Handling databases in search for microquasars

P.L. LUQUE ESCAMILLA, J. MARTÍ, J.A. COMBI, J.F. ALBACETE-COLOMBO, J.R. SÁNCHEZ-SUTIL, A. MUÑOZ ARJONILLA

Izmir, Turquía

Congreso; Contribution to the 7th. Microquasar Workshop, Foca 2008; 2008

Microquasars are X-ray binary systems with properties that resemble those of quasars. They are composed of a compact object (black hole or neutron star) that is accreting matter from its companion star. Because of the deep gravity well, a huge amount of energy can be released in Xrays from the accretion disk. Relativistic jets are also formed which radiate a broad band non-thermal spectrum from radio to even very high-energy gamma-rays. When the jets interact with the interstellar medium (ISM), extended bow shocks may appearas it has been recently illustrated in the Cygnus X-1 case by Gallo et al. (2005, Nature 436, 819). The situation is analogous to the case of lobes from radio galaxies (see,for instance, Kaiser et al. (2004, ApJ, 612, 332). There a of maximum shock may give rise to a bright hot spot. Microquasars undergo strong flares from time to time due to the dynamics of the jet formation.