Eclipse} {Light} {Curves} of {Exoplanets}},
	volume = {156},
	issn = {0004-6256},
	shorttitle = {A {More} {Informative} {Map}},
	url = {http://adsabs.harvard.edu/abs/2018AJ....156..235R},
	doi = {10.3847/1538-3881/aae57f},
	abstract = {Only one exoplanet has so far been mapped in both longitude and
latitude, but the James Webb Space Telescope should provide
mapping-quality data for dozens of exoplanets. The thermal phase mapping
problem has previously been solved analytically, with orthogonal maps
(spherical harmonics) yielding orthogonal light curves (sinusoids). The
eclipse mapping problem, let alone combined phase+eclipse mapping, does
not lend itself to such a neat solution. Previous efforts have adopted
either spherical harmonics or various ad hoc map parameterizations, none
of which produce orthogonal light curves. We use principal component
analysis to construct orthogonal “eigencurves,” which we
then use to fit published 8 μm observations of the hot Jupiter HD
189733b. This approach has a few advantages over previously used
techniques: (1) the light curves can be precomputed, accelerating the
fitting process, (2) the eigencurves are orthogonal to each other,
reducing parameter correlations, and (3) the eigencurves are
model-independent and are ranked in order of sensitivity. One notable
result of our analysis is that eclipse-only mapping of HD 189733b is far
more sensitive to the central concentration of dayside flux than to the
eastward offset of that hot spot. Mapping can, in principle, suffer from
degeneracies between spatial patterns and orbital parameters. Previous
mapping efforts using these data have either assumed a circular orbit
and precise inclination, or have been pessimistic about the prospects of
eclipse mapping in the face of uncertain orbital parameters. We show
that for HD 189733b the combined photometry and radial velocity are
sufficiently precise to retire this concern. Lastly, we present the
first map of brightness temperature, and we quantify the amplitude and
longitude offset of the dayside hot spot.},
	urldate = {2020-06-23},
	journal = {The Astronomical Journal},
	author = {Rauscher, Emily and Suri, Veenu and Cowan, Nicolas B.},
	month = nov,
	year = {2018},
	keywords = {eclipses, infrared: planetary systems, methods: data analysis, planets and satellites: atmospheres, planets and satellites: individual: HD 189733b},
	pages = {235},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/UFLQKDZ6/Rauscher et al. - 2018 - A More Informative Map Inverting Thermal Orbital .pdf:application/pdf}
}

@article{zotero-3281
}

@article{foreman-mackey2017,
	title = {Fast and {Scalable} {Gaussian} {Process} {Modeling} with {Applications} to {Astronomical} {Time} {Series}},
	volume = {154},
	issn = {0004-6256},
	url = {http://adsabs.harvard.edu/abs/2017AJ....154..220F},
	doi = {10.3847/1538-3881/aa9332},
	abstract = {The growing field of large-scale time domain astronomy requires methods
for probabilistic data analysis that are computationally tractable, even
with large data sets. Gaussian processes (GPs) are a popular class of
models used for this purpose, but since the computational cost scales,
in general, as the cube of the number of data points, their application
has been limited to small data sets. In this paper, we present a novel
method for GPs modeling in one dimension where the computational
requirements scale linearly with the size of the data set. We
demonstrate the method by applying it to simulated and real astronomical
time series data sets. These demonstrations are examples of
probabilistic inference of stellar rotation periods, asteroseismic
oscillation spectra, and transiting planet parameters. The method
exploits structure in the problem when the covariance function is
expressed as a mixture of complex exponentials, without requiring evenly
spaced observations or uniform noise. This form of covariance arises
naturally when the process is a mixture of stochastically driven damped
harmonic oscillators—providing a physical motivation for and
interpretation of this choice—but we also demonstrate that it can
be a useful effective model in some other cases. We present a
mathematical description of the method and compare it to existing
scalable GP methods. The method is fast and interpretable, with a range
of potential applications within astronomical data analysis and beyond.
We provide well-tested and documented open-source implementations of
this method in C++, Python, and Julia.},
	urldate = {2020-06-20},
	journal = {The Astronomical Journal},
	author = {Foreman-Mackey, Daniel and Agol, Eric and Ambikasaran, Sivaram and Angus, Ruth},
	month = dec,
	year = {2017},
	keywords = {planetary systems, methods: data analysis, asteroseismology, methods: statistical, stars: rotation},
	pages = {220},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/ZFDGTC4P/Foreman-Mackey et al. - 2017 - Fast and Scalable Gaussian Process Modeling with A.pdf:application/pdf}
}

