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space_sciences/02678_107.txt | h) observation (Imanishi, Koyama, &Tsuboi 2001). This weakens the possibility thatthe ASCA X-Ray flare period is physically relatedto the protostellar rotation rate. Hereafter we assume that the rotation axis of YLW 15 is inclined57 ° from our line of sight, the most likely inclination angle for a random distribution. ... | |
space_sciences/05501_13.txt | MlOl ULX-1 throughout the ongoing MlOl 1 Ms exposure with Chandm. During the 2004 July 5-11 observations, it entered a brief but less extreme high state with a peak Lx - 4.3 x lo3* ergs s-l, but quickly returned to its quiescent level. The details of the X-ray observations will be reported elsewhere.
Using HST ACS dat... | |
space_sciences/24649_140.txt | 2014 Conference and Exposition, San Diego, California, 4-7 August 2014
David L. Akin and Mary L. Bowden, “Design of an Affordable Near-Term Variable Gravity Research Facility inCislunar Space” AIAA 2014-4197, AIAA Space 2014 Conference and Exposition, San Diego, California, 4-7 August2014 | |
space_sciences/18359_8.txt | V. B. Braginsky36, M. Branchesi48,49, J. E. Brau50, T. Briant51, D. O. Bridges6,A. Brillet41, M. Brinkmann9, V. Brisson37, A. F. Brooks1, D. A. Brown14, D. D. Brown23, F. Brückner23,S. Buchman19, A. Buikema11, T. Bulik | |
space_sciences/20204_13.txt | ,4]. We tentatively identified adenine in the supernatant portion for the entire temperature series. Previously, Borquez et al. reportedadenine yields from the (unhydrolyzed) supernatant of 0.1 M ammonium cyanide as a function of temperature (-78, -20, 60, 80, and 100 °C). They showed that adenine yields were only slig... | |
space_sciences/16738_17.txt | Mehner et al. 2010; Teodoro et al. 2012).
In 2003, Chandra and XMM-Newton performed four pointed observations during theshallow minimum, but both acquired only one observation each during the deep minimum.Since the X-ray flux dropped below the RXTE sky background during the minimum, wecould not measure with RXTE the fl... | |
space_sciences/01639_167.txt | t datasystem, readout electronics and detectors. The system also includes latching relays so that
discrete commands can be used to power on / off the computercontrol systems, and power controllers for software commandingthe readout electronics and detector high voltage power, Inaddition, all critical voltages and relay... | |
space_sciences/15227_34.txt | 5,16, M. MacInnis30,D. M. Macleod13, M. Mageswaran6, K. Mailand6, E. Majorana23, I. Maksimovic101, V. Malvezzi68, N. Man49,I. Mandel25, V. Mandic76, M. Mantovani20, F. Marchesoni44,102, F. Marion9, S. Marka ´ 32, | |
space_sciences/19118_32.txt | r activity (IVA) scenarios (Wilson 1997).
B. Current NASA Permissible Exposure Limits
Current permissible exposure limits (PELs) for short-term and career astronaut exposures to space radiation have been approved by the NASA Chief Health and Medical Officer as documented in NASA Standard 3001, Vol. 1, Revision A, 2014.... | |
space_sciences/16849_139.txt | n the internal shocks. To accommodate IceCube non-detection, revisions to the neutrino flux from
internal shocks have also been proposed [184, 185]. Newcalculations in the models alternate to internal shocksare being done as well, e.g. [186]. Data from the fullIceCube detector will either constrain the neutrino product... | |
space_sciences/24944_15.txt | nHeliophysics without a constant, reliable observer of the sourcesof atmospheric dynamics and space weather. The purpose ofthe present paper is to present the argument, submitted asa white paper to the Decadal Survey for Solar and SpacePhysics (Heliophysics) 2024–2033 (Ugarte-Urra et al., 2022),that Heliophysics as a f... | |
space_sciences/13431_160.txt | d mapping algorithm which uses B-splines to model atmospheric signal and to remove it from the data. The method has been used to make high precision ( < -40 dB) beam maps, with solid angles in the 148 GHz, 218 GHz, and 277 GHz bands of(218.2 ±4)nsr, (118.2 ± 3)nsr, and (104.2 ± 6)nsr, respectively. The beam profiles an... | |
space_sciences/21131_88.txt | 8, 127Buenzli, E., Apai, D., Morley, C. V., et al. 2012, The AstrophysicalJournal Letters, 760, L31Burgasser, A. J., Cruz, K. L., Cushing, M., et al. 2010, ApJ, 710,1142Burgasser, A. J., Marley, M. S., Ackerman, A. S., et al | |
space_sciences/07463_123.txt | (harder) during the plateau stage, and steeper (softer) during the exponential rise. Taken together with the decoupling between the X-ray and the radio flux, it seems likely that the radio emission here has a different physical origin from that during the plateau. The plateau seems much like the standard LHS, in the ra... | |
space_sciences/01840_67.txt |
The individual quadrants show significant differences in the spatial extent of the emissionand shape of the profiles. This is consistent with a sun-comet angle/orbital phase dependence inthe acceleration (Figure 2a,b). Moving radially outward in the sunward and anti-tail (orbitleading) quadrants, the OH surface bright... | |
space_sciences/13408_33.txt | d to this work.
