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space_sciences/16184_91.txt | 0.8 magnetotail identification criterion of Maezawa et al. [1997]. According to this criterion, the 23 RE half-width of the magnetotail in the east/west direction exceeds the 18 RE half-width in the north/south dimension. Were the criterion to be raised to |Vx|/V < 0.5, the magnetotail cross-section would be nearly ci... | |
space_sciences/09604_52.txt | t prediction limits. Smoothing removes a considerable amount of the choppiness that ain figure 2. The occurrences of the 12-mma of ΔRmaxpos are across the top, the individual valuesthe 12-mma of ΔRmaxpos are to the upper right, the occurrences of the 12-mma of ΔRmaxneg areacross the bottom, and the individual values of... | |
space_sciences/23366_84.txt | laxies. This represents a fundamental shift in thinking about starburst efficiencies in galaxies of different mass.
For /β to increase either must increase or β must decrease, or both. For the highest mass galaxies the valuesof and β must converge to 1.0 to maintain an outflow. This would require that all radiation f... | |
space_sciences/12791_49.txt | e experimental efforts essential to achieving even the first detections.
DETECTING GRAVITATIONAL WAVES
All GW detectors today operate by monitoring changes in the light travel time between point masses caused by a passing GW. In this section we give an overview of the key ideas in GW detection, and a brief survey of cu... | |
space_sciences/15527_103.txt | f the slow solar wind, Sol. Phys., 277,355-373, doi:10.1007/s11207-011-9909-0.Riley, P., J. A. Linker, and Z. Mikić (2001), An empirically driven globalMHD model of the corona and inner heliosphere, J. Geophys. Res.,106, 15,889–15,901, doi:10.1029/2000 | |
space_sciences/21772_106.txt | . . . . . . . . . . . . . . . . . . . . . . . . . . 249 Homogeneous strengthless model of atmopheric entry of asteroid 2008 TC3. Individual images show the asteroid at times t = 0:5 s, t = 2.7 s, t = 3.5 s, t = 4.0 s, andt = 4.5 s, respectively | |
space_sciences/16216_7.txt | sity of California, Santa Cruz, CA95064, USA15Universite Bordeaux 1, CNRS/IN2p3, Centre d’ ´ Etudes Nucl ´ eaires de Bordeaux Gradignan, 33175 Gradignan, France ´
ABSTRACT
We report the discovery of the millisecond pulsar PSR J2043+1711 in a search of a FermiLarge Area Telescope (LAT) source with no known associations,... | |
space_sciences/13748_202.txt | m STEREO and Wind instrumentation. Solar Phys. 256, 201.doi:10.1007/s11207-009-9350-9.Bisi, M.M., Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M.: 2009b, Coronal mass ejection reconstructions from interplanetary scintillation data using a kinematic model: a brief review. In: Duldig, M. (ed.) | |
space_sciences/23255_163.txt | 1-D photochemical model to simulate a modern Earth-like atmosphere on TRAPPIST-1e.Their results also show that H2O lines are very shallow and their detection with JWST will be extremely challenging.TRAPPIST-1e has an orbital period of 6.1 days and orbits in the HZ of a 2550 K star. Its incident flux is colder thanany o... | |
space_sciences/16848_80.txt | , a best-fit flatmodel gives χ2/dof = 0.15/2).