@article{acosta-pulido2017,
	title = {A {New} {Statistical} {Approach} to the {Optical} {Spectral} {Variability} in {Blazars}},
	volume = {5},
	url = {http://adsabs.harvard.edu/abs/2017Galax...5....1A},
	doi = {10.3390/galaxies5010001},
	abstract = {We present a spectral variability study of a sample of about 25 bright blazars, based on optical spectroscopy. Observations cover the period from the end of 2008 to mid 2015, with an approximately monthly cadence. Emission lines have been identified and measured in the spectra, which permits us to classify the sources into BL Lac-type or FSRQs, according to the commonly used EW limit. We have obtained synthetic photometry and produced colour-magnitude diagrams which show different trends
associated with the object classes: generally, BL Lacs tend to become bluer when brighter and FSRQs become redder when brighter, although several objects exhibit both trends, depending on brightness. We have also applied a pattern recognition algorithm to obtain the minimum number of physical components which can explain the variability of the optical spectrum. We have used NMF (Non-Negative Matrix Factorization) instead of PCA (Principal Component Analysis) to avoid un-realistic negative components. For most targets we found that 2 or 3
meta-components are enough to explain the observed spectral variability.},
	urldate = {2020-06-19},
	journal = {Galaxies},
	author = {Acosta-Pulido, Jose and Castro Segura, Noel and Carnerero, Maria and Raiteri, Claudia},
	month = jan,
	year = {2017},
	pages = {1},
	file = {Full Text:/Users/fb90/Zotero/storage/2B99IFR7/Acosta-Pulido et al. - 2017 - A New Statistical Approach to the Optical Spectral.pdf:application/pdf}
}

@article{selim2017,
	title = {Automated morphological classification of galaxies based on projection gradient nonnegative matrix factorization algorithm},
	volume = {43},
	issn = {0922-6435},
	url = {http://adsabs.harvard.edu/abs/2017ExA....43..131S},
	doi = {10.1007/s10686-017-9524-7},
	abstract = {The development of automated morphological classification schemes can
successfully distinguish between morphological types of galaxies and can
be used for studies of the formation and subsequent evolution of
galaxies in our universe. In this paper, we present a new automated
machine supervised learning astronomical classification scheme based on
the Nonnegative Matrix Factorization algorithm. This scheme is making
distinctions between all types roughly corresponding to Hubble types
such as elliptical, lenticulars, spiral, and irregular galaxies. The
proposed algorithm is performed on two examples with different number of
image (small dataset contains 110 image and large dataset contains 700
images). The experimental results show that galaxy images from EFIGI
catalog can be classified automatically with an accuracy of ∼93\% for
small and ∼92\% for large number. These results are in good agreement
when compared with the visual classifications.},
	urldate = {2020-06-19},
	journal = {Experimental Astronomy},
	author = {Selim, I. M. and Abd El Aziz, Mohamed},
	month = apr,
	year = {2017},
	keywords = {Galaxies: classification, Nonnegative matrix factorization (NMF): image processing},
	pages = {131--144}
}

@article{ren2018,
	title = {Non-negative {Matrix} {Factorization}: {Robust} {Extraction} of {Extended} {Structures}},
	volume = {852},
	issn = {0004-637X},
	shorttitle = {Non-negative {Matrix} {Factorization}},
	url = {http://adsabs.harvard.edu/abs/2018ApJ...852..104R},
	doi = {10.3847/1538-4357/aaa1f2},
	abstract = {We apply the vectorized non-negative matrix factorization (NMF) method to the post-processing of the direct imaging data of exoplanetary systems such as circumstellar disks. NMF is an iterative approach, which first creates a nonorthogonal and non-negative basis of components using the given reference images and then models a target with the components. The constructed model is then rescaled with a factor to compensate for the contribution from the disks. We compare NMF with existing methods (classical reference differential imaging method, and the
Karhunen-Loève image projection algorithm) using synthetic
circumstellar disks and demonstrate the superiority of NMF: with no need of prior selection of references, NMF not only can detect fainter circumstellar disks but also better preserves their morphology and does not require forward modeling. As an application to a well-known disk example, we process the archival Hubble Space Telescope STIS
coronagraphic observations of HD 181327 with different methods and compare them, and NMF is able to extract some circumstellar materials inside the primary ring for the first time. In an appendix, we
mathematically investigate the stability of NMF components during the iteration and the linearity of NMF modeling.},
	urldate = {2020-06-19},
	journal = {The Astrophysical Journal},
	author = {Ren, Bin and Pueyo, Laurent and Zhu, Guangtun Ben and Debes, John and Duchêne, Gaspard},
	month = jan,
	year = {2018},
	keywords = {protoplanetary disks, stars: imaging, stars: individual: HD 181327, techniques: image processing},
	pages = {104},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/CEG8FYEP/Ren et al. - 2018 - Non-negative Matrix Factorization Robust Extracti.pdf:application/pdf}
}

