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space_sciences/05819_349.txt | s a density of 2 x lo3 ~rn-~, anionization parameter U=O.Ol, a covering factor of c=0.29, a filling factor of 6.5 x without any radial dependence, and extends from - 153 to - 362 pc from the center. We have also assumed the “low oxygen” abundances adopted by Alexander et al. (ZOOO), in order to be able to compare our r... | |
space_sciences/16633_254.txt | o-bladed propeller powered by a rare-earth-magnet-driven brushlessDC motor supplies AV propulsion. Science cameras are mounted directlyto the underbelly of the fuselage structure behind double-pane transparentwindows. All flight control servo actuators are mounted internal to the fuselage and transmit control forces an... | |
space_sciences/22007_43.txt | s) background-subtracted count images by thecoadded exposure maps to get the final flux images.
2.1. Temperature Map of the Small-scale Structure | |
space_sciences/17151_69.txt | s and line ratios. These equations take intoaccount the correlations between level populations and lineemissivities. Interestingly, the behaviors of uncertainties in level populations and uncertainties in emissivities for transitions fromthe same upper levels are often different and even inverse. Thisis the case, in pa... | |
space_sciences/06304_193.txt | nfrared region of the spectrum (this varies with the optics used), well suited for investigations involving silicon. The Bordeaux implementation uses an external pulse-picker for repetition rate control, but these lasers can be cavity dumped as well. The pulse width of Ti:sapphire lasers is typically less than 100 fs, ... | |
space_sciences/16214_257.txt | f, M. J., Bjorkman, J. E., andWhitney, B.: 2002, ApJ 564, 887Zhu, Z., Nelson, R. P., Hartmann, L., Espaillat,C., and Calvet, N.: 2011, ApJ 729, 47 | |
space_sciences/16639_156.txt | rected [OIII]λ5007 with the BAT 14–195 keV luminosity.Contrary to the results of Heckman et al. (2005), they found onlya weak linear correlation between the reddening-corrected [OIII]luminosity and LX. They suggested that the [OIII] luminosityis affected by extinction poorly corrected by using the Balmerdecrement, and ... | |
space_sciences/05976_90.txt | tuate more than 1 km when it is within approximately 37 hours to TCA).
2.2.2.2 Group 2 (∆EDR > 0.03 W/kg)
For the downtrack component, group 2 represents those objects with a ∆EDR > 0.03 W/kg. Figure 2-5 shows the deviation from the actual miss distance for group 2 conjunctions and also demonstrates that the behavior... | |
space_sciences/16376_251.txt | mptions could haltat smaller sizes.
5.4. Planets in the Cold Disk Systems?
Cold disks must have large inner voids, as inferred fromthe absence of emission at 100μm. In the inner parts of the“cold disk” systems, the planetesimal formation is likely to haveadvanced further, ending up with the formation of planets (J. P.M... | |
space_sciences/00332_61.txt | 0.005 magnitudes for bright stars, while the increased roundofferror contributes another 0.002 magnitudes of uncertainty. Given a limiting accuracy ofabout 0.011 magnitudes determined for multiphot, these uncertainties will contribute littleto the overall error budget.
