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space_sciences/18481_305.txt | w-stat.stanford.edu/~mcoram/[Donoho 1994] Donoho, D., (1994), Smooth Wavelet Decompositions with Blocky Coefficient Kernels, in Recent Advances inWavelet Analysis, L Schumaker and G. Webb, eds., AcademicPress, pp. 259-308.[Donoho and Johnstone 1998] Donoho, D., and Johnstone, I.(1998), Minimax estimation via wavelet sh... | |
space_sciences/24181_8.txt | ecommendation: A dedicated coronal synoptic telescope with a large field-of-view(i.e., COSMO-LC) is needed to identify the dominant CME driving mechanisms, bymeasuring coronal magnetic fields from precursor state into eruption.
In the UV, a new opportunity has arisen to make use of the strong H I Lyman-α coronal line,w... | |
space_sciences/06251_30.txt | f an infinite number of junctions perfectly matched to a one-sun solar spectrum being 66%). It can thus be argued that quantum structures can exhibit global efficiency improvements by reducing thermal losses. Several approaches to accomplishing this in practice have been outlined [22-24]. However, it must be noted in o... | |
space_sciences/14188_227.txt | 4 515 [l27[ Ryan F 0 1995 PItIlS. Rev. 052 5707 [12SJ Ryan F' ]) 1997 Pill/s. Rev. 0 56 IS45 [129] BanlCk Land Cuth,.'!" C 2007 Pill/s. /lev. 0 15 0.12003 [130J finn I, S II"d Thorne K S 2000 PIIIIS. | |
space_sciences/25148_5.txt | 3) Ryugu –a unique opportunity to study space weathering on carbonaceous materials [4]. Initial studies have established that the surface morphology and chemical signatures of space weathering in returnedsamples share characteristics with laser irradiation experiments simulating micrometeoroid bombardment, indicating t... | |
space_sciences/07590_110.txt | ohesivematerials they observed the appearance of forbidden azimuthal zones in the ejecta distribution. These zones havebilateral symmetry, and extend both up and down-stream of the primary crater. They note that similar ejecta patterns are evident in large craters on the moon and planets. As well as the bulk ejecta fro... | |
space_sciences/22157_101.txt | rmal oxide patterning method for compensatingcoating stress in silicon x-ray telescope mirrors,” Proc. SPIE 10699,1069942 (2018).26. K. W. Chan et al., “Alignment and bonding of silicon mirrors for highresolution astronomical x-ray optics,” Proc. SPIE 10699, 1069940(2018).27. T. Saha et al., “Grazing incidence wavefron... | |
space_sciences/07003_21.txt | d to vacuum, heat is absorbed as CO2 and water vapor are removed from the sorbent. The consequent reduction in temperature during the regeneration period diminishes the rate at which CO2and water vapor can be removed from the sorbent, resulting in a reduced regeneration compared to an isothermal case.
An alternative c... | |
space_sciences/07817_181.txt | ; PSDs were generated by binning periodograin points by a factor of 25.
The S statistic was calculated by summing over temporal frequencies <10-~.~ HZ to exclude PSD points that were dominated by power due to Poisson noise. For all PSD pairs and bands, IS1 was found to 0.54 or less. Extending the duration to 74.0 ksec... | |
space_sciences/07547_3.txt | l and ionized atoms along with ionization loss in the thermosphere where charged and neutral populations interact. It will be shown here that trapped-belt flux J is bivariant in energy E and thermospheric neutral density ρ, as J(E,ρ). One can conclude that proton lifetimes in these belts are also directly affected by s... | |
space_sciences/14581_204.txt | s effectively in deep space at 1 AU, and will only encounter very short eclipse periods.
The magnetic cleanliness requirements are likely to be a driver for the AXIOM mission, as described in section 4.3.8. Electrostatic cleanliness is also required to avoid spacecraft charging.
5.5 Current heritage and critical issu... | |
space_sciences/22207_89.txt | . Adv. in Space Research, 2005, 36, 184 - 189.
9 Bartell, L. S.; Guillory, J. P. Electron-Diffraction Study of the Structure and Internal Rotation of Cyclopropyl Carboxaldehyde. J. Chem. Phys., 1967, 43, 647 - 653.