@article{ren2020,
	title = {Using {Data} {Imputation} for {Signal} {Separation} in {High}-contrast {Imaging}},
	volume = {892},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2020ApJ...892...74R},
	doi = {10.3847/1538-4357/ab7024},
	abstract = {To characterize circumstellar systems in high-contrast imaging, the fundamental step is to construct a best point-spread function (PSF) template for the noncircumstellar signals (i.e., starlight and speckles) and separate it from the observation. With existing PSF construction methods, the circumstellar signals (e.g., planets, circumstellar disks) are unavoidably altered by overfitting and/or self-subtraction, making forward modeling a necessity to recover these signals. We present a forward modeling-free solution to these problems with data imputation using sequential nonnegative matrix factorization (DI-sNMF), which first converts this signal separation problem to a "missing data" problem in statistics by flagging the regions that host circumstellar signals as missing data, then attributes PSF signals to these regions. We
mathematically prove it to have negligible alteration to circumstellar signals when the imputation region is relatively small, which thus enables precise measurement of these circumstellar objects. We apply it to simulated point-source and circumstellar disk observations to demonstrate its proper recovery of them. We apply it to Gemini Planet Imager K1-band observations of the debris disk surrounding HR 4796A, finding a tentative trend that the dust is more forward scattering as the wavelength increases. We expect DI-sNMF to be applicable to other general scenarios where the separation of signals is needed.},
	urldate = {2020-06-19},
	journal = {The Astrophysical Journal},
	author = {Ren, Bin and Pueyo, Laurent and Chen, Christine and Choquet, Élodie and Debes, John H. and Duchêne, Gaspard and Ménard, François and Perrin, Marshall D.},
	month = apr,
	year = {2020},
	pages = {74},
	file = {Submitted Version:/Users/fb90/Zotero/storage/A2FQV5FC/Ren et al. - 2020 - Using Data Imputation for Signal Separation in Hig.pdf:application/pdf}
}

@article{vavasis2009,
	title = {On the {Complexity} of {Nonnegative} {Matrix} {Factorization}},
	volume = {20},
	issn = {1052-6234},
	abstract = {Nonnegative matrix factorization (NMF) has become a prominent technique for the analysis of image databases, text databases, and other information retrieval and clustering applications. The problem is most naturally posed as continuous optimization. In this report, we define an exact version of NMF. Then we establish several results about exact NMF: (i) that it is equivalent to a problem in polyhedral combinatorics; (ii) that it is NP-hard; and (iii) that a polynomial-time local search heuristic exists.},
	number = {3},
	journal = {SIAM J. on Optimization},
	author = {Vavasis, Stephen A.},
	month = oct,
	year = {2009},
	keywords = {complexity, data mining, feature detection, nonnegative matrix factorization, nonnegative rank, NP-hard},
	pages = {1364--1377}
}

@incollection{lee2001,
	title = {Algorithms for {Non}-negative {Matrix} {Factorization}},
	url = {http://papers.nips.cc/paper/1861-algorithms-for-non-negative-matrix-factorization.pdf},
	urldate = {2020-06-19},
	booktitle = {Advances in {Neural} {Information} {Processing} {Systems} 13},
	publisher = {MIT Press},
	author = {Lee, Daniel D. and Seung, H. Sebastian},
	editor = {Leen, T. K. and Dietterich, T. G. and Tresp, V.},
	year = {2001},
	pages = {556--562},
	file = {NIPS Full Text PDF:/Users/fb90/Zotero/storage/AV3S5J9E/Lee and Seung - 2001 - Algorithms for Non-negative Matrix Factorization.pdf:application/pdf;NIPS Snapshot:/Users/fb90/Zotero/storage/Z6UT86GI/1861-algorithms-for-non-negative-matrix-factorization.html:text/html}
}