References
Busche, J. R. & Hillier, D. 1. 2005, Al, 129,454 Corcoran, M. F. 2011, Bulletin de la Societe Royale des Sciences de Liege, 80, 578 Damineli, A. et al. 2008a, MNRAS, 384,1649 Damineli, A. et al. 2008b, | |
space_sciences/12066_67.txt | s, and then the hardness ratio declines along with the X-ray fluxto the start of the minimum. As noted above, this decline in hardness is dominated bythe increasing relative contribution of the soft cosmic X-ray background to the observedrl Car spectrum in the PCU2 field of view as the hard flux from the colliding wind... | |
space_sciences/18214_74.txt | s and radiators were simulated using a Geant4 (http://geant4.web.cern.ch/geant4/)Monte Carlo, which uses the measured optical properties ofthe reflector, PMT quantum efficiency, absorption length, andRayleigh scattering length in the Cherenkov radiator. Thesesimulations were used to optimize the performance of the ligh... | |
space_sciences/00776_112.txt | . This crushedzone was determined to stretch over a distance of about 3mm around the borehole. The next layer was untouchedartificial permafrost. It could not be determined if thecrushed zone around the borehote was also thawed at anytime.
The tip of the smcxxh penetrator did not show any signsof dulling, even after th... | |
space_sciences/16384_19.txt | Jllxy forilIHlion. In a major gahL'l::y Illerl.\cr e\'cut, the Sl\ lOHs hosted ill two Imgt: tllCrgjllg gala:des dynHlJlicaliy interact a ... thc pur('1lL galaxies coale.'$C(' and form a final bulge. S~ID H lIlerging call be ('ons.id('f('(1 in three st. | |
space_sciences/06825_28.txt | w some results from the RQMD event generator as it is exercised within the FLUKA code. These fluence plots (number of particles cm-2) were all prepared to aid in the planning for proposed future measurements at the Alternating Gradient Synchrotron (AGS) at the Brookhaven National Laboratory on Long Island | |
space_sciences/16152_51.txt | tional to 1/τ . For present purposes, however,the main point is an empirical one. Persistence in NIRSpec’s flight SCAs decays according to a 1/tpower law and there is no evidence of any long timeconstant persistent tail that would complicateeither flight operations or calibration. 2.1.10. Performance Summary
Overall, w... | |
space_sciences/07956_71.txt | Xspec f akeit command using the detector and the ancillary response files created for each source region. Thus, the effect of the spectral evolution could be consistent with the expectation of the curvature effect for GRB 060211A and GRB 060202. However, we do not see a strong spectral evolution for other GRBs except f... | |
space_sciences/21965_52.txt | tsurprising in light of the larger aperture and optical design which is closer to being on axis.