10 Johnson, S. Preface, A Dictionary of the English Language, 1755, London; W. Strahan | |
space_sciences/25109_10.txt | , Fl 32899202-358-7432Agency-Patent-Licensing@mail.nasa.gov
National Aeronautics and Space AdministrationAgency Licensing ConciergeKennedy Space CenterMS LASSO-012Kennedy Space Center, Fl 32899202-358-7432Agency-Patent-Licensing@mail.nasa.gov
www.nasa.gov
APPLICATIONS
The technology has several potential applications:
... | |
space_sciences/14913_106.txt | t the mean time between failure and modes of failure.
5. High-abrasion Dust
High-abrasion dust is characterized generically as in-situ regolith material the size of granules of sand or smaller in which no natural erosion processes are present; i.e., water or atmospheric mechanisms that have eroded or smoothed the edg... | |
space_sciences/01080_28.txt | aints on the temperature and density of the LIC,the magnetic field strength in the cloud remains poorly determined. While extremely high fields(> 8#G) appear increasingly unlikely due to the lack of detection of the heliosi)heric bow shock,the range of plausible values for the field still extends from _ 1 - 5#G. An arg... | |
space_sciences/20817_14.txt | e non-linear solver together with the Gauss-Seidel method as the iterative linear solver in each Newton iteration. The software is written in OpenCL and runs in parallel on the GPU cores, which allows for fast computation of large areas and long time scales. | |
space_sciences/02214_127.txt | , is not statistically significant compared to onewith vns sin i = 0 (see §4.3). The dashed curves show the models with vns sin i = 38 and 50km s-1, which are equal to our 90% and 99% confidence upper limits. The dotted curve shows thebest fitting model with Cdyn as an additional free parameter. This fit has Vns sini =... | |
space_sciences/16211_142.txt | e, such a study may give rise to insightsabout the average spectral behavior of the galaxy populations.
Cai et al. (2013) modelled dust-dominated galaxies togetherwith lensed high-redshift dust-dominated galaxies. However, Figure 6 indicates that at the ACT frequencies, this model underpredicts the counts, an effect al... | |
space_sciences/20940_140.txt | e for the array-structure portion of the Option I work, based on the provided SoW.
Responses to the RFI were received from Orbital ATK, DSS, SolAero and Lockheed Martin. Based on evaluation of these responses, we selected MegaFlex from Orbital ATK as the array-structure technology for JPL's EESP project. As detailed in... | |
space_sciences/16633_95.txt | d as atmospheric vapor. Titan’s high tropopause temperatureallows significant quantities of methane into the upper atmosphere. Theresolar ultraviolet light initiates a chemical cascade that converts methane intoreactive species that eventually lead to complex organic molecules. Becausethe produced hydrogen gets lost to... | |
space_sciences/07676_42.txt | O, they exhibit highly variable isotopic compositions depending on the diverse chondriteclasses and planetary objects. They result from : (i)nucleosynthetic processes ; (ii) heterogeneity in theSolar nebula ; (iii) fractionation processes uponaccretion ; (iv) differenciation and evolution ofplanetary objects. On Venus,... | |
space_sciences/04437_68.txt | n, and it would have to compete with other such missions atthe advisory committee and National Academy level. This could have a budgetless than the NGST, if the NGST aperture is sufficient, or larger, if the scientificgoals are sufficiently compelling to justify a larger telescope. It could have avariety of instruments... | |
space_sciences/21047_42.txt | i C0 pv2 A where the drag coefficient is the curve-fit of White 7,
In the drag equation, v is the relative velocity between the particle and the background flow. At every step of the ODE integration, relative velocity is computed by interpolating the background flow velocity onto the particle position. The background ... | |
space_sciences/16399_88.txt | t to estimate the effect of the residuals by analyzing clustersubsamples selected according to galactic latitude.
To summarize, we constructed two sets of maps, according tothe specific data sets: (A) CMB subtracted using a template, (B)CMB subtracted exactly using the 217 GHz channel. In simulation (A) six maps are co... | |
space_sciences/15221_73.txt | t show any absorption due toO VII; therefore, this line is still represented with a Gaussian profile. We have found largeresiduals around most of the oxygen absorption features, the most prominent being aroundthe O I and O II Kα lines. The fit statistics gives a poor reduced chi-square of χ2 = 1.769which forced us to r... | |
space_sciences/03876_109.txt | r 1978), where 1, is the normalized residual flux at that radial velocity.