@article{paatero1994,
	title = {Positive matrix factorization: {A} non-negative factor model with optimal utilization of error estimates of data values},
	volume = {5},
	copyright = {Copyright © 1994 John Wiley \& Sons, Ltd},
	issn = {1099-095X},
	shorttitle = {Positive matrix factorization},
	url = {https://onlinelibrary.wiley.com/doi/abs/10.1002/env.3170050203},
	doi = {10.1002/env.3170050203},
	abstract = {A new variant ‘PMF’ of factor analysis is described. It is assumed that X is a matrix of observed data and σ is the known matrix of standard deviations of elements of X. Both X and σ are of dimensions n × m. The method solves the bilinear matrix problem X = GF + E where G is the unknown left hand factor matrix (scores) of dimensions n × p, F is the unknown right hand factor matrix (loadings) of dimensions p × m, and E is the matrix of residuals. The problem is solved in the weighted least squares sense: G and F are determined so that the Frobenius norm of E divided (element-by-element) by σ is minimized. Furthermore, the solution is constrained so that all the elements of G and F are required to be non-negative. It is shown that the solutions by PMF are usually different from any solutions produced by the customary factor analysis (FA, i.e. principal component analysis (PCA) followed by rotations). Usually PMF produces a better fit to the data than FA. Also, the result of PF is guaranteed to be non-negative, while the result of FA often cannot be rotated so that all negative entries would be eliminated. Different possible application areas of the new method are briefly discussed. In environmental data, the error estimates of data can be widely varying and non-negativity is often an essential feature of the underlying models. Thus it is concluded that PMF is better suited than FA or PCA in many environmental applications. Examples of successful applications of PMF are shown in companion papers.},
	language = {en},
	number = {2},
	urldate = {2020-06-19},
	journal = {Environmetrics},
	author = {Paatero, Pentti and Tapper, Unto},
	year = {1994},
	note = {\_eprint: https://onlinelibrary.wiley.com/doi/pdf/10.1002/env.3170050203},
	keywords = {Alternating regression, Error estimates, Factor analysis, Principal component analysis, Repetitive measurements, Scaling, Weighted least squares},
	pages = {111--126},
	file = {Snapshot:/Users/fb90/Zotero/storage/E3DBKKU7/env.html:text/html}
}

@misc{zotero-3291,
	title = {Positive matrix factorization: {A} non‐negative factor model with optimal utilization of error estimates of data values - {Paatero} - 1994 - {Environmetrics} - {Wiley} {Online} {Library}},
	url = {https://onlinelibrary.wiley.com/doi/abs/10.1002/env.3170050203},
	urldate = {2020-06-19},
	file = {Positive matrix factorization\: A non‐negative factor model with optimal utilization of error estimates of data values - Paatero - 1994 - Environmetrics - Wiley Online Library:/Users/fb90/Zotero/storage/7Z5W46S9/env.html:text/html}
}

@article{folkner2014,
	title = {The {Planetary} and {Lunar} {Ephemerides} {DE430} and {DE431}},
	volume = {196},
	url = {http://adsabs.harvard.edu/abs/2014IPNPR.196C...1F},
	abstract = {The planetary and lunar ephemerides DE430 and DE431 are generated by fitting numerically integrated orbits of the Moon and planets to observations. The present-day lunar orbit is known to submeter accuracy through fitting lunar laser ranging data with an updated lunar gravity field from the Gravity Recovery and Interior Laboratory (GRAIL) mission. The orbits of the inner planets are known to subkilometer accuracy through fitting radio tracking measurements of spacecraft in orbit about them. Very long baseline interferometry measurements of spacecraft at Mars allow the orientation of the ephemeris to be tied to the
International Celestial Reference Frame with an accuracy of 0''.0002. This orientation is the limiting error source for the orbits of the terrestrial planets, and corresponds to orbit uncertainties of a few hundred meters. The orbits of Jupiter and Saturn are determined to accuracies of tens of kilometers as a result of fitting spacecraft tracking data. The orbits of Uranus, Neptune, and Pluto are determined primarily from astrometric observations, for which measurement
uncertainties due to the Earth's atmosphere, combined with star catalog uncertainties, limit position accuracies to several thousand kilometers. DE430 and DE431 differ in their integrated time span and lunar dynamical modeling. The dynamical model for DE430 included a damping term between the Moon's liquid core and solid mantle that gives the best fit to lunar laser ranging data but that is not suitable for backward integration of more than a few centuries. The ephemeris DE431 is similar to DE430 but was fit without the core/mantle damping term, so the lunar orbit is less accurate than in DE430 for times near the current epoch, but is more suitable for times more than a few centuries in the past. DE431 is a longer integration (covering years -13,200 to +17,191) than DE430 (covering years 1550 to 2650).},
	urldate = {2020-06-16},
	journal = {Interplanetary Network Progress Report},
	author = {Folkner, W. M. and Williams, J. G. and Boggs, D. H. and Park, R. S. and Kuchynka, P.},
	month = feb,
	year = {2014},
	pages = {1--81},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/5NFTKTQX/Folkner et al. - 2014 - The Planetary and Lunar Ephemerides DE430 and DE43.pdf:application/pdf}
}

