Physics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..222...95g&link_type=abstract
The Interplay among Black Holes, Stars and ISM in Galactic Nuclei, Proceedings of IAU Symposium, No. 222. Edited by T. Storchi-B
Physics
2
Scientific paper
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.
Eracleous Michael
Filippenko Alexei V.
Gezari Suvi
Halpern Jules P.
No associations
LandOfFree
Monitoring the profile variability of the double-peaked Balmer lines in Arp 102B does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Monitoring the profile variability of the double-peaked Balmer lines in Arp 102B, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Monitoring the profile variability of the double-peaked Balmer lines in Arp 102B will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1112803