Relativistic superluminal radio jets in microquasars in our galaxy
| dc.creator | Yadav, J S | |
| dc.date | 2006-12-04 | |
| dc.date | 2006-12-05 | |
| dc.date.accessioned | 2026-07-07T10:21:08Z | |
| dc.date.available | 2026-07-07T10:21:08Z | |
| dc.description | We discuss the origin of superluminal radio jets in Black hole X-ray binaries with relativistic radio jets in our Galaxy popularly known as microquasars. We classify the relativistic superluminal jet according to the radio emission in black hole X-ray binaries (transient or persistent) rather than the mass of the companion. The black hole X-ray binaries with transient radio emission (mostly LMXBs) produce superluminal jets with $β_{app} >$ 1 when the accretion rate, $\dot{m}_{accr}$ is high and the bolometric luminosity L$_{bol}$ approaches the Eddington Luminosity, L$_{Edd}$. On the other hand, the black hole X-ray binaries with persistent radio emission (mostly HMXBs) produce superluminal jets with $β_{app} <$ 1 at relatively low $\dot{m}_{accr}$. We specially discuss the case of V4641 Sgr, a HMXB with transient radio emission which produces superluminal radio jets like in LMXBs. | |
| dc.description | 6 pages, 2 figures,VI Microquasar Workshop: Microquasars and Beyond, September 18-22, 2006, Como, Italy | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0612070 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0612070 | |
| dc.identifier | PoSMQW6:101,2006 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/175074 | |
| dc.subject | Astrophysics | |
| dc.title | Relativistic superluminal radio jets in microquasars in our galaxy | |
| dc.type | text |