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Titlebook: Microquasars; Proceedings of the T A. J. Castro-Tirado,J. Greiner,J. M. Paredes Conference proceedings 2001 Springer Science+Business Media

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發(fā)表于 2025-3-21 17:28:14 | 只看該作者 |倒序瀏覽 |閱讀模式
書目名稱Microquasars
副標(biāo)題Proceedings of the T
編輯A. J. Castro-Tirado,J. Greiner,J. M. Paredes
視頻videohttp://file.papertrans.cn/634/633414/633414.mp4
圖書封面Titlebook: Microquasars; Proceedings of the T A. J. Castro-Tirado,J. Greiner,J. M. Paredes Conference proceedings 2001 Springer Science+Business Media
描述The Third Microquasar Workshop (or the ‘Fifth‘ Workshop on Galactic Relativ- istic Jet Sources), was held in Granada, Andalucia (Spain) on 11-13 September 2000. The aim of this workshop in Granada, following the previous Microquasar Workshops in Greenbelt (1997) and Paris (1998) and the Workshops on galactic sources with relativistic jets in Jodrell Bank (1996) and Milton Keynes (1998), was to focus on the theoretical and observational aspects of microquasars. The study of microquasars, the sources in our Galaxy displaying powerful re- lativistic jets, is a rapidly advancing field in astrophysics. The new instrumentation on ground (MERLIN, SCUBA, VLA, VLT) and aboard satellites (ASCA, BSAX, ISO, IXAE and RXTE) has provided important results, and much more is expected to come from Chandra and XMM-Newton. In the further future, powerful instru- mentation will come online in the sub-mm (ALMA) and gamma-rays (INTEG- RAL), extending our coverage to important regions for the study of microquasars. Energy transport via relativistic jets is one of the most important physical mechan- isms taking place in compact objects. Large efforts have been devoted to properly understand the disk-jet co
出版日期Conference proceedings 2001
關(guān)鍵詞Accretion; Galaxy; Quasar; astrophysics; relativistic jet; star
版次1
doihttps://doi.org/10.1007/978-94-010-0700-9
isbn_softcover978-94-010-3828-7
isbn_ebook978-94-010-0700-9
copyrightSpringer Science+Business Media New York 2001
The information of publication is updating

書目名稱Microquasars影響因子(影響力)




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發(fā)表于 2025-3-21 20:21:04 | 只看該作者
https://doi.org/10.1007/978-94-010-0700-9Accretion; Galaxy; Quasar; astrophysics; relativistic jet; star
板凳
發(fā)表于 2025-3-22 02:12:42 | 只看該作者
地板
發(fā)表于 2025-3-22 08:06:55 | 只看該作者
Observations of GRS 1915+105 from the USA Experiment on ArgosWe present first results from a monitoring campaign of GRS 1915+105 undertaken with the USA X-ray timing experiment on the ARGOS satellite. A variety of behaviour has been observed, ranging from low, steady X-ray emission to rapid quasi-periodic flaring on timescales of approximately 10–120 seconds.
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發(fā)表于 2025-3-22 11:18:55 | 只看該作者
Identification of the Donor in GRS 1915+105We report on medium-resolution H and K band spectroscopy of GRS 1915+ 105 using the 8m VLT at ESO. We clearly identify absorption bandheads from .CO/.CO. Together with other features we classify the donor as a K-M III star.
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發(fā)表于 2025-3-22 13:36:32 | 只看該作者
On the Mass-Donating Star in GRS 1915+105Geometric constraints and the lack of eclipses in GRS 1915+105 are used to place limits on the mass of the companion star. We rule out any companion with .. > 19.4.. for a black hole mass of .. ? 30..
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發(fā)表于 2025-3-22 18:09:48 | 只看該作者
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發(fā)表于 2025-3-23 00:53:56 | 只看該作者
XTE J1550–564: A Superluminal Ejection During the September 1998 OutburstIn 1998 September, the X-ray transient XTE J155072–564 underwent a major outburst in soft and hard X-rays, followed by a radio flare. Australian Long Baseline Array images obtained shortly after the peak in the radio flare showed evolving structure. The components observed have an apparent separation velocity of > 2..
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發(fā)表于 2025-3-23 02:47:02 | 只看該作者
Optical Behaviour of XTE J1550–564 and XTE J1859+226 from Outburst to QuiescenceWe present here the optical light curves of the Soft X-ray Transients XTE J1550–564 and XTEJ1859+226 from outburst to quiescence
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發(fā)表于 2025-3-23 08:00:12 | 只看該作者
Minioutbursts in XTE J1859+226Photometry of the X-ray transient XTE J1859+226, obtained during outburst, showed at least 3 minioutbursts. During the second one, the source exhibited a 0.3 mag modulation with QPO flaring activity during the minimum.
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