For Cf < 1, the optical depth at a particular v,. is given by:
(Hamann et al. 1997~). The ionic column density is then obtained by integrating the optical depth across the profile:
(Savage & Sembach 1991), where X is the wavelength and f is t... | |
space_sciences/09518_139.txt | DMDs are a particular type of Micro-Electro-Mechanical Systems (MEMS). MEMS integrate microscopic mechanical elements, in our case moving mirrors, together with their control electronics on a common silicon substrate. Whereas t,he control electronics is fabricated using standard integrated circuit processes, the mechan... | |
space_sciences/02393_7.txt | e VIII, and the Raman scattering bands at 6830 ._, and 7088_. The Raman bands and other high ionization features vary considerably throughouthe outburst. These features will enable us to correlate variations in the FUSE spectrawith variations in tile optical spectra.
ppSecond, we began an analysis of FUSE spectra of Z ... | |
space_sciences/15177_109.txt | n front of theWD along our line of sight (Shore et al. 2012). Our best guessat the orbital period of V407 Cyg (43 years; Munari et al. 1990)is significantly longer than the timescale of our observations, sowe assume this viewing angle is constant across our radio lightcurve. We show a schematic picture of the binary in... | |
space_sciences/15315_54.txt | e perturbation (7) is the derivative w.r.t. u on the right-hand side:
The other ingredient in the waveform-mode perturbation (7) is the derivative w.r.t. u on the right-hand side:
After merger, the effective coefficient A/A˙ + iϕ˙
willasymptote to a constant complex number:
This implies a simple, QNM-driven leakage fr... | |
space_sciences/16737_15.txt | . 2004) toreproduce a dynamical solar spectrum at any epoch.
2. THE DATA
The remote-sensing OMI (part of the Aura instrumental suite;Levelt et al. 2006) has collected information about trace gasesin the Earth’s atmosphere since 2004 July. OMI comprises threedifferent spectral channels, UV1 (264–311 nm spectral domain,r... | |
space_sciences/21347_6.txt | B. P. Weiss, F. Westall, R. M. Wheeler, M. P. Zorzano), 1Department of Earth, Ocean & Atmospheric Science, Florida State University, Tallahassee, FL 32310, USA (humayun@magnet.fsu.edu).
Introduction: Based on meteoritic evidence, Mars accreted as early as 2 Ma after the formation of the first solids in the solar syste... | |
space_sciences/03533_42.txt | d. W. Russ Stone, p. 749, IEEE Press, 2002.
9. Cairns, I. H., and G. P. Zank, Turn-on of 2-3 kHz radiation beyond the heliopause, Geophys. Res. Lett., 29(7), 10.1029 2001GL014112, 47-1, 2002.
3 Presentations at Conferences or Institutions | |
space_sciences/16365_278.txt | 6, NGC 625,NGC 1705) than that in the H ii region. A trend might exist,with the discontinuity being essentially null for the lowest metallicity objects, and then constant around ∼1 dex for metallicities 1/6 Z (value in the ionized gas). However, if nitrogenis used as a metallicity tracer instead of oxygen, the resultsc... | |
space_sciences/24947_141.txt | ourlidas, A., Savani, N. P., Szabo,A., . . . Yu, W. (2016, May). A Circular-cylindrical Flux-rope Analytical Model forMagnetic Clouds. APJ, 823(1), 27. doi: 10.3847/0004-637X/823/1/27Odstrcil, D. (2003, August). Modeling 3-D solar wind structure. Advances in Space | |
space_sciences/22751_159.txt | d time series is tsBPk = tsk − ∆BPk. Sinusoid Removal. In development, it was planned that the SPSD detection would follow a harmonicremoval algorithm, so we almost decided to ignore issues which arose in light curves with periodic behavior.Concern that the harmonic removal might be incomplete in the presence of SPSDs ... | |
space_sciences/25761_102.txt | . The radius develops according to the parameterized spatial and temporal profile of buildup and decay in the program. If a value of zero or more than 10,000 km is used for StormMaxRadius, the storm is taken to be of global dimensions and uniformly covers Mars, and it builds up and decays in intensity according to the ... | |
space_sciences/00598_9.txt | nization lines has beenknown previously, these spectra show an extreme of this phenomenon. Furthermore, the