@article{dobos2019,
	title = {Tidal heating and the habitability of the {TRAPPIST}-1 exoplanets},
	volume = {624},
	issn = {0004-6361},
	url = {http://adsabs.harvard.edu/abs/2019A%26A...624A...2D},
	doi = {10.1051/0004-6361/201834254},
	abstract = {Context. New estimates of the masses and radii of the seven planets orbiting the ultracool M-dwarf TRAPPIST-1 star permit improved modelling of their compositions, heating by tidal dissipation, and removal of tidal heat by solid-state convection. Aims: Here we compute the heat flux due to insolation and tidal heating for the inner four planets. Methods: We apply a Maxwell viscoelastic rheology to compute the tidal response of the planets using the volume-weighted average of the viscosities and rigidities of the metal, rock,
high-pressure ice, and liquid water/ice I layers. Results: We show that TRAPPIST-1d and e can avoid entering a runaway greenhouse state. Planet e is the most likely to support a habitable environment, with Earth-like surface temperatures and possibly liquid water oceans. Planet d also avoids a runaway greenhouse, if its surface reflectance is at least as high as that of the Earth. Planets b and c, closer to the star, have heat fluxes high enough to trigger a runaway greenhouse and to support volcanism on the surfaces of their rock layers, rendering them too warm for life. Planets f, g, and h are too far from the star to experience significant tidal heating, and likely have solid ice surfaces with possible subsurface liquid water oceans.},
	urldate = {2020-06-06},
	journal = {Astronomy and Astrophysics},
	author = {Dobos, Vera and Barr, Amy C. and Kiss, László L.},
	month = apr,
	year = {2019},
	keywords = {astrobiology, methods: numerical, planets and satellites: interiors, planets and satellites: terrestrial planets},
	pages = {A2},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/QB6M35BC/Dobos et al. - 2019 - Tidal heating and the habitability of the TRAPPIST.pdf:application/pdf}
}

@article{kislyakova2017,
	title = {Magma oceans and enhanced volcanism on {TRAPPIST}-1 planets due to induction heating},
	volume = {1},
	issn = {2397-3366},
	url = {http://adsabs.harvard.edu/abs/2017NatAs...1..878K},
	doi = {10.1038/s41550-017-0284-0},
	abstract = {Low-mass M stars are plentiful in the Universe and often host small,
rocky planets detectable with current instrumentation. These stars host
magnetic fields, some of which have been observed to exceed a few
hundred gauss. Recently, seven small planets have been discovered
orbiting the ultra-cool M dwarf TRAPPIST-1, which has an observed
magnetic field of 600 G. We suggest electromagnetic induction heating as
an energy source inside these planets. If the stellar rotation and
magnetic dipole axes are inclined with respect to each other, induction
heating can melt the upper mantle and enormously increase volcanic
activity, sometimes producing a magma ocean below the planetary surface.
We show that induction heating leads the four innermost TRAPPIST-1
planets, one of which is in the habitable zone, either to evolve towards
a molten mantle planet, or to experience increased outgassing and
volcanic activity, while the three outermost planets remain mostly
unaffected.},
	urldate = {2020-06-06},
	journal = {Nature Astronomy},
	author = {Kislyakova, K. G. and Noack, L. and Johnstone, C. P. and Zaitsev, V. V. and Fossati, L. and Lammer, H. and Khodachenko, M. L. and Odert, P. and Güdel, M.},
	month = oct,
	year = {2017},
	pages = {878--885},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/ZNJ65MUU/Kislyakova et al. - 2017 - Magma oceans and enhanced volcanism on TRAPPIST-1 .pdf:application/pdf}
}

