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Observational signature of tidal disruption of a star by a massive black hole

Published online by Cambridge University Press:  24 November 2004

Tamara Bogdanović ,
Michael Eracleous ,
Suvrath Mahadevan ,
Steinn Sigurdsson  and
Pablo Laguna
Tamara Bogdanović
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: tamarab@astro.psu.edu, mce@astro.psu.edu, suvrath@astro.psu.edu, steinn@astro.psu.edu, pablo@astro.psu.edu Center for Gravitational Wave Physics
Michael Eracleous
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: tamarab@astro.psu.edu, mce@astro.psu.edu, suvrath@astro.psu.edu, steinn@astro.psu.edu, pablo@astro.psu.edu
Suvrath Mahadevan
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: tamarab@astro.psu.edu, mce@astro.psu.edu, suvrath@astro.psu.edu, steinn@astro.psu.edu, pablo@astro.psu.edu
Steinn Sigurdsson
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: tamarab@astro.psu.edu, mce@astro.psu.edu, suvrath@astro.psu.edu, steinn@astro.psu.edu, pablo@astro.psu.edu Center for Gravitational Wave Physics
Pablo Laguna
Affiliation:
Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA email: tamarab@astro.psu.edu, mce@astro.psu.edu, suvrath@astro.psu.edu, steinn@astro.psu.edu, pablo@astro.psu.edu Center for Gravitational Wave Physics
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Abstract

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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.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
POSTERS
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS222 , March 2004 , pp. 81 - 82
Copyright
© 2004 International Astronomical Union