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121.
122.
M. van der Klis 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2646-2656
Millisecond X-ray time variability studies of accreting low-magnetic-field neutron stars and stellar-mass black holes in X-ray binaries probe the motion of matter in regions of strong gravity. In these regions, general relativity (GR) is no longer a small correction to the classical laws of motion, but instead dominates the dynamics: we are studying motion in strongly curved spacetime. Such millisecond X-ray variability studies can therefore provide unique tests of GR in the strong-field regime. The same studies also constrain neutron-star parameters such as stellar mass and radius, and thereby the equation of state (EOS) of ultradense matter. I briefly review the status, and discuss the prospects for mapping out space-time near accreting stellar-mass compact objects, and measuring the EOS of dense matter, through millisecond timing, particularly with an eye towards future missions. The overwhelming consideration for timing sensitivity is collecting area: contrary to most applications, the signal-to-noise ratio for the aperiodic timing phenomena produced by accretion flows increases proportionally with count rate rather than as the square root of it. A 10 times larger instrument turns 1σ effects into 10σ effects (or does as well in 1% of the time). With the Rossi X-ray Timing Explorer (RXTE), using 0.6 m2 collecting area, we have found several timing diagnostics from the accretion flow in the strong field region around neutron stars and black holes, as well as signals from neutron star surface hot spots. Combined work between RXTE and the new sensitive X-ray spectrographs onboard Chandra and XMM can already begin to clinch the geometry and physical mechanisms underlying these signals. Future instruments, larger in area by an order of magnitude and in some cases with enhanced spectral capabilities, are expected to turn these diagnostics of GR into true tests of GR. They are also expected to put strong constraints on neutron-star structure, and thereby on the EOS of supranuclear density matter. 相似文献
123.
J. Kleczek H. Nussbaumer K. A. van der Hucht J. P. de Greve G. Ooms R. J. Rutten H. van der Laan F. W. Jäger G. C. M. Reijnen w. Bijleveld J. Kistemaker C. de Jager E. R. Mustel Y. Ne'eman E. R. Priest H. Stiller W. Seifert O. Namba M. Kuperus Roel Hoekstra F. L. H. M. Stumpers S. Frank J. T. F. Zimmerman C. de Loore R. Gendrin J. Schrijver P. S. Mulder K. A. Pounds R. S. Young L. Houziaux O. Engvold B. J. Bok W. de Graaff 《Space Science Reviews》1983,36(4):415-432
124.
O. Ooms Hans Van Der Woerd Henny J. G. L. M. Lamers Josip Kleczek J. Kovalevsky R. Gathier T. Jarzebowski J. P. Swings K. A. van der Hucht O. Namba R. Mewe D. Lynden-Bell Jan Kuijpers M. van der Klis D. de Hoop H. Wittenberg W. Iwanowska P. S. Thé J. Schrijver S. R. Pottasch 《Space Science Reviews》1984,38(3-4):385-387
125.