SN 2005db. This SN was observed on three epochs, abouttwo years after maximum light (676–695 days), using Swift/XRT. The combined image, with an exposure time of 13.6 ks,shows a faint source (five photons) with an FAP of 2×10−4 pertrial. However, given the fact that we hav... | |
space_sciences/02160_51.txt | r the differences in theatios of compounds between experiments and those observed inhe meteorites, e.g., 3-deoxyhexonic acids are relatively abundantn the glucose experiments (Fig 3C) but relatively minor productsn Murchison. It should be noted that if alkaline alteration ofugars was actually the principal mode of form... | |
space_sciences/17402_70.txt | r) component (Laor1991) was included in our model spectrum and applied toall spectra. The Laor model parameters are the line energy,EL, the emissivity index, a dimensionless inner disk radius,rin = Rin/Rg (with Rg = GMBH/c2), inclination, i, and thenormalization of the line, NL (in units of photons cm−2 s−1).Note that ... | |
space_sciences/14561_23.txt | , F. Ozel, L. PD. Psaltis, N. Rea, P. Reig, Tiengo, D. Torres, R. Turod1, L. Zampieri, S. Zane,
The (curThe LOFT Coordination Team: Belloni (INAF, Italy), J. Braga (INPItaly), T. Courvousier (Univ. Geneve, SCzech Republic), G.L. Israel (IN | |
space_sciences/17798_10.txt | e to a change in policy by the U.S.Navy, the NVI support contract was ended. At the beginning of 2012 the VLBI division hadfilled only three positions, Dr. Kerry Kingham, Mr. David Hall, and Ms. Roxanne Innis. BruceThornton was hired in February, and in May Mr. Daniel Veillette joined the VLBI division. Dr.Kerry Kingha... | |
space_sciences/00283_8.txt | , Meibom A., Krot A. N., Wood J. A., Keil K. (2000) The condensation origin of zoned metal gainsin QUE94411: Implications for the formation of Bencubbin/CH - like chondrites. Lunar Planet. Sci. 31,Abstract # 1606, Lunar and Planetary Institute, Houston (CD-ROM).*[7] Petaev M. I., Meibom A., Krot A | |
space_sciences/16466_310.txt | y, Centro Astronónomico Hispano-Alemán,c/ Jesús Durbán Remón, 2-2, 04004 Almería, Spain 26 Nagoya University, Japan 27 Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117Heidelberg, Germany 28 Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen,The Netherlands 29 Hersch | |
space_sciences/17155_158.txt | o low to match the numberdensity of their z = 2 counterparts.
Recently Carollo et al. (2013) claimed that the numberdensity of small early-type galaxies in the L∗ mass rangehas not strongly evolved since z ∼ 1. We rule out thatfield-to-field variations explain the discrepancy with ourresults. All five fields show a dec... | |
space_sciences/14836_143.txt | 448, 172 - 175
Delio Russo, N., DiSanti, M. A., Magee-Sauer, K., Gibb, E. L., Mumma, M. J., Barber, R. 1., and Tennyson, J., 2004. Water production and release in comet 153P/Ikeya-Zhang (C/2002 Cl): accurate rotational temperature retrievals from hot-band lines near 2.9-llm | |
space_sciences/14247_391.txt | f the most massive stars sink to the cluster’s centre dueto mass segregation before they evolve and explode. There, they start to physically collide. The most massive star gainsmore and more mass and forms a runaway star that may collapse to form an intermediate-mass black hole (Freitag et al.,2006a,c, Gürkan et al., 2... | |
space_sciences/22408_50.txt | 6). HEX-P will detect the majority of these sources, including those in the central Galactic cusp. The broad HEX-P energy band will enable classification of the sources, distinguishing the unbroken power law tail of BH binaries from the optically thin thermal bremsstrahlung (with ionized Fe emission lines) of magnetic ... | |
space_sciences/23801_20.txt | sodeduring which the flux fluctuated by a factor of 3 overa timescale of seconds. Such variability episodes are aparticularly rare feature of the most energetic bursts,and may be associated with super-expansion of the stellar photosphere (in’t Zand et al. 2019). In particular,in’t Zand et al. (2011) suggested that such... | |
space_sciences/00098_24.txt | catesthat the Lx/LH_ ratio is a good indicator of the presence of AGNs. Hard X-ray surveys conductedat high angular resolution, such as afforded by Chandra, would be crucial to refine the true AGNfraction in nearby galaxies. | |
space_sciences/00942_26.txt | e light cylinderalong open field lines above the null charge surface cannot be replenished frombelow. The first outer gap 7-ray pulsar models (Cheng, Ho & Ruderman 1986[CHR]) assumed that emission is seen from gaps associated with both magneticpoles, but this picture, although successful in fitting the spectrum of the ... | |
space_sciences/04797_99.txt | E. Mayer, B. E. Jaegar, R. K. Crane, and X. Wang, “Ka-Band Scintillations:Measurements and Model Predictions,” Proc. IEEE, vol. 85, no. 6, pp. 936–945,1997.[11] D. C. Cox, H. W. Arnold, and H. H. Hoffman, “Observation of Cloud Produced Amplitude Scintillation on 19 and | |
space_sciences/24770_839.txt | 2022.05.026, (in press).Richardson, I.G., 2014. Identification of Interplanetary Coronal MassEjections at Ulysses Using Multiple Solar Wind Signatures. Sol. Phys.289 (10), 3843–3894. https://doi.org/10.1007/s11207-014-0540-8.Richardson, I.G., 2018. Solar wind stream interaction regions throughoutthe heliosphere. | |
space_sciences/18636_122.txt | icant evolution in the best-fit [OIII]–Hαrelation in the ∼4.5 billion years elapsed between these
two epochs. We make the working assumption that therelation continues not to evolve significantly out to redshift z ∼ 2, or, in other words, that any evolution ismasked by the large scatter observed in the relation.