550 West 120th StreetMail Code 5347Tel: 212-854-3257Fax: 212-854-8121
July 31 2000 high-ionizationlinesarestronglyblueshifted;they havenearlynoemissionto thered sideof the rest wavelength | |
space_sciences/16310_12.txt | 3-49 HLX-1 (hereafter referred to as HLX-1) not only
is a ULX but is currently the best intermediatemass black hole candidate. If HLX-1 harbors anintermediate-mass black hole, it accretes at comparable fractions of the Eddington luminosity,as stellar-mass black holes in binaries (14). Hence,HLX-1 is expected to display... | |
space_sciences/04518_78.txt | cNamara 2003), the region around the radio emitting plasma is cooler than the surrounding gas. The central galaxy of Abell 2597 (Sarazin et al. 1995) is a luminous radio source and there are indeed "cavities" in the X-ray emission similar to those seen in Perseus and Abell2052 (McNamaraet al. 2001). However, analysis o... | |
space_sciences/15170_22.txt | y distribution for a measurementof polarization amplitude, a, and position angle, ϕ is given by
where a, a0, ϕ, ϕ0, and N are the measured amplitude, the true amplitude, the measuredposition angle, the true position angle, and the number of detected photons, respectively(see, for example, Weisskopf, Elsner & O’Dell 201... | |
space_sciences/09669_61.txt | f zf = 10, thenthe z′ − [3.6] = 5.4 color would cause one to infer aphotometric redshift of z = 1.39 for SpARCS J003550-431224, which is reasonably consistent with the spectroscopic value. One possibility for the overestimate of thephotometric redshift is that the BC03 models are tooblue at young ages, as suggested by ... | |
space_sciences/08240_22.txt | l, the H I-correlated component of the infrared einission was subtracted from the data,. Caseful error analysis, including estimates of systematic error ill subtraction of the iliterplanctary and Galactic foregrounds, sllo~ved that the mean residual intensity was significantly (more than 3a) greater thail zero at a11 t... | |
space_sciences/03424_158.txt | , Initiation-Promotion Model of Tumor Prevalence in Mice From Space Radiation Exposure. Radiat. Environ. Biophys. 34, 145- 149 (1 995a). EA. Cucinotta, Townsend, L. W., J.W. Wilson, J.L. Shinn, G.D. Badhwar, and R. R. Dubey, Light Ion Components of the Galactic Cosmic Rays: Nuclear Interactions and Transport. Adv. | |
space_sciences/07529_29.txt | d have been at one solar radius. This technique works well for CMEs showing a constant velocity. However, some CMEs show evidence for acceleration or, in some cases, deceleration in the LASCO C2 and/or C3 heightto-time plots. In these cases, linear fits to all LASCO height-to-time data clearly yield incorrect start tim... | |
space_sciences/22691_21.txt | e highest resolution availablewithin the MMS mission (see Yamada et al. 2016). Theadditional components are caused by a moderate inertial termfollowed by large pressure forces activated when approachingthe reconnection site. Basically, the electric field related to thefull electron pressure tensor becomes the main cont... | |
space_sciences/00776_381.txt | nly by private enterprise and the legal right of privateroperty in space and on the Moon. Finally, this paper adocates the use of lunar land grants as the key to unleashinge needed capital and the econormc power of private enterrise in the creation of a 21 st century lunar space economy. | |
space_sciences/20694_176.txt | ) project as an ongoing research projectthat tests and validates new and more energy efficient aircraft designs forflight. The goal of the project is to demonstrate a new capability-drivenapproach in aircraft aviation using an all-electric propulsion system.Validating an electric motor driven aircraft leads the way to ... | |
space_sciences/09390_98.txt | nspace human systems (e.g., EVA suits, life support).
7. References
Cohen, H. 1967 at http://www.sae.org/technical/papers/670622
Farquhar, R. W. et al. 2004, Acta Astronautica, 55, 687. | |
space_sciences/20765_10.txt | l model (§3.2); and a molecular-transport model (§3.3). As the methodologies for constructing these models were discussed in the previous papers10,11,12 of this series, the current paper describes updates to the models and to model parameters.