Medium energy neutral atom (MENA) imager for the IMAGE mission 总被引:1,自引:0,他引:1
Pollock C.J. Asamura K. Baldonado J. Balkey M.M. Barker P. Burch J.L. Korpela E.J. Cravens J. Dirks G. Fok M.-C. Funsten H.O. Grande M. Gruntman M. Hanley J. Jahn J.-M. Jenkins M. Lampton M. Marckwordt M. McComas D.J. Mukai T. Penegor G. Pope S. Ritzau S. Schattenburg M.L. Scime E. Skoug R. Spurgeon W. Stecklein T. Storms S. Urdiales C. Valek P. van Beek J.T.M. Weidner S.E. Wüest M. Young M.K. Zinsmeyer C. 《Space Science Reviews》2000,91(1-2):113-154
The Medium Energy Neutral Atom (MENA) imager was developed in response to the Imaging from the Magnetopause to the Aurora for Global Exploration (IMAGE) requirement to produce images of energetic neutral atoms (ENAs) in the energy range from 1 to 30 keV. These images will be used to infer characteristics of magnetospheric ion distributions. The MENA imager is a slit camera that images incident ENAs in the polar angle (based on a conventional spherical coordinate system defined by the spacecraft spin axis) and utilizes the spacecraft spin to image in azimuth. The speed of incident ENAs is determined by measuring the time-of-flight (TOF) from the entrance aperture to the detector. A carbon foil in the entrance aperture yields secondary electrons, which are imaged using a position-sensitive Start detector segment. This provides both the one-dimensional (1D) position at which the ENA passed through the aperture and a Start time for the TOF system. Impact of the incident ENA on the 1D position-sensitive Stop detector segment provides both a Stop-timing signal and the location that the ENA impacts the detector. The ENA incident polar angle is derived from the measured Stop and Start positions. Species identification (H vs. O) is based on variation in secondary electron yield with mass for a fixed ENA speed. The MENA imager is designed to produce images with 8°×4° angular resolution over a field of view 140°×360°, over an energy range from 1 keV to 30 keV. Thus, the MENA imager is well suited to conduct measurements relevant to the Earth's ring current, plasma sheet, and (at times) magnetosheath and cusp. 相似文献
126.
We investigate links between the observational environment as experienced by the Hipparcos satellite and the performance of
the spacecraft and payload instrumentation, with particular emphasis on finding out whether some of these effects may have
been inadequately represented in instrument calibrations and could thus have affected the scientific results of the mission.
Scan-coverage and radiation effects are primarily random effects with only some long-term systematics. However, long- (days
to weeks) and short-term (hours) temperature variations reflected in the performance of some of the spacecraft instrumentation.
It is shown that only a small sign of some long-term thermal variations could be detected in the payload instrumentation.
These findings further limit the scope left for the occurrence of large-scale correlated errors in the Hipparcos astrometric
data. On the other hand, a number of great circles were identified which showed a highly significant drift of the basic angle,
which had not been detected in the preparation of the published data. The data from these circles may have, in some cases,
led to, very localised, slightly anomalous results, in particular where stars are accidentally affected by two or more of
such circles.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
127.
K.D. Moloto N.E. Engelbrecht R.D. Strauss D.M. Moeketsi J.P. van den Berg 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2019,63(1):626-639
Three-dimensional studies of the transport and modulation of cosmic ray particles in turbulent astrospheres require large-scale simulations using specialized scientific codes. Essentially, a multi-dimensional Fokker-Planck type equation (a parabolic diffusion equation) must be integrated numerically. One such approach is to convert the relevant transport equation into a set of stochastic differential equations (SDEs), with the latter much easier to handle numerically. Due to the growing demand for high performance computing resources, research into the application of effective and suitable numerical algorithms to solve such equations is needed. We present a case study of the performance of a custom-written FORTRAN SDE numerical solver on the CHPC (Centre for High Performance Computing) Lengau cluster in South Africa for a realistic test problem with different set-ups. It is shown that SDE codes can scale very well on large parallel computing platforms. Finally, we consider an extremely computationally expensive application of the SDE approach to cosmic ray modulation, studying the behaviour of galactic cosmic ray proton latitude gradients and relative amplitudes in a physics-first manner. This is done using a modulation code that employs diffusion coefficients derived from first principles, which in turn are functions of turbulence quantities in reasonable agreement with spacecraft observations and modelled using a two-component turbulence transport model (TTM). We show that this approach leads to reduced latitude gradients qualitatively in line with spacecraft observations of the same, without making ad hoc assumptions as to anisotropic perpendicular diffusion coefficients as are often made in many cosmic ray modulation studies. 相似文献
128.