To fit... | |
space_sciences/22715_27.txt | meters on thecontinuum model was later confirmed by Boldin et al. (2013).
In this paper we present an analysis of data taken during agiant outburst of 4U 0115+634 in 2011 with Suzaku and RXTE.These data were previously analyzed by Iyer et al. (2015), whoclaim the detection of complex and strong cyclotron lines. InSect.... | |
space_sciences/04126_229.txt | f edles, mean speed and, arguably, a mean pattern and intensity for the field being transported. If the mean number of eddies, mean speed, and mean field properties can and do change by their own magnitude from one ensemble to the next in the sequence, say from one epoch to another, then the sequence variance will not ... | |
space_sciences/06868_94.txt | d of a power-law, a PEXRAV component, and a LAOR diskline component. We tested inclination angles of 30", 50", and 70". The outer radius Rout was kept fixed at 400 R,. The inner radius Ri, was kept free, but in all fits, Ri, went to very large values, usually 250-350 R,, with very poor constraints. Several values of th... | |
space_sciences/19890_25.txt | rammable computer board and an off-the-shelf Light-EmittingDiode (LED). Because the LED tests are inexpensive (∼ $100 US of totalequipment) and can be readily reproduced by other meteor camera networks,we will focus on those tests in this work.
The Arduino board was programmed to increase the duty cycle of theLED in 25... | |
space_sciences/01432_39.txt | k positive fluxes visible in Figure 1 have a signal-to-noise ratio,--7.
Since the FUSE bandpass stops short of wavelengths where the unobscured continuumHE2347-4342 is visible (A > 1190 /_), we obtained low-resolution HST/STIS spectratemporaneously with the FUSE observations to establish the continuum level. On0 August... | |
space_sciences/10089_4.txt | eDRUMS can completely suspend a baseball-sized solid or liquid sample during combustion or heat-based synthesis. Because the samples never contact the container walls, materials can be produced in microgravity with an unparalleled quality of shape and composition. The ultimate goal of the SpaceDRUMS hardware is to assi... | |
space_sciences/15884_8.txt | : starburst –X-rays: galaxies
Online-only material: color figures
1. INTRODUCTION
Ultraluminous infrared galaxies (ULIRGs) emit most of theirtotal energy output in the far-infrared (FIR) domain, with anFIR luminosity greater than 1012 L (Sanders & Mirabel 1996).Many ULIRGs are a composite of an active galactic nucleus(... | |
space_sciences/03373_24.txt | n the companion's outer layers. While it is not conclusively known whether the compact object is a BH (see Schmutz, Geballe & Schild 1996 who estimate compact object mass at > 7 solar masses) or NS (Hanson, Still & Fender 2000, Mitra 1998) the existence of giant radio flares and strong, relativistic and variable radio ... | |
space_sciences/22598_67.txt | g t = x∕Vsw (assuming aconstant solar wind horizontal flow speed Vsw). In the present model, this approach is extended by matchingthe upper boundary parameters of the 1-D electron cloud solution with the expansion front of the self-similarsolution, 𝜉f = −Mzf ∕x, parametrized by | |
space_sciences/26228_99.txt | ktransition; and (iv) the hEzi component remains nearzero throughout the shock transition.
It is worthwhile noting that the form of the transverseaveraged cross-shock electric field hExi leads to atransverse-averaged cross-shock potential hφi with afunctional form vs. x that is very similar to the change inthe transver... | |
space_sciences/05518_96.txt | V, where the K edges for the different oxygen ions appears according to the ionization parameter.