We chose the SM to carry the compensation for these exercises, since for the moment we have only a telescopemodel available to work with. We do not mean to suggest such an option for the actual system design, sincetampering... | |
space_sciences/23688_72.txt | t) located at 2C , D7 ≅ (−150, 0) /. The bleed-over counts are recorded in He+ TOF bins corresponding to solar wind proton energies. Since these counts are registered as He+ ions, when converted to He+ velocity they appear with speeds lower than the bulk proton speed by the factor [02302= 2. In the right panel, the maj... | |
space_sciences/26220_54.txt | e are movingfrom an Eulerian to a co-rotating Lagrangian description of the rings. Thus, the Lagrangian derivative used in SCL,𝐷∕𝐷𝑡 = 𝜕∕𝜕𝑡 + Ω𝜕∕𝜕Θ, becomes the time derivative 𝜕∕𝜕𝑡 in the co-rotating frame. | |
space_sciences/09540_37.txt | t of cross-field diffusion such that q = 1 corresponds to the isotropic Bohm diffusion limit. It can be related to parallel ( 611 = X v/3 ) and perpendicular ( KL ) spatial diffusion coefficients through the relation KL/K~~ = 1/(1+ q2) (see Forman, Jokipii & Owens, 1974, Ellison et al., 1995, or Jokipii, 1987) | |
space_sciences/05108_12.txt |
We compared our data with Starburst99 evolutionary models to estimate the ages and masses of the knots. Most of the ultraviolet knots are younger than 10 - 20 million years (Myrs), not surprising since the massive young stars which produce most of the ultraviolet emission only live about 10 Myrs. The sizes of the knot... | |
space_sciences/12442_61.txt | netic indices. The middle and right panels of Figure 7 show that this is indeed the case. The net currents intensify as the Dst* index becomes more negative (as the ring current indentifies) and the Kp index increases (as the global level of geomagnetic activity is enhanced). These correlations indicate that the net cu... | |
space_sciences/16586_123.txt | l., 2000] and the higher anisotropy ofsurfaces in this angular range. The success of MARS-ReCOis, by contrast, less dependent on the properties of the surface materials. In particular, MARS-ReCO performs slightlyworse when dealing with bland materials such as Soil-2,which may be too dark and too isotropic to be accurat... | |
space_sciences/26322_43.txt | litude inthat case given the exponential drop in density).
3.5. Cross-field drift speeds
As mentioned earlier, we observe two distinct types of crossfield movements during these events: (i) movement of a threadlike structure that separates from the main loop; and (ii) movement of the separated thread toward its new loc... | |
space_sciences/17049_170.txt | i, N.E., Sahal-Bréchot, S., Lemaire, P.: Linear polarization of the O VI λ 1031.92coronal line. II. Constraints on the magnetic field and the solar wind velocity field vectorsin the coronal polar holes. Astron. Astrophys. 396, 1019–1028 (2002)16. Casini, R., Judge, P.G.: Spectral lines for polarization measurements of ... | |
space_sciences/01818_10.txt | nication among groups who aredeveloping informal astronomy education projects, by providing a communitybulletin board. "Best Practices" posts articles and resources aimed at improvingthe quality of future informal science education programs and projects.
Plans for maintaining and disseminating. The site is periodically... | |
space_sciences/01764_69.txt | l models," J. Geophys. Res., 106,15,869 (2001).
Riley, P., J. A. Linker, Z. Mikic, and R. Lionello, "MHD modeling of the solar coronaand heliosphere: Comparison with observations," in Space Weather (P. Song, G.Siscoe, and H. Singer, eds.), American Geophysical Union, GeophysicalMonograph 125, 159 (2001). | |
space_sciences/25583_48.txt | L of RLT with 1% betamercaptoethanol (Fisher Scientific). For all samples, the tissue wasfirst homogenized using GenoGrinder (SPEX SamplePrep 2010;GenoGrinder) and metal beads at 1,700 rpm for 2 min, followedby homogenization using QIAshredder columns (Qiagen). All theRNA was extracted using a RNeasy Plant Mini kit (Qi... | |
space_sciences/22632_163.txt | tudes only during low-inclination flybys where thehorizon circle encompasses all latitudes. On high-inclinationflybys, on the other hand, the horizon circle is near-equatorial,limiting the latitudinal information that can be obtained.High-inclination flybys do provide the opportunity for surfacetemperature mapping of p... | |
space_sciences/13166_32.txt | n the cosmic X-ray background within the PCA field-of-view in the direction of V\V Hyi. Therefore, while we can be confident that VW Hyi was fainter in superoutburst by 0.42±0.09 c S-l PCU-1 (approximately 5 x 10-12 erg cm-2s-1) than in quiescence, we cannot determine the actual flux level or the spectral shape during ... | |
space_sciences/22668_6.txt | d of 7 km/s and addresses the complexities associated with that addition.
