Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-26T05:15:30.419Z Has data issue: false hasContentIssue false
  • English
  • Français

Monitoring the profile variability of the double-peaked Balmer lines in Arp 102B

Published online by Cambridge University Press:  24 November 2004

Suvi Gezari ,
J. P. Halpern ,
M. Eracleous  and
A. V. Filippenko
Suvi Gezari
Affiliation:
Columbia University, New York, NY 10027, USA email: suvi@astro.columbia.edu
J. P. Halpern
Affiliation:
Columbia University, New York, NY 10027, USA email: suvi@astro.columbia.edu
M. Eracleous
Affiliation:
Pennsylvania State University, USA
A. V. Filippenko
Affiliation:
University of California, Berkeley, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We present the results of over 20 years of optical spectroscopic monitoring of the prototypical double-peaked emitter, Arp 102B. Its distinct double-peaked, extremely broad (FWHM ≈15,000 km s−1) low-ionization lines (Hα, Hβ, and Mg II) are well-modeled by emission from photoionized gas in a relativistic Keplerian accretion disk around a central black hole (Chen & Halpern 1989; Halpern et al. 1996). A ubiquitous property of double-peaked emitters is long-term variability in the shape of their line profiles on the timescale of months to years, which is consistent with the dynamical timescale of an accretion disk. This variability can be attributed to inhomogeneities in the line-emitting disk, i.e., hot spots, spiral arms, eccentricity, and warps. We characterize the profile variability of Arp 102B in detail, and use it to constrain physical models for the structure and dynamics of its line-emitting accretion disk.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. 95 - 96
Copyright
© 2004 International Astronomical Union