The top-left plot (log(<) = -3) represents the opacity for a low-ionized plasma, where a sharp K edge appears near to the 545 eV region, due to 0 I as well as the resonance structure near 530 - 540 eV that correspond to t... | |
space_sciences/00752_30.txt | luncertainties. Therefore minor ions may be treated approximately as test particles in thesolar wind. A comparison between the UVCS observations and the model results is shownin Figure 3 (from Hu, Esser and Habbal 2000).
We also examined the accuracy of a common FIP effect diagnostic, the ratio of Ne VI toMg VI lines i... | |
space_sciences/17669_25.txt | e band-gap of the semiconductor pass right through the device and do not contribute to the photo-generated current. High energy photons can be absorbed, but the resulting elec- trons are collected and extracted at a lower voltage limited by the semiconductor band-gap. Any difference in energy between the photon and the... | |
space_sciences/10029_43.txt | Von photopion production. The inelasticity rapidly drops for higher incidentproton energies.
As shown in Ref.[14], in order to modify the effect of photopion productionon the UHECR spectrum above the GZK energy we must have δπ > δp. It isshown in Figure 10 of Ref. [30] that for most of the allowed parameter spacenear t... | |
space_sciences/13878_11.txt | r any known stellar-mass black hole, hence the term "ultraluminous".
Based on their variability on short timescales (some ULXs are known to vary on timescales of the order of a few minutes) and high luminosities, some ULXs are almost certainly powered by accretion onto black holes (excluding the population of X-ray br... | |
space_sciences/19737_5.txt | t, the Simulation Interoperability Standards Organization (SISO) is developing a Space Reference FOM. The Space Reference FOM Product Development Group is composed of members from several countries. They contribute experiences from projects within NASA, ESA and other organizations and represent government, academia and... | |
space_sciences/09380_18.txt | easing global star-formation rate density (e.g., Ghosh & White 2001). In this scenario, HMXBs trace the immediate star-formation rate of a galaxy and LMXBs trace its starformation history with a lag of a few Gyr. With the advent of deep Chandra and XMM-Newton surveys (see, e.g., Brandt & Hasinger 2005 for a review), it... | |
space_sciences/05915_48.txt | 3f instrument. In any event, there seems to be little point in continuing along these same lines. We intend to perform new searches among smaller ,orains (0.1 - 1 pm) from Acfer 094, taking advantage of the much higher sensitivity and smaller beam size of the NanoSIMS. Since automated ion mapping in the NanoSIMS is not... | |
space_sciences/17150_40.txt | s slightly from theconvention used in previous analyses of the ACT data ([16, 22]). In each case we describe theparameterization used in the fiducial model; in a later section we consider possible extensionsor modifications.
In the rest of this section we describe how each of the components in eq. (2.4) aremodeled. To ... | |
space_sciences/06882_46.txt | n a reaction with a sufficiently energetic proton (Le. one that fulfills the kinematic threshold). This results in a condition for the column density of the plasma which is identical to that of a critical nuclear chain reaction (we re-iterate for the benefit of the reader that criticality is a condition on the column d... | |
space_sciences/22751_144.txt | t either include many or implement a complexdetection algorithm,• the sinusoidal signals were often time varying, requiring additional nuisance model parameterswhich exacerbate many of the problems listed above. | |
space_sciences/05015_149.txt | tage, from 2:l for Fe I1 to 1.7:l for Fe IX. The energies of the Ka components moves down with increasing ionization, by -5 eV, across the third row, due to the interaction between the 2p and the 3d orbitals. The KP energy increases monotonically with increasing ionization. The character of the profile changes qualitat... | |
space_sciences/26341_137.txt | . 2016, ARA&A, 54, 227Keating, B. G., Shimon, M., & Yadav, A. P. S. 2013, ApJL, 762, L23Kisner, T., Keskitalo, R., Zonca, A., et al. 2021, hpc4cmb/toast: UpdatePybind11, v2.3.14, Zenodo, doi:10 | |
space_sciences/09655_118.txt | r within the Orion Nebula cluster, where the bulk of stars have t < 3 Myr. The age discrepancy is similar to the case of S96, but otherwise the situation is different, because S96 is much more massive than the Orion Nebula cluster, and the older population resides in the outer region of S96 | |
space_sciences/13880_93.txt | e official XSPEC manual and in the brief cookbook, which will be delivered together with the source code. As a general concern for users, we pOint out that usually the emerging spectrum obtained from the Comptonization of a seed photon population with any given energy distribution S(E) can be presented as the sum of th... | |
space_sciences/22643_101.txt | ..........................................4-2Figure 4-5 Spacecraft Assessment Graphs Selection Window .................................................................4-3Figure 4-6 Spacecraft Assessment Average Flux vs. Size Graph.................................................... | |
space_sciences/15320_10.txt | , heated plasmas, or deflected flows [Omidi et al., 2009]. The signatures of hot flow anomalies and foreshock cavities have been seen in the magnetosheath, and the corresponding pressure variations may cause large amplitude magnetopause motion and perturbations of the magnetospheric magnetic field [Paschmann et al., 19... | |
space_sciences/04263_21.txt | h that the main components in the LW/R spectrum match those in the corresponding SWP spectrum.