Overall, the multiphot algorithms are nearly iden... | |
space_sciences/16868_203.txt | rXiv:1303.5088)Press W. H., Teukolsky S. A., Vetterling W. T., Flannery B. P., 2007, Numerical Recipes in C: The Art of Scientific Computing, 3rd edn. CambridgeUniv. Press, New York, NY, USARex M. et al., 2010, A&A, 518, L13Sambruna R. M. et al., | |
space_sciences/13075_53.txt | o the amount of charge. The emission direction of each photoelectron is then estimated from the track image. Thus, this photoelectric polarimeter is simultaneously sensitive to all phases of polarization and docs not require rotation about the Z-axis. Of course, rotation about thc Z-axis would be desirable to allow the... | |
space_sciences/16900_181.txt | e based on an assumption that the absorber can be modeled as a thin resistivemembrane. When the absorber is a pair of orthogonalgrids, it deviates from the ideal membrane model in thefollowing three ways: 1) there is a finite distance betweenthe layers of orthogonal grids, 2) the grids have non-zeropitch and consist of... | |
space_sciences/23281_58.txt | e that both the start and end times of the storms are defined independent of electron and RBC dynamics. Figure 1 shows an example CME storm which occurred on 11 February 2000, and the identification of the start of the storm and end of the storm, t0 and t1 respectively. See figure caption for details. By identifying th... | |
space_sciences/18058_104.txt | n. Soc., 42, 27–32.O’Brien, T. P., and R. L. McPherron (2000), An empirical phase space analysis of ring current dynamics: Solar wind control of injection anddecay, J. Geophys. Res., 105, 7707–7719.Schwenn, R. (2006), Space weather: The solar perspective, Living Rev. Sol. Phys., 3, 2, doi:10.129 | |
space_sciences/09884_167.txt | yman, R. C. Elphic, W. C. Feldman, J.J. Hagerty, MCNPX benchmark for cosmic ray interactions with the Moon, Journal ofGeophysical Research, vol. 111, p. E06004 (2006).[18] L. Sihver, D. Mancusi, T. Sato, K. Niita, H. Iwase, Y. Iwamoto, N. Matsuda, H. Nak | |
space_sciences/21631_192.txt | y.• Use of lightweight radioisotope power generators could enable missions to deep space far from the Sun. Some of these were studied in previous NIAC studies (Nosanov et al., 2013).• If a close solar flyby is chosen for the mission, one would have to rely on the advanced materials needed to protect spacecraft with sol... | |
space_sciences/14576_6.txt | ICHAROSIi, D. SAf..ITLEBEN .22, f\1. SEIFFER'!' 0, '[ C S ' S T S 10 0 T 1.3 K L T 1'1 R n · 0.1 B n · I.' 1\, , HEPHERD , . . TAOGS , ' .. \JIMA 2 . . HOMPSON 2 . "" ILLIAMSON | |
space_sciences/19902_329.txt | lains district of Australia (Bristow et al., in prep.) support this idea.
The geochemical conditions required by Fe-saponite and magnetite authigenesis at Yellowknife Bay coupled with absence of definitive carbonate detections there place thermodynamic constraints on the levels of carbon dioxide in martian surficial e... | |
space_sciences/07979_133.txt | e fact that are subsequently observed. This appendix describes the first of such trial forecasts and comparisons.
Based on data from past events, when giant sunspot groups appear it is seen that the largest solar flares (X9.0 and larger)
(A) are most likely to start when these sunspot groups rotate into a region wher... | |
space_sciences/18291_77.txt | e, on due to the edge-onsource geometry which could reduce the X-ray flux reaching us.
We thank all members of the Suzaku hardware and software teams and the ScienceWorking Group. M.S., K.M. and T.E. are supported by the Japan Society for the Promotionof Science (JSPS) Research Fellowship for Young Scientists, the Gran... | |
space_sciences/02588_122.txt | hange in ionization age behind the rim give some indicationof variations in density around the remnant. Taking the electron temperature from thermalmodels, combined with the results of radio and X-ray expansion studies, the electron to meantemperature ratios behind the shock are _< 0.1 -0.2, indicating a modest amount ... | |
space_sciences/16218_76.txt | 3) and (22) have been verified experimentally with our seed laser described in [13]. Figure 3 (left) shows the standard deviation of the absolute frequency of the slave laser and frequency offset between the slave and master lasers measured within a gating time from 1 s to 1 ms. The absolute frequency noise was measure... | |
space_sciences/18203_69.txt | g cm−2s−1, as reported inNowak et al. (2012). All errors are at the 90% confidence level. strength B, and the temperature of the electrons Te. Assuming a thermal distribution of electrons,the spectrum due to synchrotron emission is calculated, which is then up-scattered by the samepopulation of electrons. Double up-sca... | |
space_sciences/24291_171.txt | i: 10.1080/03091928408210078Berger, M. A., & Field, G. B. 1984, JFM, 147,133, doi: 10.1017/S0022112084002019Biskamp, D. 1993, NonlinearMagnetohydrodynamics (New York: CambridgeUniv. Press)Borovikov, D., Sokolov, I. V., Manchester, | |
space_sciences/09318_9.txt | cattering halos are created by the smallangle scattering of X-rays as they pass through dust grains. When an inconling X-ray interacts with the electrons in a grain large compared to the X-ray wavelengththe resulting Rayleigh scattering adds coherently in the forward direction leading to small-angle scattering; see van... | |