1 INTRODUCTION
The DebriSat hypervelocity impact experiment, performed at the Arnold Engineering Development Center, is intended to update the catastrophic break-up models for modern satellites [2]. To this end, the DebriSat was built with many... | |
space_sciences/05802_64.txt | r in the form of power laws. These include, in particular, the (k,w), i.e. mode number and frequency, spectra of the correlations of the various fluctuations of the dynamic field variables.
Such power law behavior has been detected in the probability distributions of solar flare intensities (Lu, 1999, in the AE burst ... | |
space_sciences/24324_69.txt | y0 = 0.0, sx = 0.10, and sy = 0.15; the amplitude Vd controls the nonlinearity. The density andmagnetic field perturbations are computed by zero-order interpolation from the interior of the computational domain,whereas the transverse velocity components are set to zero at the boundary. This results in periodic perturba... | |
space_sciences/03778_42.txt | tabilizability, detectability, and standard rank conditions on the generalized plant are assumed.
To avoid the problem of overparametrization, a canonical form description for the controller can be used. It was shown in Ref. 20 that if either a controller or observer canonical form is imposed on the compensator struct... | |
space_sciences/13750_133.txt | a quasi-static torus there will be an Xray induced evaporation of a dense infrared driven flow. Even without X-rays in the verylow density part the dust will decouple from the gas, breaking the one-fluid hydrodynamicsapproximation, and thus such dust even if survived will be quickly blown away. Summingup we believe tha... | |
space_sciences/16101_40.txt | f the galaxies with detected line emissionare UV-bright.
4.2. Oxygen Abundances
We next convert the measured [N ii]/Hα ratios into oxygenabundances. To demonstrate the spread in oxygen abundancebetween metallicity calibrations, we calculate the oxygen abundance in three different calibration systems: Maiolino et al.(20... | |
space_sciences/20816_59.txt | d the spacer heights be adjusted precisely and efficiently? (5) How are the mirror bonded accurately?
3.1 Precision of placement a single mirror segment in 4-point mountPermanently bonded
Needless to say, without additional assistance, friction between the spacers and the mirror will prevent the mirror from settling on... | |
space_sciences/07798_188.txt | h during a period of strong solar wind, so it was ambiguous which, if either, density dominates. The collection observations detailed above show that significant SWCX contamination can occur when observing through the lomier density flanks of the magnetosheath if the solar wind is particularly strong. Conversely, there... | |
space_sciences/12816_4.txt | rofisica, Postal 12245-970 - Sao Jose Campos, SP, Brazil
Preprint online version: April 2011
ABSTRACT
The existence of an isotropic component of the high-latitude radio sky has been recognized for nearly fifty years, but has typically been assumed to be Galactic in origin. We use receut radio observations to test wh... | |
space_sciences/14409_110.txt | c luminosity of the He II >.4686 emission line from eq. (2).
The results are shown in Fig. 6a, v!here the intrinsic line luminosities are shown - as well as the photon fluxes - for two events: 2003.5 and 2009.0. The line luminosity of the 2003.5 event was higher than that of 2009.0 (for a given phase): the peak values... | |
space_sciences/18298_90.txt | ) is the bolometric LC of SN Ic 2011bm presented by Valenti et al. (2012). SN 2011bm has a very high peakluminosity and (most importantly) a very slow evolution of thebolometric LC and a broad peak, which is difficult to explainwithout assuming a very high (> 30 M⊙) main-sequence massfor the progenitor. This is the kin... | |
space_sciences/14435_31.txt | 5 (1974).[2] Fishman, G. J., and Austin, R. W., “Large-area Multi-crystal NaI(Tl) Detectors for X-ray and Gamma-ray Astronomy”, Nucl. Inst. and Meth., v. 140, pp. 193-196 (1976).[3] Fishman, G. J.; Meegan, C. A.; Watts, Jr., J. W., and Derrickson, J. H., “New Limits | |
space_sciences/07238_6.txt | l libraries by including the near-UV and significant numbers of metal poor andsuper-solar abundance stars. Numerous calibration challenges have been encountered, some expected, some not; these arise from the use of the E1 aperture location,non-standard wavelength calibration, and, most significantly, the serious contam... | |
space_sciences/13062_187.txt | egies for Solar Dynamics Observatory. International Symposium on Space Flight Dynamics, 2007. 2
1Kuo-Chia (Alice) Liu, Thomas Kenney, Peiman Maghami, Pete Mule, Carl Blaurock, and William B Haile. Jitter Test Program and On-Orbit Mitigation Strategies for Solar Dynamics Observatory. International Symposium on Space Fli... | |
space_sciences/05462_33.txt | V, a 5-segment RSRB, upper stages, and modified SSME.
gppgOther considerations include transitioning from the SSP to the SDV program. Return to flight of the Shuttle, remaining Shuttle missions, and maintaining the capability to manufacture Shuttle components are the primary transition issues.