For a range of volatilities, we have used the CCMM to simulate the accumulat... | |
space_sciences/02803_63.txt | 9, A&A 347, 975Rowland, N., Houck, J. R., Skrutskie. M. F. et al., 1993,DACD 1_ 1_o _7 iSolar abundance from Grevesse et al. (1993) and Anders & Grevesse (1989)20, B star abundances are the average of Gies Gies & Lambert (1992) and Killian-Montenbruck | |
space_sciences/22119_21.txt | 6) J. Geophys. Res-Planet., 121, 1865-1884. [2] Keller L.P. and McKay D.S. (1993) Science, 261, 1305-1307.[3] Noguchi T. et al. (2011) Science, 333, 1121-1125.[4] Loeffler, M.J. et al. (2009) J. Geophys. Res- Planet., | |
space_sciences/15256_117.txt | d “Interviews with Apollo Astronauts” on February 23, 2010.
A 3-person team interviewed 8 of the 11 surviving Apollo crewmembers in a series of focused interviews to discuss their experiences on the lunar surface. Eppler presented the results of these interviews, along with recommendations for the design of future lun... | |
space_sciences/17120_109.txt | 2 1023+25 does notshow variability in either its thermal or non-thermal emission.
We fit the broad-band SED with the model described inGhisellini & Tavecchio (2009), focusing on the X-ray energyband as an important constraint, and we analyze in detail thenon-thermal jet emission of the source. We confirm that B21023+25... | |
space_sciences/07158_28.txt | s to be in error. A group of bit errors caused by one particle strike is called a burst. The exact bit pattern can convey much information regarding the location of the strike and the mechanism of the error event. For example in an alternating HI-LO pattern if a string of seven bits end up being LO, that is, three HI b... | |
space_sciences/13767_19.txt | , is the restricted band pass and poor spectral resolution, which makes it impossible to measure cluster temperatures.
In this paper, we present the analysis of a sample of31 galaxy clusters observed with ROSAT/PSPC, with theaim of characterizing the cluster emission at large radii andcomparing the results with three d... | |
space_sciences/15835_37.txt | ntered where the wind changesits direction and has the stronger wind shear, represented bythe dashed line. In the same figure we can see that none ofthe other months exhibit the downward diurnal modulationand only show variances increasing with height.
In Fig. 6, which shows meridional variances at Cariri, wecan see in... | |
space_sciences/01116_52.txt | S TO LEFT VIEWED FROMTOP IN ROTATION PLANEHZ COMPLETESA RIGHT HAND SYSTEM
TO INSERTION TIME (ONLY AT BANG = ZERO, OR PI)X0 INSERTION POSITION ALWAYSPOSITIVEY0 ALWAYSAT ZEROZ0 OUT OF PLANE COMPONENTAT INSERTION ALWAYSPOSITIVEPHASE0 INSERTION PHASE ZERO IF INSERT AT BANG = ZEROPI IF INSERT AT BANG = PIT = POSITION TIME | |
space_sciences/25968_119.txt | tive liquid/solid (?), i.e. the bound H2O, converted to a gas. While the magnitude of this has not been computed or measured in simulants, it is likely to be at least as large as the volume increase of water being converted to vapor, approximately a factor of 1700. Therefore, even if the surface bound H2O is only 0 | |
space_sciences/12302_6.txt | d, and operates the Kepler Science Data Pipeline, amajor analysis software component of the NASA Kepler Mission. The Science Operation Center’s charter is to design, develop, operate, and maintain a science data pipeline for use in analyzing photometric data from the Kepler spacecraft in support of the Mission’s search... | |
space_sciences/17419_79.txt | y of the data for some projects, e.g., power-spectral analysis of the ISM structure. 1l1e ditli::rent steps of this custom algorillun are described in the following subsections. Figure 2 illustrates the steps of the PACS data processing, especially the baseline subtraction, for one timeline corresponding to one bolomet... | |
space_sciences/09667_73.txt | h of our ACS "white-light" filter approximation datasets (1 9.3 and 19.1 mag arc~ec-~ respectively; see Table 3). As the 1998 epoch STIS data are significantly fainter than that measured in each bandpass of our ACS data, it is clear that no combination of the ACS data can reproduce the behavior of the STIS scattered li... | |
space_sciences/00350_126.txt | . Note that our extinction estimates include a few negative values(Figs. 8 and 9). While these values might suggest that our fiducial line needs to be loweredto bluer colors, that would imply a bias toward larger extinctions given the distribution ofstandard stars in the color-color plane. Therefore, we retain our orig... | |
space_sciences/14585_23.txt | 1000, Le., more than ~300 - 1000 observations within a 24 hr interval. By restricting our attention to long outbursts lying within these times of large nabs during the last 10 yr, and furthermore restricting the data to digital V -band photometry only (so as exclude the individual color biases inherent in the visual da... | |
space_sciences/03553_19.txt | , the 9.5 pm feature matched by GEMS, and a feature near 20 pm. We have, thus far, been unable to measure the 20 pm absorption of the GEMS in L2011*B2. This remains a high priority. A new FTIR facility, t8hatcan measure spectra from 2.5 to 200 pm, has been constructed at the NSLS. This should allow us to compare the fa... | |
space_sciences/09665_31.txt | A (10,000 K) doublets can be cleanly seen against the general disk continuum.