space_sciences/23596_75.txt | tive to estimate M˙loc,cr at the inner and outer scalesof the ADR. In the region of the disk where dust still exists, the smallest possible value ofM˙loc,cr is possible at the smallest possible r ' Rin ' r0.01. The disk at Rin is geometricallythick when M˙loc is comparable to | |
space_sciences/02576_115.txt | g should be correct for all pixels whose error is not dominated by theother noise component (background). We also note that this 0 I line has a complex profile, with two geocoronaland ,,ne nearby photosphericfeature (seeFigure 7). Nevertheless,wedecidedto keepthis line i_ our analysisasit addsimportant constraints on t... | |
space_sciences/03523_143.txt | s not an X-ray warm absorber, in agreement with the conclusion of Brotherton et al. (2002) based on FUSE observations of 0 VI and Lyp, and despite our earlier claim based on nonsimultaneous GHRS observations (CK99). The new STIS observations were obtained when the UV continuum and broad emission lines Auxes were low, a... | |
space_sciences/18290_25.txt | hrotronemitting electrons are produced where the jetheads hit the interstellar medium (ISM). Similarstructures have been found in other non-nuclearBHs: notably, the ring around Cyg X-1 (33), the“ears” of SS 433 (34), and the bubbles aroundseveral ULXs (35). We speculate that the LBAradio source arises from the eastern ... | |
space_sciences/07338_17.txt | tunately close to the J = 5 − 3 Oxygen lineat 834.1 GHz. As a result, it cannot be directly observed from the ground and the onlyastronomical detection was from ISO at too low spectral resolution to address the chemicalorigins questions (Cernicharo et al. 1997). However, the 13CH+ J = 1−0 transition is shiftedfar enoug... | |
space_sciences/14238_38.txt | s from neutral or singly ionized ions, with the exception of He II 304which is problematic. Young, O’Dwyer and Mason (2012) developed a method whereby theyused Fe VIII line in the Quiet Sun region to obtain the orbital variation and reference wavelength. We have also used this method and the Fe VIII λ186.6 line in the ... | |
space_sciences/16737_54.txt | f. our Figure 5 and Figure 13 from Pagaranet al. (2009). In particular, we note that the SSI changes remainconsistently positive at λ < 800 nm in both (OMI+GOME-2and SCIAMACHY) data sets, thus contrasting the SORCE/SIMand SORCE/SOLSTICE results. We understand that the transition from facular-dominated irradiance variat... | |
space_sciences/16438_192.txt | . Carlstrom, D. Dowell,L. Duband, S. Golwala, M. Halpern, M. Hasslefield, K. Irwin, W. Jones, J. Kaufman, B. Keating,C.-L. Kuo, A. Lange, T. Matsumura, B. Netterfield, C. Pryke, J. Ruhl, C. Sheehy, and R | |
space_sciences/02425_3.txt | y and Solar Physics, NASA/Goddard Space Flight Center,Greenbelt, Maryland 20771. In the past yea1, we have focussed on studying individual clusters foundin this sample with Chandra, as well as using Chandra to measure theluminosity-temperature relation for a sample of distant clusters identifiedthrough the ROSAF study... | |
space_sciences/06874_87.txt | s-section gpert in the TL and Tpert = L/Zfp = gPertnL. Even though the specific mechanism providing this viscosity needs to be understood, this time scale tdif apparently “controls)’ the diffusion supply of the matter into the innermost region of the accretion disk (TL). | |
space_sciences/13745_11.txt | a decade), particularly as the majority of truly necessary development and design programs are already well underway using ISS. The justifications include (1) taking advantage of the experience gained with the ISS development program before it is lost; (2) learning and applying early lessons via actual space operations... | |
space_sciences/18035_71.txt | ekal, R. L. Kessel, D. G. Sibeck, and A. Ukhorskiy (2012), Science objectives and rationale for the Radiation BeltStorm Probes mission, Space Sci. Rev., doi:10.1007/s11214-012-9908-y.Morley, S. K., M. G. Henderson, G. D. Reeves, R. H. W. Friedel, and D. N | |
space_sciences/15869_184.txt | , Eberhardt, P., Krankowsky, D., & Hodges, R. R. 1993, A&A, 277,677Morbidelli, A., Levison, H. F., & Gomes, R. 2008, The Dynamical Structure ofthe Kuiper Belt and Its Primordial Origin, eds. M. A. Barucci, H. Boehnhardt,D. P. Cruikshank, A. Morbidelli | |
space_sciences/13776_1.txt | Sky Event Reporting Metadata (VOEvent)Version 2.0
IVOA Recommendation 27 June 2011
This version: http://www.ivoa.net/Documents/VOEvent/20110711Latest version: http://www.ivoa.net/Documents/VOEvent/Previous version: http://www.ivoa.net/Documents/REC/VOE/VOEvent-20061101.html | |
space_sciences/09390_12.txt | o enable such goals through in-space servicing, beginning as soon as about the middle of the next decade. The ability to service spacecraft will increase science value and lower mission risk for an entire class of ambitious missions. Moreover, given the rapid advance of technology, especially in detectors, computing, a... | |
space_sciences/16198_45.txt | c energy in a turbulent plasma byscattering from colliding regions of magnetizedplasma.
