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排序方式: 共有226条查询结果,搜索用时 31 毫秒
171.
Silvia Martínez-Núñez Peter Kretschmar Enrico Bozzo Lidia M. Oskinova Joachim Puls Lara Sidoli Jon Olof Sundqvist Pere Blay Maurizio Falanga Felix Fürst Angel Gímenez-García Ingo Kreykenbohm Matthias Kühnel Andreas Sander José Miguel Torrejón Jörn Wilms 《Space Science Reviews》2017,212(1-2):59-150
Massive stars, at least \(\sim10\) times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy.In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution.Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations.This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems. 相似文献
172.
H. Kunow W. Dröge B. Heber R. Müller-Mellin K. Röhrs H. Sierks G. Wibberenz R. Ducros P. Ferrando C. Rastoin A. Raviart C. Paizis 《Space Science Reviews》1995,72(1-2):397-402
Since June 1992 the Kiel Electron Telescope on board ULYSSES measures 26-day variations of the order of 6% in the fluxes of high energy H and He. In May 1993 ULYSSES entered into the unipolar region of the southern polar coronal hole, but continued to observe similar effects: increases in the MeV proton channels due to acceleration near the shocks of the corotating interaction region and decreases in the intensity of galactic nuclei associated with the same region. Amplitude variations are presented for different magnetic rigidities and the effects are discussed in view of corotating shock development in a 3-dimensional heliospheric structure. 相似文献
173.
Helmut Lammer Eric Chassefière Özgür Karatekin Achim Morschhauser Paul B. Niles Olivier Mousis Petra Odert Ute V. Möstl Doris Breuer Véronique Dehant Matthias Grott Hannes Gröller Ernst Hauber Lê Binh San Pham 《Space Science Reviews》2013,174(1-4):113-154
The evolution and escape of the martian atmosphere and the planet’s water inventory can be separated into an early and late evolutionary epoch. The first epoch started from the planet’s origin and lasted ~500 Myr. Because of the high EUV flux of the young Sun and Mars’ low gravity it was accompanied by hydrodynamic blow-off of hydrogen and strong thermal escape rates of dragged heavier species such as O and C atoms. After the main part of the protoatmosphere was lost, impact-related volatiles and mantle outgassing may have resulted in accumulation of a secondary CO2 atmosphere of a few tens to a few hundred mbar around ~4–4.3 Gyr ago. The evolution of the atmospheric surface pressure and water inventory of such a secondary atmosphere during the second epoch which lasted from the end of the Noachian until today was most likely determined by a complex interplay of various nonthermal atmospheric escape processes, impacts, carbonate precipitation, and serpentinization during the Hesperian and Amazonian epochs which led to the present day surface pressure. 相似文献
174.
Boynton W.V. Feldman W.C. Mitrofanov I.G. Evans L.G. Reedy R.C. Squyres S.W. Starr R. Trombka J.I. d'Uston C. Arnold J.R. Englert P.A.J. Metzger A.E. Wänke H. Brückner J. Drake D.M. Shinohara C. Fellows C. Hamara D.K. Harshman K. Kerry K. Turner C. Ward M. Barthe H. Fuller K.R. Storms S.A. Thornton G.W. Longmire J.L. Litvak M.L. Ton'chev A.K. 《Space Science Reviews》2004,110(1-2):37-83
The Mars Odyssey Gamma-Ray Spectrometer is a suite of three different instruments, a gamma subsystem (GS), a neutron spectrometer, and a high-energy neutron detector, working together to collect data that will permit the mapping of elemental concentrations on the surface of Mars. The instruments are complimentary in that the neutron instruments have greater sensitivity to low amounts of hydrogen, but their signals saturate as the hydrogen content gets high. The hydrogen signal in the GS, on the other hand, does not saturate at high hydrogen contents and is sensitive to small differences in hydrogen content even when hydrogen is very abundant. The hydrogen signal in the neutron instruments and the GS have a different dependence on depth, and thus by combining both data sets we can infer not only the amount of hydrogen, but constrain its distribution with depth. In addition to hydrogen, the GS determines the abundances of several other elements. The instruments, the basis of the technique, and the data processing requirements are described as are some expected applications of the data to scientific problems. 相似文献
175.