Another source of uncertainty in this study is the non-uniform time epoch. As Cha & Sembach (2000) have shown, the velocities and the equivalent widths of the interstellar line components in this region can vary of time scal... | |
space_sciences/13302_91.txt | f the two GPHS heat sources, one for each advanced Stirling convertor (ASC). Each GPHS module is surrounded by insulation to minimize heat leakage thus maximizing heat input to the convertors. The displacer side of the ASC is toward the GPHS module and cold-side is attached to the housing via the cold-side adapter flan... | |
space_sciences/13321_30.txt | ruded into the flow the same distance from the sting (within 0.5 mm).
A more thorough description of the facility, including detailed explanations of the gas injection system, the instrumentation available in the facility, schematics and photographs, comparisons with other similar facilities, and measured free stream ... | |
space_sciences/24987_566.txt | 7. doi:10.1088/0004-637x/698/2/l152
Shimizu, T., Imada, S., Kawate, T., Ichimoto, K., Suematsu, Y., Hara, H., et al.(2019). “The Solar-C_EUVST mission,” in UV, X-Ray, and Gamma-Ray SpaceInstrumentation for Astronomy XXI of Society of Photo-Optical InstrumentationEngineers (SPIE) Conference | |
space_sciences/17066_185.txt | l, T. R., Ishibashi, K., &Hillier, D. J. 2003b, ApJ, 586, 432Smith, N. 2006, ApJ, 644, 1151Smith, N. 2011, MNRAS, 415, 2020Smith, N. 2013, MNRAS, 429, 2366Smith, N., & Frew, D. J. | |
space_sciences/12049_6.txt | f (X Tauare given in Table 1. UV EMISSION LINES IN RED GIANTS
Almost all late-type evolved giants show signatures of plasma at T of 10,000 -300,000 K. We have compiled and analyzed data obtained with HST/GHRS,HST/STIS and FUSE on evolved late-type stars [1, 2, and 3] for this study. These dataindicate that: | |
space_sciences/15340_168.txt | f!galaxy!properties!as!a!function!of!the!effective!radius
This! provides,! as! a! function! of! reff,! the! effective! solid! angle! of! the! galaxy! after! PSF!convolution!Ωeff;!the!shape!penalty!factor!fpen,!defined!by which! is! 1! for! a! well+resolved! Gaussian! galaxy! (Bernstein! | |
space_sciences/14054_55.txt | 8] also fail to reproduce the bulk flow result using Planck and ROSAT galaxy clusters.
The detection of a non-zero mean pairwise momentum from a kSZ signal presented here can also be interpreted as a measure of baryons on cluster length scales; a deficit of observed baryons has long been a cosmological puzzle [39]. Ou... | |
space_sciences/10358_63.txt | g for the gain in dark ramps via equation I of Rauscher et al.(2007). We also compared our results to ultra-low light level data collected for similarFPAs undergoing testing for the JWST Near-Infrared Spectrograph project (Rauscher, priv.comm.). These results all confirm the gain decreases with signal level and that th... | |
space_sciences/26220_57.txt | e vertical shear of the BW (𝜏BWsh, §2.1.4). These torques cause the most important aspects of the wake’srotation, which we analyze in the idealized case of an isolated wake (§2.1.5). Later, we derive the torque due to thewake-to-wake gravitational interaction (𝜏wake, §2.1.6) and study its effect (§2.1.7).