In some bursts, additional thermal and nonthermal components are also seen in the prompt emission spectra, revealing more complexity in thoseGRBs. Fermi observations of unusually energeticGRBs and follow-up observations at longer w... | |
space_sciences/23956_65.txt | s.
2.3.2 High-resolution spectroscopy with the fiber-fed extendedrange optical spectrograph
TOI-257 was observed with the fiber-fed extended range opticalspectrograph (FEROS) instrument (R = 48 000, Kaufer et al. 1999)
on the MPG 2.2 m telescope at La Silla Observatory between2018 December 15 and 2019 January 22 | |
space_sciences/15223_51.txt | 2009.Chang, J., Adams, J.H., Ahn, H.S., et al. An excess of cosmic ray electronsat energies of 300–800 GeV. Nature 456, 362–365, 2008.Cortina, J., 2011 for the MAGIC Collaboration, Highlights of theMAGIC Telescopes, arXiv:1110.4747.
Dogiel, V.A., Fradkin, M.I., Kurnosova, | |
space_sciences/02328_68.txt | 1.Boogert, A.C.A.Blake, G.A. & A.G.G.M. Tielens 2002b, ApJ, in press.Bryden, G., Chert, X., Lin, D.N.C, Nelson, R.P., & Papaloizou 1999, ApJ, 514, 344.Charnely, S.B. 2000, in Astronomical and Biological Origins, ed. C.B. Cosmovici | |
space_sciences/12182_4.txt | , and could also have been important for initiating prebiotic chemistry on the early Earth [1]. Comets are comprised of molecular ices, that may be pristine interstellar remnants of Solar System formation, along with high-temperature crystalline silicate dust that is indicative of a more thermally varied history in the... | |
space_sciences/24770_379.txt | s(see Cluster S1 TI2 paper by Pevtsov et al. (2023)).
5.2. Interaction processes with large-scale field structures
Knowing the propagation direction and orientation of aCME event is key to a) interpret observational data and b)properly feed models. Changes in the initial propagationdirection have manifold reasons. Duri... | |
space_sciences/13940_124.txt | g to be the most important exosphedc supply process on the sunlit side of an asteroid. At the near Earth distances, IS is expected to be even more significant. The escape velocity of a Near Earth Object (NEO) is very low (i.e. 0.52 mls for a NEO of mass _1012 kg and of raelius -0.5 Ian), the particles released from the... | |
space_sciences/21042_18.txt | sult of this experience, the SDO ACS team has continued to investigate the dynamics of slosh. This continuing investigation and the flight experience have resulting in the following lessons learned: First, the settling burn, which was defined by the geyser slosh mode, needs to be a function of the settling time of seve... | |
space_sciences/16235_3.txt | n gyroscale is a topic that is being investigated extensivelynowadays, both theoretically and observationally. Although recent observations gave evidence of the dominanceof kinetic Alfven waves (KAWs) at sub-ion scales with ´ ω<ωci, other studies suggest that the KAW mode cannotcarry the turbulence cascade down to elec... | |
space_sciences/21022_56.txt | n in Fig. 5, derived from these models, shows the degree of variation in both
energy and intensity across many orders of magnitude. The electron flux (curve with open circles) is derived by the integration of differential intensity over the energy and solid angle. The energy flux (curve with open triangles) is obtaine... | |
space_sciences/09208_15.txt | s that will ultimately be used in the operational S&OC Flight Operations Subsystem (FOS).
