Observational signature of tidal disruption of a star by a massive black hole; Observational signature of tidal disruption of a star by a massive black hole; T. Bogdanovic et al

• Published in: Proceedings of the International Astronomical Union 2004-03, Vol.2004 (IAUS222), p.81
• Main Authors: Bogdanovic, Tamara, Eracleous, Michael, Mahadevan, Suvrath, Sigurdsson, Steinn, Laguna, Pablo
• Format: Article
• Language: English
• Subjects: Astronomy
• ISSN: 1743-9213; 1743-9221

We have modeled the time-variable profiles of the HΑ emission line from the non-axisymmetric disk and debris tail created in the tidal disruption of a solar-type star by a $10^{6} M_{\odot}$ black hole. We find that the line profiles at these very early stages of the evolution of the post-disruption debris do not resemble the double peaked profiles expected from a rotating disk since the debris has not yet settled into such a stable structure. The predicted line profiles vary on fairly short time scales (of order hours to days). As a result of the uneven distribution of the debris and the existence of a 'tidal tail' (the stream of returning debris), the line profiles depend sensitively on the orientation of the tail relative to the line of sight. Given the illuminating UV/X-ray light curve, we also model the HΑ light curve from the debris. [PUBLICATION ABSTRACT]