2.1.1. | |
space_sciences/14241_74.txt | . The aquanauts used these products to successfully train themselves and carry out these unfamiliar tasks.
The NEEMO 16 mission was highly successful. All major mission objectives were accomplished and over 1200 data points were collected to inform our decisions on NEA exploration operational concepts, EVA tools, and c... | |
space_sciences/09321_74.txt | s other than Ne, which is especially prominent; 0 is only slightly higher than average.
In the bottom panel of Figure 6, we compare regions without significant abundance enhancements-the SE Arm extending south from the BEK, the SE Low SB region, and the eastern edge of the BEK. The latter two are prominent in the 0 VI... | |
space_sciences/13931_44.txt | 0s showed the promise for transforming our knowledge of ecosystems and the services they provide us [25].
NASA’s Earth Observing System (EOS) and its suite of diverse sensors were developed in the 1990s and now form the basis for an enormous amount of earth science research and improved understanding [12]. The recognit... | |
space_sciences/25693_51.txt | l as in Series One, each subject gave an acceptability score and feedback after the session was completed.
Methodology and Data Collection
For both series of studies, a task acceptability scale was used by the subjects. Task acceptability is the ability to complete a task effectively, efficiently, and reliably without... | |
space_sciences/10655_41.txt | luding the Auger effect), Comptonheating, charge transfer and collisional de-excitation. The cooling term includes radiativeand dielectronic recombination, bremsstrahlung, collisional ionization, collisional excitationof bound levels and charge transfer. All processes include their respective inverses so thatthe popula... | |
space_sciences/09370_33.txt | s, and are nuillbered for ease of reference to iildividual regions and features. The nebular enlissioii consists of a few regions of knots towards tlle center of the renlilaiit (boxes 1,2 and 3), the bright NW knots (boxes 5 and G), knots and faint filailleilts along tlle iiortlleril limb (box 7, extendiiig into G and ... | |
space_sciences/12077_5.txt | f type II bursts, thus29 confirming the close physical connection between type II bursts and CMEs. The average height30 (~1.5 Rs) of STEREO CMEs at the time of type II bursts is smaller than that (2.2 Rs) obtained for31 SOHO (Solar and Heliospheric Observatory) CMEs. We suggest that this may indicate, at least32 partly... | |
space_sciences/11398_14.txt | r neutral ptssignificantly overestimate wind opacity. Unfortl.111atf'l,y.due to the lack of easily available tools for incorporatingappropriate radiative transfer and opacities, inadequatemodels, such.as those intended for neutral interstellarmedium absorption, are routinely applied to account forwind attenuation. This... | |
space_sciences/13953_82.txt | RELL2 and MEDICINA/NOTO it was 60–70 mJy.
5 DATA ANALYSIS: H2O MASER SOURCES
When scrutinizing the cross-correlation spectra, I found severalobjects with very strong peaks in IF9; for example, the object0221+618 at the baseline MEDICINA/ONSALA60 (see Fig. 3). | |
space_sciences/16728_109.txt | Uand ∼95 AU, respectively. These resonant populations are shownin Fig. 6. Typically, a population in 3:2 resonance is associated with capture during outward planetary migration, as is thecase in our own solar system (Malhotra 1993, 1995). But here,these structures is most probably appear because we used thechaotic-zone... | |
space_sciences/03160_84.txt | d data (taken downstream from ACE) show both alphas and protons takingart in the waves. His hypothesis is that we are observing the evolution of the waves and their effects as thewind travels between tile spacecraft. Peter Gary's analysis at LANL suggests that the spacing between thewo s/c may be sufficient to see the ... | |
space_sciences/13746_183.txt | r Vtt when δ = 7 agrees rather well with the result from the spectral comparison,however. The results also agree qualitatively in that Vtt for δ = 3 is larger than Vtt for δ = 7in both cases. But the quantitative results for δ = 3 do not agree. The model assumptionthat V (N) is constant in the thick-target region is cl... | |
space_sciences/22711_25.txt | hly ionized ions,in order to model absorption features associated to O VI–O VIII ions.