1.3 Where We Are Going
The JWST launch readiness date is June 2013. By that date, the JWST Ground Segment will have been developed and tested, and operations personnel training will be completed. Ground Segment testing will incl... | |
space_sciences/07794_21.txt | ffort, with U.S. funding provided by the Department of Energy and NASA.
References
- The "Top -+ Down" approach will search LAT error boxes for X-ray couilterparts with nonthermal, hard spectra, then use the X-ray position to find corresponding optical and radio sources. An example of this method is the identificatio... | |
space_sciences/10744_64.txt | s will be provided by the Space Telescope Science Institute in Baltimore, Md. Science Goals and Objectives
The Kepler Mission is a photometric space mission that will continuously observe a single 100-squaredegree field of view (FOV) of the sky of more than 100,000 stars in the Cygnus-Lyra region for four ormore years | |
space_sciences/05467_238.txt | L.; Filippenko, A. V.; et a1 (including Holland, S. T.); 2003: “Cosmological Results From High-z Supernovae”; ApJ; 594; 1. Magnetotail Current Sheet As Derived From Geotail And Polar Data”; J. Geophys. Res.; v. 109; A03218; doi:10.1029/2003JAO10062. Tsyganenko, N. A | |
space_sciences/25117_93.txt | ntile.(h) σ ≡ standard deviation.(i) σ2 ≡ variance.2. Fundamental parameters(a) ε o ≡ permittivity of free space.(b) μo ≡ permeability of free space.(c) c ≡ speed of light in vacuum (in kilometers persecond) = e m - o o 1 2 ( ) .(d) kB ≡ the Boltzmann constant (in joules per kelvin).(e) e � | |
space_sciences/00776_156.txt | 1999) Directional Control ofthe Subsurface Explorer Report in Support of the MartianSubsurface Explorer. A COSTING STRATEGY FOR MANUFACTURING IN ORBITUSING EXTRATERRESTRIAL RESOURCES
Ganesh, B., Matos, C.A., Coker, A., Hausaman, J., Komerath, N.M.School of Aerospace EngineeringGeorgia Institute of Technology | |
space_sciences/12929_134.txt | " of simpler entities that are adapted to living off the landand one another in a pyramid of complexity. Without this we will be forever bound to the network ofthat sort that already exists on Earth: a pyramid that includes Earth's networked biosphere andcivilization's networked industry. To release ourselves from the ... | |
space_sciences/17496_41.txt | e code andhave been recently updated (Belczynski et al. 2010).2. The time evolution of orbital properties. StarTrack numerically integrates a set of four differential equations describing the evolution of orbital separation, eccentricity, andcomponent spins, taking into account tidal interactions,magnetic braking, grav... | |
space_sciences/11175_85.txt | s a reasonable representation if the time interval between nanoflares isshort compared to a cooling time. When such conditions apply, the conductive and theradiation terms of the energy balance equation are comparable in magnitude to each otherand to the mean heating rate, (Q) (Vesecky et al. 1979):
Here, KO is the coe... | |
space_sciences/24410_115.txt | 2017) YSO model, and the fitted mass divided by fittedenvelope accretion rate. The photospheric age is fairly wellconstrained, to ∼105 yr for the more massive YSOs >5 Me,increasing to ∼106 yr for the lower-mass Må ; 2Me YSOs | |
space_sciences/14677_78.txt | sults are shown in Figure 8 for FRMS (FMea gives consistent results). Note the significant increase in the 4- 20 keV pulsed flux in the 2006 June observation following the cluster of bursts. This incre""e is not present in 2 -4 ke V. Also note the significant rise and subsequent decay of the pulsed flux following the l... | |