High time resolution, spatially-resolved asteroseismology will require broadband, near-UV or optical light (3,000- 10,000K) to provide sufficient signal to enable the resolution of internal structure and flows (modes to at least dcgrecs of o... | |
space_sciences/25826_40.txt | g of the study is that a potential TDAMM GOF differs significantly from mission GOFs.Mission GOFs exist to incentivize and support observers using NASA observatories. GOFs are activeduring the operations and sustainment phase of the NASA mission lifecycle. They implement communityengagement and proposal selection proce... | |
space_sciences/09603_165.txt | . Svalgaard, L.; Cliver, E.W.; and Yohsuke, K.: “Sunspot Cycle 24: Smallest Cycle in 100 Years?Report ADA434948, Air Force Research Lab, Hanscom AFB, Space Vehicles Directorate, MA, January 2023. Henson, B.; and Hosanskey, D.: Next Solar Max: Doozy or Dud? Last modified June 2008. UCAR Quarterly Online, Spring 2006 | |
space_sciences/21468_69.txt | e Zerodur mirror’s estimated inertial WFE meets the allocation defined in Figure 4. The most challenging allocation is primary tetrafoil with a 6.8 margin. Design refinements may reduce the PM’s contribution to this error. 5.3 Predicted Thermal WFE Stability Performance | |
space_sciences/13420_82.txt | mputers in the equipment room through Ilmltimode fiber-optic carriers. The signals
from each MCE are decoded by a PCI card from Astronomical Research Cameras, Inc. in each of the three data acquisition computers.s
The base clock rate of the MCE is 50 MHz. This is divided down to 100 clock cycles per detector row by 3... | |
space_sciences/16197_41.txt | yApollo 15 and Apollo 16 missions (Metzger et al. 1973). Thesedata provided the first insight into the chemical composition ofthe regolith. More recently, spatially resolved observations of the
nuclear emission lines by the Lunar Prospector (e.g., Lawrenceet al. 1998; Prettyman et al. 2006), Kaguya (Kobayashi et al.201... | |
space_sciences/12105_105.txt | l slightly favored HSE timing errors in which theforecast HSE occurs before the observed HSE.
[61] 1 computed forecast probabilities for both polarityreversals and HSEs within a 24 hour forecast window. Averaged over all data sets, a HSE forecast within the next24 hours will be correct 17% of the time. A forecast of no... | |
space_sciences/16214_63.txt | n the diffuse interstellar matter. The grain sizedistribution for the former is described in Woodet al. (2002), and that for the latter is similar toKim et al. (1994) (hereafter KMH; Whitney et al.2003a). The former affects the thermal balancein the disk via radiative transfer, and is successful in fitting the SED of t... | |
space_sciences/22566_80.txt | d be expected to be evanescent in the chromosphere. B. De Pontieu et al. (2004) showed that using an input spectrum of p-modes in a numerical simulation could reproduce model spicules with characteristics that closely matched spicules observed in an active region | |
space_sciences/14212_42.txt | dfor aperture effects but not for interstellar extinction.Magnitudes are presented in the AB system.