Fig. 1 shows the oxygen photoabsorption cross-sections includedin the present analysis. Note that, in the computation of such crosssections, the Auger broadening can be the dominant broadening
process, and is included. As the plot sh... | |
space_sciences/03885_52.txt | o favor the soft EOSs [Baym & Pethick (1979)l.
We conclude that (1) the application of our analytical model to the data leads to the determination of the NS mass and radius as a function of the distance to the system. For the range of allowed distances 4.5-5.0 kpc we obtain rather narrow constrains for the NS radius i... | |
space_sciences/26327_376.txt | 2010; Opher et al. 2011).
As discussed by Burlaga et al. (2020a), there is no compelling direct evidence in Voyagerdata for magnetic reconnection, even in the distant IHS. On the other hand, observationsalone are not sufficient to conclude that magnetic reconnection does not occur and, arguably,reconnection cannot rea... | |
space_sciences/03650_153.txt | r model calculates the particle radial drift rate using a constant pressure gradient term y (see section 1.2), which will not be the case towards the outer edge of the nebula.
During the very same initial lo5 years when CAIs seem to have formed, the inner nebula was hot enough to evaporate quite a large mass in inward... | |
space_sciences/23490_64.txt | f hemispheric asymmetry. Results of each case are discussed in thefollowing paragraphs and figures.
The injected primary EDF in our cases was selected by Equation 2 with the characteristic energy ofE0 = 1 keV and the normalized constant C to provide the energy flux equal to 1 erg * cm−2 * s−1. The resultsof these stead... | |
space_sciences/18008_41.txt | ∼41%for the GP of center flares and ∼23% for the GP for limb
flares. We take limb flares to have an east–west location >70◦.Using the five flares seen in the TIM TSI and estimatedVUV emission simultaneously obtained from TIMED SEEand GOES, respectively, the TSI flare irradiances during TIMeclipse periods can be reconst... | |
space_sciences/18755_20.txt | tions over a longer period of time than can be allocated in “cryo interruptus” mode. As such, one of the two UVVis flight operational windows was intended to be mainly a focusing and calibration window, working with the BIRC bench in “cryo interruptus” mode. Encouraging pointing results were demonstrated, despite conse... | |
space_sciences/16981_90.txt | s made of glass”, SPIE 8861, 10 24pp (2013). 23 Zhang, W. W., Biskach, M. P., Blake, P. N., Chan, K. W., Evans, T. C., Hong, M. L., Jones, W. D., Kolos, L. D., Mazzarella, J. M., McClelland, R. S., O'Dell, S. L., Saha, | |
space_sciences/25230_162.txt | e of Technology.
Appendix AVarying Input Beam
A.1. Passband Variations
Variations in the detector passband will impact the shape ofthe effective beam and therefore affect the performance of thefitting algorithm. While we leave the detailed analysis of thisphenomenon for future work, it is useful to show how the inputbe... | |
space_sciences/21321_62.txt | f iPTF17cw, and theposition of its radio counterpart (see Figure 2).
Properly accounting for the on-axis point-spread function wemeasure a 0.5–7.0 keV count rate of 5.0 10 2.94.8 ´ 4 -+ - count s−1(90% confidence interval). Adopting a power-law spectral modelwith photon index Γ = 2 and NH ≈ 1 | |
space_sciences/04809_114.txt | easure all significant radiation components for which theNCRP (1996) had established minimal requirements. Also, the flightpackage had to be operational and the first flight occur before or near themaximum in the galactic cosmic ray intensity (ca. spring/summer 1997)and continue through the next cosmic ray minimum. The... | |
space_sciences/03899_130.txt | rbing gas assuming no response to continuum variations on a 10 days time scale for all absorbers. Using the temperatures from the models, we derived the following limits on the electron density (ne) and distance from the central .source (D): For the log(U0X) = -2.4 component, ne < 5 x lo4 cm-3 and D > 3.2 pc. For the l... | |
space_sciences/25099_8.txt | F, Cl, and OH abundances of apatite from primitive achondrite meteorites.
