Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2010-04-03
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
Accepted for publication in Astronomy & Astrophysics
Scientific paper
Doppler tomography of emission line profiles in low mass X-ray binaries allows us to disentangle the different emission sites and study the structure and variability of accretion disks. We present UVES high-resolution spectroscopic observations of the black hole binary A0620-00 at quiescence.These spectroscopic data constrain the orbital parameters Porb=0.32301405(1) d and K2=437.1+-2.0 km/s. These values, together with the mass ratio q=M2/M1=0.062+-0.010, imply a minimum mass for the compact object of M1(sin i)^3=3.15+-0.10 Msun, consistent with previous works.The H$\alpha$ emission from the accretion disk is much weaker than in previous studies, possibly due to a decrease in disk activity. Doppler imaging of the H$\alpha$ line shows for the first time a narrow component coming from the secondary star, with an observed equivalent width of 1.4+-0.3 Angstroms, perhaps associated to chromospheric activity. Subtracting a K-type template star and correcting for the veiling of the accretion disk yields to an equivalent width of 2.8+-0.3 Angstroms. A bright hot-spot is also detected at the position where the gas stream trajectory intercepts with the accretion disk. The H$\alpha$ flux associated to the secondary star is too large to be powered by X-ray irradiation. It is comparable to those observed in RS CVn binaries with similar orbital periods and, therefore, is probably triggered by the rapid stellar rotation.
Casares Jorge
Gonzalez Hernandez Jonay I.
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