IV. Approach, Processes... | |
space_sciences/15106_69.txt | 4 keVand the other with a higher temperature of kTX = 1.7 keV.The lower-temperature component has an absorption-correctedflux and emission measure that are roughly four times higherthan the flux and emission measure associated with the highertemperature component, and its temperature is characteristicof plasma heated i... | |
space_sciences/12605_88.txt | ecreaseswith increasing turnover radius (not shown graphically, but the values are in the Table. In lineartheory, which is not strictly applicable here butyields useful approximations, the turnover radiusin the rotation curve sets the location of the ILRs,and they in turn determine where inflowing gaspiles up, which ul... | |
space_sciences/26327_724.txt | s Space Phys 100(A9):17059–17067. https://doi.org/10.1029/95JA01261Woodham LD, Wicks RT, Verscharen D, Owen CJ (2018) The role of proton cyclotron resonance as a dissipation mechanism in solar wind turbulence: a statistical study at ion-kinetic scales. Astrophys J 856(1):49.https://doi.org/10 | |
space_sciences/14058_11.txt | aI. 2010; Anderson et aI. 2010; Rossi et aI. 2010; Zanotti et aI. 2010). Emission might occur in the
late inSJl.iral from effects such as enhanced accretion, periodic Newtoman perturbations, or shearing of the disk due to gravitational waves (Kocsis & Loeb 2008; Schnitlman & Krolik .2008) | |
space_sciences/18102_71.txt | 0 with our absorption coefficientsplotted alongside those of Quirico and Schmitt (1997). Once more,the agreement is good.
4.3. Additional comments
Of the six hydrocarbon ice phases covered in this paper, onlyfive are likely to be important for astronomical objects. The formation of metastable ethylene ice required a mu... | |
space_sciences/02245_65.txt | bility of these objects, providing important information about thecharacteristic sizes of the gamma-ray emitting regions. Constraining models of AGN high-energy emissionrequires observations across all wavelengths, so once again use of the the combined capabilities of all theexperiments is essential.
Gamma-ray bursts (... | |
space_sciences/15282_40.txt | t six pumps since it proved closest to the conservative calculations and adding more did not greatly improve performance.
The 12 Cryogenic pumps provide a significant pumping capacity. They exceed the effective chamber pumping speed of the original eighteen diffusion pumps which was 270K Torr-l/m of air as compared to ... | |
space_sciences/26051_38.txt | ˆs:
For an arbitrary vector v, sˆ×v = S×v. Note that Equations 3 and 5 from the Beyerle(2009) model do not necessarily represent a set of simple rotations about the line-ofsight vector. They represent the phase correction as observed by the canonical exampleof crossed dipole receiver and transmitter antennas | |
space_sciences/13420_199.txt | R. SPIE, 2008. C. E. Tucker and P. A. R. Ade. Thermal filtering for cryogenic detector arrays. In Jonas Zmuidzinas, Holland. Stafford and vYilliam D. Duncan, Proc. SP1E, volume 62750U. Jnly 2006. D. \Voody, D. :\1. Bradford, R. 1\1. Dragovan, P. Goldsmith, J. | |
space_sciences/16858_109.txt | 3, respectively. This amounts to -0.3%, -0.7%, -0.2%, -0.3% deviations, respectively. This is not an exact comparison since the dipole of a vibrationally averaged structure is different from the vibrationally averaged dipole.
The vibrationally averaged structure for the GS, 1, 2, and 3 levels are r(SO)0 = 1.435172 Å,... | |
space_sciences/15116_155.txt | s small,usually increasing the measurement error by less than 5% compared with that calculated above.