S. Patsourakos J.-C. Vial J.-R. Gabryl S. Koutchmy U. Schühle 《Space Science Reviews》1999,87(1-2):291-294
Polar coronal holes represent the most convincing site from which the high-speed solar wind originates. Here we report high-accuracy Doppler shifts measured in the O VI (1037.6 Å) line obtained by SUMER on SOHO inside an interplume region within the south polar coronal hole. We infer limits on the outflow velocity and draw hints about the flow geometry. 相似文献
176.
Cosmic Ray Induced Ion Production in the Atmosphere 总被引:1,自引:0,他引:1
G. A. Bazilevskaya I. G. Usoskin E. O. Flückiger R. G. Harrison L. Desorgher R. Bütikofer M. B. Krainev V. S. Makhmutov Y. I. Stozhkov A. K. Svirzhevskaya N. S. Svirzhevsky G. A. Kovaltsov 《Space Science Reviews》2008,137(1-4):149-173
An overview is presented of basic results and recent developments in the field of cosmic ray induced ionisation in the atmosphere, including a general introduction to the mechanism of cosmic ray induced ion production. We summarize the results of direct and indirect measurements of the atmospheric ionisation with special emphasis to long-term variations. Models describing the ion production in the atmosphere are also overviewed together with detailed results of the full Monte-Carlo simulation of a cosmic ray induced atmospheric cascade. Finally, conclusions are drawn on the present state and further perspectives of measuring and modeling cosmic ray induced ionisation in the terrestrial atmosphere. 相似文献
177.
Tilman Spohn Karsten Seiferlin Axel Hagermann Jörg Knollenberg Andrew J. Ball Marek Banaszkiewicz Johannes Benkhoff Stanislaw Gadomski Wojciech Gregorczyk Jerzy Grygorczuk Marek Hlond Günter Kargl Ekkehard Kührt Norbert Kömle Jacek Krasowski Wojciech Marczewski John C. Zarnecki 《Space Science Reviews》2007,128(1-4):339-362
MUPUS, the multi purpose sensor package onboard the Rosetta lander Philae, will measure the energy balance and the physical parameters in the near-surface layers – up to about 30 cm depth- of the
nucleus of Rosetta’s target comet Churyumov-Gerasimenko. Moreover it will monitor changes in these parameters over time as
the comet approaches the sun. Among the parameters studied are the density, the porosity, cohesion, the thermal diffusivity
and conductivity, and temperature. The data should increase our knowledge of how comets work, and how the coma gases form.
The data may also be used to constrain the microstructure of the nucleus material. Changes with time of physical properties
will reveal timescales and possibly the nature of processes that modify the material close to the surface. Thereby, the data
will indicate how pristine cometary matter sampled and analysed by other experiments on Philae really is. 相似文献
178.
We have observed the X-ray burst sources 4U1728-33 and 4U1813-14 with the ME detectors aboard EXOSAT, and present here results of a spectral analysis of their persistent emissions. For both sources the data can be well fitted by a double blackbody continuum and a Gaussian emission line. The two spectral components can be interpreted in terms of a blackbody radiation from the neutron star, and emission from the inner part of an accretion disc. The line feature is consistent with the 6.7 keV iron emission line expected in the presence of a hot extended object (X-ray corona) around the neutron star. 相似文献
179.
B2-RuAl合金中原子扩散的第一原理计算 总被引:1,自引:0,他引:1
采用第一原理赝势平面波方法,计算B2-RuA l合金中Ru和A l在不同情况下的扩散,用扩散激活能有效地表述和研究其化学反应的难易。计算发现:在空位扩散时,A l原子要比Ru原子容易扩散,即Ru原子比A l原子更稳定一些;当考虑不同扩散浓度和周边原子影响的情况时,也是A l原子要比Ru原子容易扩散,但其扩散激活能不同,所以在对B2-RuA l合金的原子扩散能计算时,周边的原子影响较大,我们应该考虑模型的尺寸效应。而比较不同扩散浓度下的扩散激活能,高浓度的扩散要难于低浓度。 相似文献
180.