@article{demory2016,
	title = {Variability in the super-{Earth} 55 {Cnc} e},
	volume = {455},
	issn = {0035-8711},
	url = {https://academic.oup.com/mnras/article/455/2/2018/1106184},
	doi = {10.1093/mnras/stv2239},
	abstract = {Abstract.  Considerable progress has been made in recent years in observations of atmospheric signatures of giant exoplanets, but processes in rocky exoplanets},
	language = {en},
	number = {2},
	urldate = {2020-06-06},
	journal = {Mon Not R Astron Soc},
	author = {Demory, Brice-Olivier and Gillon, Michael and Madhusudhan, Nikku and Queloz, Didier},
	month = jan,
	year = {2016},
	note = {Publisher: Oxford Academic},
	pages = {2018--2027},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/SZV5YSMC/Demory et al. - 2016 - Variability in the super-Earth 55 Cnc e.pdf:application/pdf;Snapshot:/Users/fb90/Zotero/storage/CU4ZYEM7/1106184.html:text/html}
}

@article{oza2019,
	title = {Sodium and {Potassium} {Signatures} of {Volcanic} {Satellites} {Orbiting} {Close}-in {Gas} {Giant} {Exoplanets}},
	volume = {885},
	issn = {0004-637X},
	url = {http://adsabs.harvard.edu/abs/2019ApJ...885..168O},
	doi = {10.3847/1538-4357/ab40cc},
	abstract = {Extrasolar satellites are generally too small to be detected by nominal
searches. By analogy to the most active body in the solar system, Io, we
describe how sodium (Na I) and potassium (K I) gas could be a signature
of the geological activity venting from an otherwise hidden exo-Io.
Analyzing ∼a dozen close-in gas giants hosting robust alkaline
detections, we show that an Io-sized satellite can be stable against
orbital decay below a planetary tidal \{\{ {\textbackslash}mathcal Q \}\}p≲
\{10\}11. This tidal energy is also focused into the satellite
driving an ∼105±2 higher mass-loss rate than
Io’s supply to Jupiter’s Na exosphere based on simple
atmospheric loss estimates. The remarkable consequence is that several
exo-Io column densities are, on average, more than sufficient to provide
the ∼1010±1 Na cm‑2 required by
the equivalent width of exoplanet transmission spectra. Furthermore, the
benchmark observations of both Jupiter’s extended (∼1000 R
J) Na exosphere and Jupiter’s atmosphere in
transmission spectroscopy yield similar Na column densities that are
purely exogenic in nature. As a proof of concept, we fit the
“high-altitude” Na at WASP-49b with an ionization-limited
cloud similar to the observed Na profile about Io. Moving forward, we
strongly encourage time-dependent ingress and egress monitoring along
with spectroscopic searches for other volcanic volatiles.},
	urldate = {2020-06-06},
	journal = {The Astrophysical Journal},
	author = {Oza, Apurva V. and Johnson, Robert E. and Lellouch, Emmanuel and Schmidt, Carl and Schneider, Nick and Huang, Chenliang and Gamborino, Diana and Gebek, Andrea and Wyttenbach, Aurelien and Demory, Brice-Olivier and Mordasini, Christoph and Saxena, Prabal and Dubois, David and Moullet, Arielle and Thomas, Nicolas},
	month = nov,
	year = {2019},
	keywords = {planets and satellites: atmospheres, planets and satellites: composition, planets and satellites: detection, planets and satellites: dynamical evolution and stability, planets and satellites: magnetic fields, planets and satellites: physical evolution},
	pages = {168},
	file = {Full Text PDF:/Users/fb90/Zotero/storage/U66LGGPE/Oza et al. - 2019 - Sodium and Potassium Signatures of Volcanic Satell.pdf:application/pdf}
}