2.2. Suzaku
We observed V407 Cyg with Suzaku (Mitsuda et al.2006) as a target of opportunity between 2010 April9 21:32 UT and April 10 19:31 UT (sequence number905001010). Here we concentrate on the data obtainedwith th... | |
space_sciences/24811_47.txt | 9, 1.4, 2.8, 7.9, and 2.8 g/cm3 were used for the NaK, LD, MD, HD, and Intact families, respectively.
One important difference in ORDEM 3.1 interpolation, when compared to ORDEM 3.0, was the change in order of operations for interpolation and summation over the five ORDEM subpopulations. While ORDEM 3.0 summed the 5 | |
space_sciences/25807_363.txt | y (black traces in panels (b1), and (b2) of Figure A1).The exception is the SEP event early on November 14that produced >25 MeV proton intensity enhancements asobserved by SOHO/COSTEP/EPHIN but not by theother spacecraft (see Section 4.2 for details on the solar originof this event).
Appendix BEnergetic Electron Anisot... | |
space_sciences/16516_160.txt | s, but with a log [LX/LBOL] belowthe canonical value of −7. Whereas variations of log [LX/LBOL]amongst clusters are possible, the most probable cause for thislow value is an underestimate of the X-ray luminosities, due tothe high interstellar absorption of the cluster, which reduces thesignal-to-noise ratio at low ener... | |
space_sciences/14183_217.txt | troduction, we discussed HCGs as apotentially special environment in terms of galaxyevolution. The apparent duality of ‘modes’ inwhich HCG galaxies are found – either starforming or quiescent – and the evident lack of anintermediate stage population are in accord withthe mid-IR color-space ‘gap’ discussed in our previo... | |
space_sciences/24376_124.txt | eaverage path length in the atmosphere, which diminishes theblueness due to Rayleigh scattering. This explains why the“clear skies with a 100% ocean surface” end-member is bluerthan all the other Earth spectra, although the ocean surfaceitself also contributes to the blueness (Crow et al. 2011). Theposition of the clea... | |
space_sciences/11840_34.txt | .30 This is in addition to the more ‘natural’ applications to chemical and biological systems.31
Motivated in part by recent data32 in which SEP characteristics appear to show patterns that are difficult to explain phenomenologically, this Technical Publication (TP) explores the effects of a specific form of coupling—v... | |
space_sciences/09380_183.txt | O1 sample with morphological types T > 2 (Sa-Irr Hubble types).
The SO1 sample covers ranges of LB and M, that are wellmatched to our main sample and are representative of latetype galaxies in the local universe. In order to compute mean X-ray luminosities for samples that were directly comparable with our results, we... | |
space_sciences/12022_17.txt | a small peak at 286.7 occurring in some areas of the sample. There is another
strong absorption at 288.4 eV with small energy shifts occurring around this energy in some of the spectra.
Discussion: Though morphologically similar, FC3,0,2,4,4 and C2054,0,35,100,5 are chemically different. Neither the initial or later s... | |
space_sciences/01287_6.txt | n asteroidal objectwhereas the cometary nature of the object was noted by Durig et al. (1999) a few days later. Theclose perihelion distance (0.77 AU) of the orbit and the prediction of a likely naked-eye visibility inJuly 2000 (Green 1999a, 1999b) attracted attention to this comet. As a result, it was monitored bydiff... | |
space_sciences/18635_30.txt | d UVOT are coaligned to allow for simultaneous multiwavelength followup of GRBs detected onboard. To identify the counterpart in the simultaneous UVOT images, we overplotted a contour map of each XRT source onto the coaligned UVOT image, and selected the counterpart visually. Once a counterpart is selected, we use the ... | |
space_sciences/19938_293.txt | n, S. J., Harding, L. B., Ruscic, B., et al. 2009, J.Phys. Chem. A, 113, 10241Knyazev, V. D., & Slagle, I. R. 2001, J. Phys. Chem. A, 105, 3196Konnov, A. A., & De Ruyck, J. 2000, Combust. Sci. and | |
space_sciences/25526_136.txt | C survey using theLUVOIR-B-like scenario detailed in Stark et al. (2019).Briefly, this consists of a 6.7 m inscribed diameter telescopewith parallel UV and visible wavelength coronagraph channelsusing deformable mirror-assisted vortex charge 6 coronagraphs. We make identical astrophysical, mission, and surveyassumption... | |
space_sciences/22933_123.txt | 6 m/s total mission 'V using 3 thruster strings operating at 26.6 kW. A return transfer back to the NRHO is assumed to require similar propellant mass, 'V and trip time.
