Monitoring Flaring State in the Black Hole X-Ray Binary/Microquasars GRS 1915+105 and Cyg X-3: Radio Timing with the Korean VLBI Network

Details Monitoring Flaring State in the Black Hole X-Ray Binary/Microquasars GRS 1915+105 and Cyg X-3: Radio Timing with the Korean VLBI Network Monitoring Flaring State in the Black Hole X-Ray Binary/Microquasars GRS 1915+105 and Cyg X-3: Radio Timing with the Korean VLBI Network

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..714..160k&link_type=abstract

X-RAY TIMING 2003: Rossie and Beyond. AIP Conference Proceedings, Volume 714, pp. 160-166 (2004).

Astronomy and Astrophysics

Astronomy

1

Black Holes, Intergalactic Matter, Quasar Absorption And Emission-Line Systems, Lyman Forest, X-Ray, X- And Gamma-Ray Telescopes And Instrumentation, Jets And Bursts, Galactic Winds And Fountains

Scientific paper

Microquasars, nearby stellar-scale analogy of quasars, are producing jets at speeds very close to the speed of light up to 0.98 c. Microquasars are also accreting transient or persistent X-ray binaries. For a decade since its discovery, the phenomena of microquasars have had a great deal of attention. The observation of transient flares and accompanied jet phenomena is one of the highlights in the fields of X-ray, radio and, very recently, infrared astronomy. The recent observations have indicated that the superluminal jets probably are the common nature of the black hole X-ray binaries and, in part, of the neutron star binary sources. The recent development in observational techniques has made it possible to study detailed feature of jet phenomena. In the radio the very long baseline interferometry (VLBI) is required to map images of jets. The first Korean VLBI Network (KVN), recently proposed for the mm-wave multi-channel receiver system of 2.5, 8.5, 23, 43, 86-129 GHz, therefore, can be a promising tool of probing the nature of microquasars. In this paper, we present the strategy of observing microquasar phenomena with radio telescopes in Korea, including KVN, and international collaboration with Japanese VLBI system, VERA. Monitoring program for microquasars with 6-14-21 m array is also presented. As an example radio timing of frequently flaring, radio-bright microquasars such as GRS 1915+105 and Cyg X-3 are discussed.

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