space_sciences/18017_21.txt | eprojected, registered vector magnetic-field data. The cadence of thedata is 720 seconds. The window size used in DAVE4VM is 19 pixels, which is determinedby examining the slope, Pearson linear correlation coefficient, and Spearman rank order between h ·(vzBh −vhBz) and δBz/δt, where vz and vh are vertical and horizont... | |
space_sciences/20876_54.txt | s and placing someclose pairs in the same voxel. Table 1 summarizes statistics for three grid sizes. Columns 5-8, giving the maximumnumber of galaxies in any one voxel and the fractions with 0, 1, and 2 or more galaxies, are useful in assessing theinformation loss in this binning. Ideally the fraction with more than on... | |
space_sciences/16192_137.txt | 7 dex) are associated to these techniques (Verstergaard2004). Shen et al. (2011) estimated the BH mass based onthe Hβ broad line and MgII line in the SDSS DR7 spectrumas log(MBH /M⊙) = 7.99 ± 0.12 and log(MBH/M⊙) = 7.79± 0.16, respectively | |
space_sciences/12095_42.txt | y X-rays that penetrate more deeplyinto the layer are reflected by the deeper, more closely spaced layers. The originalconcept for graded multilayers introduced a power law layer variation with distance.Yamashita et al. [23] introduced the "supermirror" concept wherein the continuousgradation is replaced by a series of... | |
space_sciences/26262_57.txt | n 5.1) and adding2 years (see below) to give the estimated PhD date. As an example, the present author’sfirst FAR article was published in July 1997, giving a career start date of January 1997(Section 5.1). The estimated PhD date is then January 1999 (the actual award date wasOctober 1998). The early career designation... | |
space_sciences/21621_81.txt | 1.[20] A. Stroeer and A. Vecchio, Class. Quantum Grav. 23,S809 (2006), arXiv:astro-ph/0605227.[21] T. Kupfer, V. Korol, S. Shah, G. Nelemans, T. R. Marsh,G. Ramsay, P. J. Groot, D. T. H. Steeghs, and E. M.Rossi, ArX | |
space_sciences/18404_8.txt | k the worst case scenario solar particle event and estimate the total dose delivered to the part from that event. However, these worst case events occur infrequently and are more common during periods when the sun is undergoing intense activity. Additionally, the sun has recently entered a period of diminished activity... | |
space_sciences/23862_480.txt | r, K.-H., Richter, I., Carr, C., Kudela, K., Shi, J. K., Zhao,H., Motschmann, U., and Lebreton, J.-P. (2006), Magnetic field investigation of the Venusplasma environment: Expected new results from Venus Express, Planetary and Space Science, 54, 1336–1343, doi:10.1016/j.pss.2006.04.018.Z | |
space_sciences/14009_140.txt | . 2005, PhD thesis, The University of Toledo, http://astrobiology.gsfc.nasa.gov/Bonev_thesis.pdfBonev, B. P., Mumma, M. J., DiSanti, M. A., et al. 2006, ApJ, 653, 774Bonev, B. P., Mumma, M. J., Gibb, E. L., et al. 2009, ApJ, 699, 156 | |
space_sciences/17164_32.txt | e-layered flexible circuity consisting of a Kapton base with aluminum traces at 100 um pitch.This flex is wire-bonded on the other end to a printed circuit board (PCB) which holds the multiplexing andreadout chips. In total there are nine of these boards, one for each semihex wafer and two for each hex, alloperated at ... | |
space_sciences/24018_121.txt | tains links to the TIC, allSectors the EB is observed in, and all Origins. In addition,it provides the data source45 (FFI for full-frame images, TPFfor target pixel files, and LCF for light-curve files). It also givesthe refined ephemerides (see Section 3.5) and morphologycoefficient (see Section 3.6) | |
space_sciences/12043_14.txt | e found toresult in electron energization via the drift-resonantinteraction.