There are broad differences between apatite X-site chemistry in chondrite parent bodies (typically F-poor[3, Fig. 1]) compared to apatite from basaltic rocks from many achondrite parent bodies (Cl-poor, apart from Mars [2, 3]). These differences ... | |
space_sciences/06846_29.txt | 3).
2.2. Energy Dependence
In this subsection I assume that At=1.024 s, for which the background dominates the burst counts at threshold (i.e., B >> Cs). 1 calculate the number of source counts C, by convolving the burst spectrum with the effective area over the energy band AE. Figure 2 shows the current understandin... | |
space_sciences/13568_97.txt | n from radiation domination to matter domination (TRMD) 100,000 years after the big bang. As effects of both of these on the galaxy power spectrum are sensitive to the assumed cosmology, they provide additional leverage, making WFIRST a yet more powerful mission for studying cosmic acceleration. In the discussion that ... | |
space_sciences/00267_153.txt | rsand a possiblenew mechanismto producewatericemantles.Astrophy$.J.499:777-792.Bernstein,M. P.,Sandford,S.A., AIIamandola,L. J.,Chang, S.,andScharberg,M. A. 1995.Organiccompounds producedby photolysisof realisticnterstellarand cometary iceanalogscontainingmethanol. Astrophys. J. 454:327-344 | |
space_sciences/04475_7.txt | 2004 in press] did a follow up study on this aspect of the chorus, interpreting this frequency difference as a natural outcom: of the dependence of the whistler-& refractive index on the wave normal angle between the wave vector k and the static magnetic field Bo and the rapid motion of highly localized source region(s... | |
space_sciences/22366_67.txt | TRL: All ≥ 6.
4.6 TAP: A Next Generation Transient Observatory
The TAP mission provides a factor of ~10 improvement in instrument sensitivity andFoV compared to Swift (the current multi-band transient mission) (Table 4). In addition, TAP’sL2 orbit ensures minimal (~10%) Earth occultation, enabling improved rapid respo... | |
space_sciences/10803_154.txt | d in a variety of space mission applications, but may also beconsidered as developmental for several reasons. The various cross section comparisons withNIST calculations show several instances where the LaRC code cross sections may be improvedby introducing selective correction terms, even though the cross section devi... | |
space_sciences/07799_47.txt | x per day ((3 per 4 ye=.), a fzctor of 2 !ox..rer than the pre-f ight verification estimate. No MDM anomalies were observed during any of the 23 > 100MeV solar energetic particle events (extreme SEE environments) that occurred between April 200 1 and June 2005.
ISS MDMs are equipped with error detection and correction... | |
space_sciences/20940_171.txt | f the project risks and their current status. Risk #1: Performance Prediction
Risk statement:
If the model predicting LILT and radiation-optimized cell efficiency at the conclusion of development is incorrect, the project may not meet its objectives at the cell level.
Context:
At the time of the proposal, no LILT dat... | |
space_sciences/07613_49.txt | s best reviewed by Amman et al. (1995). Thus, Priscu et al. (1999) used this method and revealed the presence of representatives of the Alfaand Beta-Proteobacteria and the actinomycetes in samples of accretion ice from Lake Vostok. Among terrestrial models considered to develop a methodology for exobiological investiga... | |
space_sciences/00918_8.txt | h and release from the cargo bay, the IUS performedo firings and separated from the Observatory. Finally, after five firings ofandra's internal propulsion system - the last of which took place 15 dayster launch - the Observatory was placed in its highly elliptical orbit. Thisbit has an apogee of 140,000 km (1/3 of the ... | |
space_sciences/12967_21.txt | rature and in-phase baseband signals. The dynamic range of the system is about 90 dB. To ensure coherence of the transmitter/receiver, a 10 MHz oven controlled local oscillator is used to produce the clocks required by different parts of the system including the radio frequency gated signal for the transmitter. The des... | |
space_sciences/17178_111.txt | s, we find there isexcellent agreement between the Hα and SED SFRs.
This is in agreement with the work of Wuyts et al. (2011b).They compare UV+IR and SED SFRs and find excellentagreement between the SFR indicators for log10(τmin/yr) =8.5. They also compare the SFR indicators when a shorterexponential decay time of log1... |
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