We list in Table 2 the mass measurements within a 150 kpcradius using aperture densitometry for both statistics for eachstructure, in both cases using rmax = 1500 kpc and r2 =1150 kpc for ζc | |
space_sciences/19778_119.txt | g the moon’s extremely tenuous atmosphere and any surface material ejected into space. MASPEX
Compiled from NASA’s Galileo spacecraft data, this colorized surface image of Europa shows the blue-white terrains that indicate relatively pure water ice. Scientists are very interested in these features because they may off... | |
space_sciences/11524_56.txt | , see below). Now, the low energy pair production cross section isgiven as
with
and
A source term for positron production may be derivedin a manner similar to that described for productionof bremsstrahlung photons. See Eq. (12). For a photon differential flux spectrum ϕν(Eν, x), positron production may occur between en... | |
space_sciences/19302_73.txt | r," Appl. Phys. Lett., vol. 85, no. 11, pp. 2107-2109, 2004. (29] D. Schmidt, H.-M. Cho, J. Hubmayr, P. Lowell, M. Niemack, G. O'Neil, J. Ullom, K. Yoon, K. Irwin, W. Holzapfel et al., "Al-Mn transition edge sensors for Cosmic | |
space_sciences/10256_41.txt | . Bui, J. Hanley, N. H. Karam, and B. T. Cavicchi, “Ultra Triple Junction GaInP2/GaAs/Ge Solar Cells – Cell Design and Qualification Status,” presented at the 3rd World Conference on Solar Energy Conversion, Osaka, Japan, May 2003.
[6] J. A. Schwartz, “Progress in Triple Junction Solar Arrays,” presented at The Space ... | |
space_sciences/17378_100.txt | n in Figure 13. Single CTBs and redesigned FSPs were used to construct this shelter. The actual shelter would be created by deconstructing the CTBs into blankets, hanging these from rails on the top of racks, and securing the redesigned storage bags to these blankets. Ten FSPs were designed to fit into a single CTB. Th... | |
space_sciences/22367_235.txt | 8. arXiv:1812.03785.[147] Michael D. Niemack. Designs for a large-aperture telescope to map the CMB 10x faster.Appl. Opt., 55(7):1686, Mar 2016. arXiv:1511.04506, doi:10.1364/AO.55.001686.[148] J. E. Austermann, J. A. Beall, S. A. Bryan | |
space_sciences/10029_61.txt | a and thereby place limits on the amount of LIV as defined bythe δπp parameter.
Our results show that the amount of presently observed GZK suppression inthe UHECR data is consistent with the possible existence of a small amountof LIV. In order to quantify this, we determined the value of δπp that resultsin the smallest... | |
space_sciences/12584_14.txt | , the mass must be brought back to the early IRIS box, roughly a reduction by 3. This is achieved by (1) using a very broad band beam splitter (7 to - 1000 microns), CVD diamond [ref. 3] [Fig. 5], to replace the dual FTS with a single FTS [Fig. 6] (2) replacing thermoelectric FIR detectors with more sensitive (4 to 5x)... | |
space_sciences/16893_152.txt | n (SED), althoughthese measures are taken at different epochs.6 (see Fig.10). TheSED is not corrected for extinction because, from the hydrogencolumn density of X-ray fits, it is at most E(B−V)=0.1. Nevertheless, the unusual shape of the SED is apparent, with a pivotenergy at 1.2 μm, where at shorter wavelengths the sp... | |
space_sciences/01006_44.txt | ('('lls(50= 0.0I._Sr = 0.01)..\ fourth order smoothing l('rm was applied for stabilitv. Two-fluid versions ()fthis numerical approach have been used successflfllv for the inodeling of the solar wind ftowin coronal holes (Ofman & Davila I999).