Peter R. Young Hui Tian Hardi Peter Robert J. Rutten Chris J. Nelson Zhenghua Huang Brigitte Schmieder Gregal J. M. Vissers Shin Toriumi Luc H. M. Rouppe van der Voort Maria S. Madjarska Sanja Danilovic Arkadiusz Berlicki L. P. Chitta Mark C. M. Cheung Chad Madsen Kevin P. Reardon Yukio Katsukawa Petr Heinzel 《Space Science Reviews》2018,214(8):120
The term “ultraviolet (UV) burst” is introduced to describe small, intense, transient brightenings in ultraviolet images of solar active regions. We inventorize their properties and provide a definition based on image sequences in transition-region lines. Coronal signatures are rare, and most bursts are associated with small-scale, canceling opposite-polarity fields in the photosphere that occur in emerging flux regions, moving magnetic features in sunspot moats, and sunspot light bridges. We also compare UV bursts with similar transition-region phenomena found previously in solar ultraviolet spectrometry and with similar phenomena at optical wavelengths, in particular Ellerman bombs. Akin to the latter, UV bursts are probably small-scale magnetic reconnection events occurring in the low atmosphere, at photospheric and/or chromospheric heights. Their intense emission in lines with optically thin formation gives unique diagnostic opportunities for studying the physics of magnetic reconnection in the low solar atmosphere. This paper is a review report from an International Space Science Institute team that met in 2016–2017. 相似文献
129.
L. van Driel-Gesztelyi C.P. Goff P. Démoulin J.L. Culhane S.A. Matthews L.K. Harra C.H. Mandrini K.-L. Klein H. Kurokawa 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, and radio observations from Culgoora and Wind/ WAVES to understand the complex development of this event. We reach three main conclusions. First, we link the first two impulsive flares to tether-cutting reconnections and the launch of the CME. This complex observation shows that impulsive quadrupolar flares can be eruptive. Second, we relate the last of the flares, an LDE, to the relaxation phase following forced reconnections between the erupting flux rope and neighbouring magnetic field lines, when reconnection reverses and restores some of the pre-eruption magnetic connectivities. Finally, we show that reconnection with the magnetic structure of a previous CME launched about 8 h earlier injects electrons into open field lines having a local dip and apex (located at about six solar radii height). This is observed as an N-burst at decametre radio wavelengths. The dipped shape of these field lines is due to large-scale magnetic reconnection between expanding magnetic loops and open field lines of a neighbouring streamer. This particular situation explains why this is the first N-burst ever observed at long radio wavelengths. 相似文献
130.
Xavier Collilieux Zuheir Altamimi David Coulot Tonie van Dam Jim Ray 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
The International Terrestrial Reference Frame (ITRF), as a realization of the International Terrestrial Reference System (ITRS), is represented by a set of station positions and linear velocities. They are intended to be used as regularized coordinates to which some corrections should be added to access instantaneous coordinates. The latest ITRS realization is the ITRF2005, which has integrated time series of station positions to form long-term solutions for the four space geodetic techniques. Currently, a purely linear model is used to parameterize station displacements in the estimation process, plus occasional discontinuities in case of earthquakes or equipment changes. However the input data have been derived without applying surface loading models and so surface loading effects are supposed to be embedded in the coordinates as measured quantities. We evaluate the effect of applying a posteriori loading corrections, which include the effect of atmospheric, non-tidal ocean, and continental water loading, to time series of positions estimated from Satellite Laser Ranging (SLR), Very Long Baseline Interferometry (VLBI), and Global Positioning System (GPS) data. We notice that they reduce about 50% or more of the annual signals in the translation and scale parameter time series of the SLR and VLBI techniques, except in SLR Z translation. In general, the estimated secular frame definition is negligibly affected and estimated positions and velocities are not significantly modified for stations that have accumulated a large number of observations. A multi-technique combination of such derived frames allows concluding that, for some cases, loading model corrections might degrade co-located station coordinates almost as much as they benefit them. However, most significant improvement of the estimated secular coordinates is observed for stations with less than 100 estimated positions as demonstrated with a multi-technique combination. 相似文献