Degeling et al. [2007] considered the effect of realisticscenario of asymmetric azimuthal distribution ofcompressional mode ULF waves on electronacceleration and demonstrated that the poloidal modewave is more efficient in electron energizatio... | |
space_sciences/23911_60.txt | 100°, both of which areclose to the photometric major axis of ∼84°. The velocitycentroids are blueshifted in the west and redshifted in the east,and based on the above photometric major axis and inclinationof the host galaxy disk (55°; Schmitt & Kinney 2000), thedeprojected velocity amplitude of the galaxy’s rotation ... | |
space_sciences/26034_329.txt | d Solar Maximum. The flux data are from Cosmic Radiation Extended Warding using the Halbach Torus
the Badhwar-O'Neill 2014 model [36]. The same weighting scheme was used to determine thedoses corresponding to the CREW HaT active magnetic shielding turned on by simplyconvolving the dose quantities with the transmission ... | |
space_sciences/17882_103.txt | oughspherically symmetric shells with a maximal radius of the simulation, ≈ 1622 AU. The radiation is injected in the first shell andthen travels outward until it is either absorbed or exits the last shell.For the results shown we used ∼ 3 × 104 shells. We note that timestepping is arbitrary because of the equilibrium ... | |
space_sciences/13759_85.txt | .3) is the model dose to the data OWl' the SnrelllE'llt. at ~ 50 oYerestimatC's (A ~ 100 -lGO snn'lllPnts. in \Ve take a further step and consider mixtures of amorphous silicates and carbonaceous materials. Vie ran a Bayesian analysis and find that the actual best composition corresponds to pure carbon. Qualitatively, ... | |
space_sciences/24410_192.txt | m withinthe Galactic molecular cloud Perseus A observed in 13COby Shetty et al. (2012; median R of 0.07 pc);5. clumps in the Magellanic Bridge studied by Kalari et al.(2020) in CO (1–0; mean R of 1.1 pc);6. clumps in the Magellanic Bridge studied in 12CO (2–1)by Valdivia-Mena et al. ( | |
space_sciences/14626_329.txt | , S., Casandjian, J. M., Cavazzuti,E., Cecchi, C., C¸ elik, O., Charles, E., Chekhtman, A., Cheung, C. C., ¨Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Colafrancesco, S.,Cominsky, L. R., Conrad, J., Costamante, L., Davis, D | |
space_sciences/20104_92.txt | riginal RaySure calibration factors for derivingdose equivalent rate from the count rate spectrum are fairly robust. However, analysis of the RaySure dataduring the RaD-X ground tests and flight measurements, along with previous measurements in the aircraftradiation environment, has shown a fairly large spread in measu... | |
space_sciences/06243_170.txt | ” NASA Technical Publication 1998-206895, page 53, 1998.
23. IBID, page 53. 24. John A. Zoutendyk, “The Space Calibration of Standard Solar Cells Using High Altitude Balloon Flights,” Proceedings of the Fourth Photovoltaic Specialists Conference, page C-4-1, 1964. | |
space_sciences/25803_127.txt | c retrievals for thespot scenario, this interpretation may have a slight edgeover a water-rich atmosphere. However, a true determination of the nature of GJ 486b remains on the horizon,with wider wavelength observations holding the key tothis world’s location along the cosmic shoreline.
ACKNOWLEDGMENTS
. We thank the a... | |
space_sciences/25803_164.txt | Kempton, E. M. R., Bean, J. L., Louie, D. R., et al. 2018,PASP, 130, 114401, doi: 10.1088/1538-3873/aadf6fKirk, J., L´opez-Morales, M., Wheatley, P. J., et al. 2019,AJ, 158, 144, doi: 10.3847/ | |
space_sciences/16205_42.txt | 22 and 2events on 2009 January 30).
