Download Microquasars: Proceedings of the Third Microquasar Workshop by Josep Martí (auth.), A. J. Castro-Tirado, J. Greiner, J. M. PDF

By Josep Martí (auth.), A. J. Castro-Tirado, J. Greiner, J. M. Paredes (eds.)

The 3rd Microquasar Workshop (or the 'Fifth' Workshop on Galactic Relativ­ istic Jet Sources), used to be held in Granada, Andalucia (Spain) on 11-13 September 2000. the purpose of this workshop in Granada, following the former Microquasar Workshops in Greenbelt (1997) and Paris (1998) and the Workshops on galactic resources with relativistic jets in Jodrell financial institution (1996) and Milton Keynes (1998), was once to target the theoretical and observational points of microquasars. The research of microquasars, the assets in our Galaxy exhibiting robust re­ lativistic jets, is a quickly advancing box in astrophysics. the recent instrumentation on floor (MERLIN, SCUBA, VLA, VLT) and aboard satellites (ASCA, BSAX, ISO, IXAE and RXTE) has supplied vital effects, and masses extra is predicted to return from Chandra and XMM-Newton. within the extra destiny, strong instru­ mentation will come on-line within the sub-mm (ALMA) and gamma-rays (INTEG­ RAL), extending our assurance to special areas for the examine of microquasars. strength shipping through relativistic jets is among the most crucial actual mechan­ isms happening in compact items. huge efforts were dedicated to correctly comprehend the disk-jet connection, or even the results of rotation or magnetic fields. a number of new vital advances were made lately, either from the perspective of the theoretical remedy of jets and the various new observational tests.

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Extra info for Microquasars: Proceedings of the Third Microquasar Workshop Granada Workshop on Galactic Relativistic Jet Sources Granada, Spain, 11–13 September 2000

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15-18, 200!. © 2001 Kluwer Academic Publishers. 16 M. FERoeI ET AL. modes of variations have been classified by Belloni et al. (2000). g. Greiner et al. 1996), both in flux and spectrum, has been interpreted by Belloni et al. (1997a) in terms of abrupt emptying of the inner portion of an accretion disk around a black hole, followed by a refilling phase. In this contribution we present the results of a recent observation of GRS 1915+ 105 performed with three of the Narrow Field Instruments (LECS, MECS and PDS) on board the Italian-Dutch X-ray satellite BeppoSAX .

G. , 2000). The optical light in X-ray bright LMXBs is dominated by reprocessing: the optical emission from viscous dissipation is smaller by a factor of '" 10- 3 . , 2000) . 2. The Mechanism Powering LMXB Superhumps Recently, eclipse mapping of V348 Pup, a superhumping CV, revealed clear evidence that the spatial distribution of the disc emission is modulated on Psh (Rolfe, Haswell and Patterson, 2000). , 2000). Figure 1 shows a '" 10% modulation in the area of the disc. This will clearly modulate Lopr.

Introduction Superhumps are a periodic photometric modulation with period Psh slightly longer than Porb' They were discovered in extreme mass-ratio cataclysmic variables (CVs) harbouring eccentric accretion discs performing apsidal precession (Warner, 1995). CV superhumps are powered by tidally-driven modulations in viscous dissipation (Murray, 2000). g. , 2000). The optical light in X-ray bright LMXBs is dominated by reprocessing: the optical emission from viscous dissipation is smaller by a factor of '" 10- 3 .

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