The results of the calculations with the three-fluid code are shown in Figur... | |
space_sciences/04074_80.txt | e to the core’s spectrum (Slane, Helfand, & Murray 2002). Specifically, we adopt a hard upper limit on the foreground column density of NH < 2 x 1W2 cm-2, above all values of NH listed in Table 2. We assume that the neutron star’s radius as viewed by a distant observer is & = 12 km and that the distance to the source i... | |
space_sciences/01339_63.txt | o stars approach periastron (which should next occur one 20, 2003). In particular, we expect that the strength of the forbidden lines will weaken nearastron, as the density in the X-ray region increases and as the UV photospheric flux in the lineon intensifies. Additional HETGS observations as the stars approach perias... | |
space_sciences/18101_69.txt | g. 2c, d,g, and h had a thickness near 0.5 lm. Two spectral properties ofamorphous C2H2 ice are readily illustrated in the mid-IR spectra.First is the symmetric shape of the single-peaked m3 band, whichhas a maximum about 14 cm1 greater than that of the peak forthe crystalline ice. Second, the position of the peak of t... | |
space_sciences/05062_124.txt | rnova remnant containing evaporating clouds without extensively modifying and testing our supernova remnant simulation package. If we were to approximate the evaporating clouds spectrum using a non equilibrium, variable iron abundance spectrum and were to add it to the above non thermally conducting SNR simulation to y... | |
space_sciences/16889_5.txt | ,400 cm−3K, in agreement with previous studies, providing a validation test for the method.On the other hand, the model overestimates the emission from the huge cavities located in thethird quadrant. Using CaII absorption data, we show that the dust to CaII ratio is very small inthose regions, implying the presence of ... | |
space_sciences/13992_35.txt | 2/2422, significantly worse than the earlier best fit. High spin (a > 0.98) is again required and the inclination is higher (I ,... 39 deg),
2,l The N._DIan poweNoW emissivity profile, q ~ 3
Duro et a1 (2011) measure the broad iron line of Cygnus X-I as seen by XMM-Newton in the EPIC-pn modified timing mode. They rep... | |
space_sciences/03914_3.txt | n (STI) Program Office plays a key part in helping NASA maintain this important role.
The NASA STI Program Office is operated by Langley Research Center, the lead center for NASA's scientific and technical information. The NASA STI Program Office provides access to the NASA STI Database, the largest collection of aero... | |
space_sciences/24946_107.txt | ticles have short enough mean free paths, andthey have been sufficiently scattered before they arrive at PSP.Without considering intervening transient interplanetary structures (such as the presence of an interplanetary CME; seeZhuang et al. 2022), the path length estimated by Chhiber et al.(2021) assumes particles hav... | |
space_sciences/05099_107.txt | varies (see the right panels of Fig. 4, Fig. 7, and Fig. lo), the loop always expanded toward the coronal source, agreeing with the flux rope model.
There are some observations which cannot be explained by the flux rope model or any of the other models in the literature. In the April 15 flare, when the HXR impulsive p... | |
space_sciences/07054_21.txt | , where itcould supplement what we think is a desirable thing . . . anorbiter on station. Owen Garriott, who flew on Skylab, has beenpioneering the activity of long-duration orbiters that could beleft at the Station and relieved on Station by another orbiter,thereby relieving the burden of having to rely on the lifeboa... | |
space_sciences/16438_105.txt | tematics. Measuring the tensor-toscalar ratio r below a level of σ(r)=0.01 requires mapping at least hundreds of square degrees of sky tonoise levels well below 10 μK in a 1-arcmin pixel (or 10 μK-arcmin), which is the lowest noise level achievedin any current CMB observation of a patch of sky larger than a few square ... | |
space_sciences/20099_18.txt | , (34∘N, 104∘W) on 25 September 2015. Thefour dosimeters onboard RaD-X each collected over 20 h of science data. RaD-X operated in Region B, whichwas defined to be above 32.5 km, for just over 6.5 h. At sunset, the balloon dropped in altitude, and an operational valve down was initiated to further drop the balloon lowe... | |
space_sciences/11637_125.txt | e number. otes
Flux-weighted (first moment) centroids are calculated for all targets. PRF centroids are also computed, but only for a small subset (PPA_STELLAR) of the long cadence targets due to the heavy computational requirements of the PRF centroiding algorithm. The PRF fitting does not necessarily converge for tar... | |
space_sciences/21847_122.txt | l line of that same previously-emerged bipole. For the AR jets studied by Sterlinget al. (2017), the jets occurred in a homologous fashion according to scenario (b). Forthe AR jets of Sterling et al. (2016) however, at least one of the jets (see §3.5 of Sterlinget al. 2016) appears to have occurred along the internal n... | |
space_sciences/16154_15.txt | remodels, are due to the modification of the atmospheric structure caused by the abundance stratification.