2.3. Data Reduction
We extracted time-integrated spectra for our 42 simultaneously detected bursts. In Figure 1, we present the burst detectedat 02:34:28.194 on 2009 January 22 as an illustrative example ofspectral integration ranges. We describe below the procedureswe followed to g... | |
space_sciences/02567_34.txt | n three dimensions
• Magnetic connectivity to Sun
• Incorporate composition into model APPENDIX E
"Modeling of Transequatorial Loops with MH4D"R. Lionello and D. SchnackPresented at the Spring AGU MeetingBoston, MA, May 29-June 2, 2001 (11)euoJoo eql lo lepolN aleos e6Je-I pue uo!lnlosaEI q6!H | |
space_sciences/16879_226.txt | e softX-rays from the WWC region can ionize the He+ only during thesetimes. This is almost exactly the same range of spectroscopic phasesthat strong He II λ4686 emission is detected. Furthermore, this isroughly the same range of phases that the post-shock ηB wind is inthe radiative-cooling regime. During this time, the... | |
space_sciences/24169_131.txt | ucts the followingcontributions to the conservative SSF,
4. Evaluating the dissipative averages
Next, the program uses the secular evolution module in Appendix B 7 to construct the orbit averages⟨J ⟩˙ diss = ⟨⟨J ⟩⟩ ˙ diss0 + ⟨δJ ⟩˙ diss defined in (88) and (89) | |
space_sciences/25799_224.txt | iety 1958; 80(7):1580-8. Eigenbrode JL. Fossil lipids for life-detection: a case study from the early Earth record. Strategies of Life Detection 2008:161-85; doi: 10.1007/978-0-387-77516-6_12 | |
space_sciences/14049_62.txt | e need for measured UV spectra of the host star when modeling the atmospheric properties of an exoplanet. The paucity of UV observations of low-mass exoplanetary host stars may bias our interpretation of potential biomarkers when direct spectroscopy of extrasolar terrestrial planets becomes feasible, possibly in the co... | |
space_sciences/22076_63.txt | nale", Proceedings of SPIE Vol. 9905, 990505 (2016).[10] Kendrick, S, Woodruff, R., et al., “UV spectroscopy with the CETUS Ultraviolet multi-object spectrometer (MOS),” AAS 140.08, (January 9, 2018).[11] MSA: jwst.nasa.gov/microshutters.html[12] Woodruff, R., et al., “Optical | |
space_sciences/16866_222.txt | o, Y., Giavalisco, M., Ferguson, H. C., Cassata, P., & Koekemoer, A. M.2012, ApJ, 757, 120Heckman, T. M., Norman, C. A., Strickland, D. K., & Sembach, K. R. 2002, ApJ,577, 691Hibbard, J. E., Guhathakurta, P | |
space_sciences/22481_44.txt | ULF wave generation in the magnetosphere, such asenhanced speeds and/or densities, are absent. During this period we only see a change in the heliosphericcurrent sheet sector, which is accompanied by substorm activity (see AE index in Figure 2e and Pi2 activityin Figure S2 in the supporting information) and the presenc... | |
space_sciences/07302_38.txt | y the lowest order asymptotic solutionφk,o(x,Ω′,E″) as
where φj(x,Ω,E) is found as an integral over the neighborhood of rays centered on Ω using the lowest orderasymptotic solution φk,o(x,Ω′,E″) along an adjacent ray directed along Ω′ | |
space_sciences/14626_279.txt | n from interplanetary dust (the zodiacal light) dominates the brightness of the sky;
6. Models of the EBL, employing various methods for determining theevolution of the galaxies’ spectral energy density with redshift seemto agree on the intensity and spectral shape of the UV to near-IRcomponent of the EBL. However, the... | |
space_sciences/22286_215.txt | X-ray source toionize the wind above its mean ionization state throughoutapproximately half the wind volume. The lines accessible toChandra HETG observations correspond to an ionization state that is significantly higher than the mean ionization state thewind would have in the absence of X-ray ionization. Weobserve H- ... | |
space_sciences/18087_55.txt | l. (2010) argue that the GeV emissionfrom 1FGL J1640.8−4634 originates from the PWN, the Fermisource is spatially unresolved and marginally consistent withthe position of the pulsar. Therefore, we searched the FermiLAT data at the position of PSR J1640−4631 for a pulsedsignal. The X-ray timing parameters and their erro... | |
space_sciences/09482_86.txt | s protons and alpha particles in solar particle events, can cause both transient and permanent SEE.
Figures 10 and 11 illustrate the periodic yet statistical nature of solar particle events. They are plots of the daily solar proton fluences measured by the Interplanetary Monitoring Platform-8 (IMP-8) and Geostationary... | |
space_sciences/22562_164.txt | 3.[71] Yashar D. Hezaveh, Neal Dalal, Daniel P. Marrone, Yao-Yuan Mao, Warren Morningstar, Di Wen,et al. Detection of Lensing Substructure Using ALMA Observations of the Dusty Galaxy SDP.81.ApJ, 823:37, May 2016. arXiv:1601.01388, doi:10.3847/0004-637X/823/1/37 | |
space_sciences/17543_55.txt | s within this energyrange. Thus, more emphasis was placed on minimizing the uncertaintyin those bins.
Figures 4−7 show the comparison of the average of the integrateddifferential flux for H, He, O, and Fe for each data set with BON11 andBON14 models. In these figures, we separated the data into two energyregions to sim... |
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