Though assumed to be representative, the presented trajectory is a single point case. Transfers with differing epochs and planetary alignment may resu... | |
space_sciences/14761_34.txt | n would require χ2i,99% > 31.2 on4 degrees of freedom. While we detect no statistically significant variations at 99%-confidence, wenote that the 3 most significant variations occur at bright locations on the inner ring.
Other effects, such as changes in the roll angle of the read-out streak, can lead to possiblyspurio... | |
space_sciences/11182_115.txt | t sickness levels for UG and FW are shown in Fig. 18 as acute radiation risk level. It shows that a male astronaut may not have any symptoms during the 3-hour EVA, however the initial ARR symptoms appear after he finds shelter. These symptoms include upset stomach, clammy and sweaty skin, and mouth watering (level 2 of... | |
space_sciences/22692_48.txt | g particleand the nucleus of a lattice atom subsequently displaces the atom from its original lattice position.
The particles producing displacement damage include protons of all energies, electrons with energies above150 keV, and neutrons (e.g., from onboard power sources). Shielding has some effect, but it depends on... | |
space_sciences/11351_599.txt | f the refereed journal, Space Science Reviews (Gardner et al. 2006). It has since also updated and extended the science case in a series of white papers that include astrobiol NASA engineers check out the unwrapped ISIM structure in the Goddard clean room. The ISIM Structure supports and holds four Webb telescope scien... | |
space_sciences/13892_57.txt | . The choice of particle physics annihilation model merely scales all satellites by the same constant factor.
1 serves as a guide for evaluating the of low-mass satellites. 'While the total number of satellites increases with decreasing mass. the J-factors of these low-mass satellites tend to decrease. This means that... | |
space_sciences/02005_101.txt | 5 SNss and 1998 TF3s. InMPEC 1999-L25.
Danzl, N. 1999. Discovery of Trans-Neptunian Object 1998 SM165. In MPEC 1999-M31.
Danzl, N., J. L. Montani, J. V. Scotti. 1999. Discovery of Apollo Asteroid 1999 TT16. InMPEC 1999-U02. | |
space_sciences/17419_176.txt | w map was reconstructed and the procedure was repeated for I 00 iterations.
Om destripi.ng routine also i11cluded the detection of jumps in bolometer timelines and a second level deglitching. Jumps u1 bolometer ti.melines were sinlllar to PACS long glitches (see Section 3.6 ), but in SPIRE they aJiected one bolometer ... | |
space_sciences/16946_103.txt | Dsize ratio of ∼0.2, albeit with significant scatter (see Figure 6).The median size ratio shows little dependence on star-formationactivity or mass, over the range probed by our sample. Giventhe enhanced B/T values in QGs, and the fact that bulgeshave smaller half-mass radii than disks, one might wonder ifthe differenc... | |
space_sciences/14781_41.txt | k – potentially ‘forever’ preventing the new technology or approach from being selected for a flight mission. Many technologies find themselves at this critical juncture, known as the TRL Valley of Death, because they are too advanced for further ground-based research and development, yet have been insufficiently prove... | |
space_sciences/01962_21.txt | y, and P.Thaddeus, 2001, Journal of Chemical Physics, submitted.
."Microwave and Laser Spectroscopy of CarbonChains and Rings," MichaelC. McCarthy and Patrick Thaddeus, 2001, Chemical Society Reviews, 30,177-185. | |
space_sciences/04282_83.txt |
The HRMA Effective Area is one of the most important parameters of the Chandra X-ray Observatory. It has been calibrated to an unprecedented precision for any X-ray telescope, to ensure an accurate measurement of the flux from X-ray sources. This paper summarizes all the measurements conducted at the MSFC/XRCF during ... | |
space_sciences/03918_66.txt | 6~10~' erg s-l consistent with a black hole mass of 45 MG.
In the Madau (1988) model, part of the radiation is scattered and enhances the surface brightness of the funnel walls and part of the radiation is absorbed by the funnel walls; only a small fraction of the intrinsically radiated luminosity is being captured by... |
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