AAS 204th Meeting, June 2004
Session 44 Active Galaxies
Poster, Tuesday, June 1, 2004, 10:00am-7:00pm, Ballroom

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[44.02] Iron K\alpha Fluorescent Line Profiles from Spiral Accretion Flows in AGNs

K. Fukumura, S. Tsuruta (Montana State University-Bozeman)

We present iron K\alpha fluorescent line profiles at 6.4 keV predicted for a relativistic black hole accretion disk in the presence of a spiral motion in Kerr geometry, the work extended from an earlier literature motivated by recent magnetohydrodynamic (MHD) simulations. The velocity field of the spiral motion, superposed on the background Keplerian flow, results in a complicated redshift distribution in the accretion disk. Based on this accretion model, the theoretical iron line profile is calculated in full Kerr geometry. An X-ray source in our model is attributed to a localized flaring region on the black hole symmetry axis, which illuminates the iron in the disk plane. The emissivity form becomes very steep because of the light bending effect.

It is found that the broad line profile generally shows many spike-like sub-peaks due to the spiral motion, especially for an illuminating source close to the disk. Such spiked features are not predicted from a standard disk-corona model. Depending on the rotational phase of the spiral wave, the line shape also changes dramatically forming a single-peak, double-peak, or a multiple-peak. Our results emphasize that in the presence of the spiral velocity field an extremely redshifted iron line profile with a noticeable spike-like feature can be realized.

The future X-ray observations with sufficient spectral resolution E / \Delta E, such as Astro-E2, can test our spiral wave model which exhibits unique spike-like features. Furthermore, they may be able to allow us to identify the characteristics of the spiral wave occurring in the innermost accretion disk.

If you would like more information about this abstract, please follow the link to http://www.physics.montana.edu/students/keigo/homepage/html/research.html. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: fukumura@physics.montana.edu

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