@article{barnes2010,
	title = {{CoRoT}-7b: {SUPER}-{EARTH} {OR} {SUPER}-{Io}?},
	volume = {709},
	issn = {2041-8205, 2041-8213},
	shorttitle = {{CoRoT}-7b},
	url = {https://iopscience.iop.org/article/10.1088/2041-8205/709/2/L95},
	doi = {10.1088/2041-8205/709/2/L95},
	abstract = {CoRoT-7b, a planet about 70\% larger than the Earth orbiting a Sun-like star, is the ﬁrst-discovered rocky exoplanet, and hence has been dubbed a “super-Earth.” Some initial studies suggested that since the planet is so close to its host star, it receives enough insolation to partially melt its surface. However, these past studies failed to take into consideration the role that tides may play in this system. Even if the planet’s eccentricity has always been zero, we show that tidal decay of the semimajor axis could have been large enough that the planet formed on a wider orbit which received less insolation. Moreover, CoRoT-7b could be tidally heated at a rate that dominates its geophysics and drives extreme volcanism. In this case, CoRoT-7b is a “super-Io” that, like Jupiter’s volcanic moon, is dominated by volcanism and rapid resurfacing. Such heating could occur with an eccentricity of just 10−5. This small value could be driven by CoRoT-7c if its own eccentricity is larger than ∼10−4. CoRoT-7b may be the ﬁrst of a class of planetary super-Ios likely to be revealed by the CoRoT and Kepler spacecraft.},
	language = {en},
	number = {2},
	urldate = {2020-06-06},
	journal = {ApJ},
	author = {Barnes, Rory and Raymond, Sean N. and Greenberg, Richard and Jackson, Brian and Kaib, Nathan A.},
	month = feb,
	year = {2010},
	pages = {L95--L98},
	file = {Barnes et al. - 2010 - CoRoT-7b SUPER-EARTH OR SUPER-Io.pdf:/Users/fb90/Zotero/storage/SDI76VVV/Barnes et al. - 2010 - CoRoT-7b SUPER-EARTH OR SUPER-Io.pdf:application/pdf}
}

@article{barnes2010a,
	title = {{CoRoT}-7b: {SUPER}-{EARTH} {OR} {SUPER}-{Io}?},
	volume = {709},
	issn = {2041-8205},
	shorttitle = {{CoRoT}-7b},
	url = {https://doi.org/10.1088%2F2041-8205%2F709%2F2%2Fl95},
	doi = {10.1088/2041-8205/709/2/L95},
	abstract = {CoRoT-7b, a planet about 70\% larger than the Earth orbiting a Sun-like star, is the first-discovered rocky exoplanet, and hence has been dubbed a “super-Earth.” Some initial studies suggested that since the planet is so close to its host star, it receives enough insolation to partially melt its surface. However, these past studies failed to take into consideration the role that tides may play in this system. Even if the planet's eccentricity has always been zero, we show that tidal decay of the semimajor axis could have been large enough that the planet formed on a wider orbit which received less insolation. Moreover, CoRoT-7b could be tidally heated at a rate that dominates its geophysics and drives extreme volcanism. In this case, CoRoT-7b is a “super-Io” that, like Jupiter's volcanic moon, is dominated by volcanism and rapid resurfacing. Such heating could occur with an eccentricity of just 10–5. This small value could be driven by CoRoT-7c if its own eccentricity is larger than ∼10–4. CoRoT-7b may be the first of a class of planetary super-Ios likely to be revealed by the CoRoT and Kepler spacecraft.},
	language = {en},
	number = {2},
	urldate = {2020-06-06},
	journal = {ApJL},
	author = {Barnes, Rory and Raymond, Sean N. and Greenberg, Richard and Jackson, Brian and Kaib, Nathan A.},
	month = jan,
	year = {2010},
	note = {Publisher: IOP Publishing},
	pages = {L95--L98},
	file = {IOP Full Text PDF:/Users/fb90/Zotero/storage/CHTKD62R/Barnes et al. - 2010 - CoRoT-7b SUPER-EARTH OR SUPER-Io.pdf:application/pdf}
}