ues, due to the radiative levitation of heavy elements. A similar effect can be seen in broad-band U, U − V photometric data(Ferraro et al. 1998, G1). The work of Behr et al. (1999, 2000b)and Moehler et al | |
space_sciences/14635_76.txt | e that the summit of ~launa Kea has always had within the indigenous Hawaiian community.
yFacilities: Subaru (Suprime-Cam), MIlIT (Hectospec), Keck (DEIMOS), Subaru (FOCAS), GALEX, Mayall (MOSAIC, NEWFlRM), and UKIRT ("'"FCAM)
Kashikawa, N., et al. 2002, PASJ, 54, 819 | |
space_sciences/24595_200.txt | d to Mercury’sDust Ring
Starting with the crater database from Kinczyk et al. (2020)we provided age estimates for six Class 5 (fresh-looking)craters with D > 40 km. Many other fresh-looking craterssmaller than 40 km are also present on the surface of Mercury.As described by the crater production function (e.g | |
space_sciences/07664_14.txt | sks. Therefore,complete and accurate models, simulations and testingare important for a successful mission.
The software factors previously noted are common toall space software. The software unique to probes isthe entry, descent and landing software that controlsthe most perilous phases of the mission. This software,f... | |
space_sciences/02343_263.txt | t Flight of the Adwmced Thin Ionization Caloriraeter (ATIC) Balloon Experiment. AmericanPhysical Society Meeting, Washington, DC, April 28-May 1,2001. Bull. APS, 46(2), 2, 2001.G. Case, S. Ellison, R. Gould, D. Granger, T.G. Guzik, J. Isbert, B. Price, M. Stewart, J.R Wefel,L. Mock, | |
space_sciences/10031_135.txt | tlers since tlie STIS ilperture, n-it11 ori- eiitatioii. siiliiplt" a oilly tliirl slice of tllr u-inrl str~rctureBJ- coliip;tririg ITSTISTIS observatioiis obser\-cd wit11 difl ferei~t positiori angle it~ld phase. n.c get iildicittioiis of thc origin of tlie | |
space_sciences/14408_1.txt | INFRARED AND X-RAY SPECTROSCOPY OF THE KES 75 SUPERNOVA REMNANT SHELL: CHARACTERlZING THE DUST AND GAS PROPERI'lES
TEA TEMIM"', PATRICK SLANE', IUC'-IA!tD G. ARENDT"', AND ELI DWEK' Accepted bv ApJ
ABSTRACT | |
space_sciences/07748_72.txt | t to 4 pages. Please revise your letter in order, to meet the page limit.
3 Au: "cf." means "compare"; is this correct here, or do you mean "see" or "e.g.)rr?
4 Au: Table 1: It is not ApJL style to have two separate sets of column heads. Table 1 has been split in two. Please check that all table references are correc... | |
space_sciences/26076_515.txt | Mazarico, Sunlit pathways between south pole sites of interest for lunar exploration - ScienceDirect). Planning this ~55km traverse involves finding a path that prioritizes illumination (represented as yellow or white) and minimizes periods of darkness (represented as blue or black) resulting in an approximately 30-day... | |
space_sciences/12824_23.txt | l. 2003), the IRAC images have a higher spatial resolution (~ 2" vs. > 6" of earlier surveys), which has led not only to a better estimate of source fluxes, but also to more accurate source positions for follow-up spectroscopic observations.
The spectroscopic sample was selected using (RAC color criteria based on the ... | |
space_sciences/16617_287.txt | mcheva, I. G., Lee, J. C., Ly, C., et al. 2013, AJ, 145, 47Moustakas, J., Zaritsky, D., Brown, M., et al. 2011, ApJ, submitted(arXiv:1112.3300)Nagao, T., Maiolino, R., & Marconi, A. 2006, A&A, 459, 85 | |
space_sciences/11244_40.txt | d by an electrically-commutated gearmotor that drives the spindle shaft via a spur geartrain. The output shaft is support by a bearing pair at the nose (near the torque coupling to the bit) and a single deep groove bearing at the rear (under the spindle gear). The maximum mean contact stress in the bearings is kept low... | |
space_sciences/14506_32.txt | iit Boch;un, 0-44780 Bochum, Germany 20 Dept. of Physics, University of 11aryland, College Park, MD 20742, USA 21 Dept. of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, tTS_\ 22 Oskar Klein Centre and Dept |
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