@article{peale1979,
	title = {Melting of {Io} by tidal dissipation},
	volume = {203},
	issn = {0036-8075},
	url = {http://adsabs.harvard.edu/abs/1979Sci...203..892P},
	doi = {10.1126/science.203.4383.892},
	abstract = {The resonant structure of Io leads to forced eccentricities that are considerably larger than the free values. Although still modest by all standards, these forced eccentricities coupled with the enormous tides induced by Jupiter lead to magnitudes of tidal dissipation that are large enough to completely dominate the thermal history of Io. In the present paper, the forced eccentricities are calculated and then substituted into an expression for the total tidal dissipation. The results point to the possibility that the dissipation of tidal energy in Io may have melted a major fraction of Io's mass.},
	urldate = {2020-06-06},
	journal = {Science},
	author = {Peale, S. J. and Cassen, P. and Reynolds, R. T.},
	month = mar,
	year = {1979},
	keywords = {Io, CORE, Eccentricity, ECCENTRICITY, ENERGY, Energy Dissipation, Galilean Satellites, HEATING, INTERIOR, IO, JUPITER, LIBRATIONS, MANTLE, Melting, MELTING, ORBITS, Planetary Mantles, PREDICTIONS, SATELLITES, Thermal Energy, THERMAL PROPERTIES, TIDAL DISSIPATION, Tides, TIDES, VOLCANISM, VOYAGER 1, Voyager Project},
	pages = {892--894},
	file = {Submitted Version:/Users/fb90/Zotero/storage/4S33YFFI/Peale et al. - 1979 - Melting of Io by tidal dissipation.pdf:application/pdf}
}

@article{misra2015,
	title = {Transient {Sulfate} {Aerosols} as a {Signature} of {Exoplanet} {Volcanism}},
	volume = {15},
	issn = {1531-1074},
	url = {https://www.liebertpub.com/doi/abs/10.1089/ast.2014.1204},
	doi = {10.1089/ast.2014.1204},
	abstract = {Geological activity is thought to be important for the origin of life and for maintaining planetary habitability. We show that transient sulfate aerosols could be a signature of exoplanet volcanism and therefore of a geologically active world. A detection of transient aerosols, if linked to volcanism, could thus aid in habitability evaluations of the exoplanet. On Earth, subduction-induced explosive eruptions inject SO2 directly into the stratosphere, leading to the formation of sulfate aerosols with lifetimes of months to years. We demonstrate that the rapid increase and gradual decrease in sulfate aerosol loading associated with these eruptions may be detectable in transit transmission spectra with future large-aperture telescopes, such as the James Webb Space Telescope (JWST) and European Extremely Large Telescope (E-ELT), for a planetary system at a distance of 10 pc, assuming an Earth-like atmosphere, bulk composition, and size. Specifically, we find that a signal-to-noise ratio of 12.1 and 7.1 could be achieved with E-ELT (assuming photon-limited noise) for an Earth analogue orbiting a Sun-like star and M5V star, respectively, even without multiple transits binned together. We propose that the detection of this transient signal would strongly suggest an exoplanet volcanic eruption, if potential false positives such as dust storms or bolide impacts can be ruled out. Furthermore, because scenarios exist in which O2 can form abiotically in the absence of volcanic activity, a detection of transient aerosols that can be linked to volcanism, along with a detection of O2, would be a more robust biosignature than O2 alone. Key Words: Volcanism—Habitability—Biosignatures—Extrasolar terrestrial planets—Planetary atmospheres. Astrobiology 15, 462–477.},
	number = {6},
	urldate = {2020-06-06},
	journal = {Astrobiology},
	author = {Misra, Amit and Krissansen-Totton, Joshua and Koehler, Matthew C. and Sholes, Steven},
	month = jun,
	year = {2015},
	note = {Publisher: Mary Ann Liebert, Inc., publishers},
	pages = {462--477},
	file = {Snapshot:/Users/fb90/Zotero/storage/I57ZBDAD/ast.2014.html:text/html;Submitted Version:/Users/fb90/Zotero/storage/ZKHZYVIA/Misra et al. - 2015 - Transient Sulfate Aerosols as a Signature of Exopl.pdf:application/pdf}
}

@article{kaltenegger2010a,
	title = {{DETECTING} {VOLCANISM} {ON} {EXTRASOLAR} {PLANETS}},
	volume = {140},
	issn = {1538-3881},
	url = {https://doi.org/10.1088%2F0004-6256%2F140%2F5%2F1370},
	doi = {10.1088/0004-6256/140/5/1370},
	abstract = {The search for extrasolar rocky planets has already found the first transiting rocky super-Earth, Corot 7b, with a surface temperature that allows for magma oceans. Here, we investigate whether we could distinguish rocky planets with recent major volcanism by remote observation. We develop a model for volcanic eruptions on an Earth-like exoplanet based on the present-day Earth and derive the observable features in emergent and transmission spectra for multiple scenarios of gas distribution and cloud cover. We calculate the observation time needed to detect explosive volcanism on exoplanets in primary as well as secondary eclipse and discuss the likelihood of observing volcanism on transiting Earth-sized to super-E