An Explanation for the ``X-ray Baldwin'' Effect
Using our newly developed ionized X-ray reflection code (reported in
Nayakshin, Kazanas and Kallman at this meeting), we compute the
reflection continuum and the iron lines from an accretion disk
illuminated by X-rays. The fact that we self-consistently include the
effects of the thermal ionization instability on the pressure and the
density structure of the illuminated layer makes our study to be much
more sensitive to the geometry of the X-ray producing region(s) and
the disk itself than the previous ionized reflection studies were.
In particular, we consider a standard-like accretion disk illuminated
by X-rays coming from: (a) a full corona; (b) magnetic flares (patchy
corona); (c) a source located at some height above the disk or the
black hole (as in the model of Reynolds and Begelman 1997) . We find
that models (a) and (c) fail to explain the ''X-ray Baldwin effect'',
and that (c) cannot even produce the typical Seyfert 1 iron line
profile. On the other hand, model (b) appears to suggest an
explanation for the X-ray Baldwin effect in AGN and is also promising
in many other respects.
File translated from TEX by TTH, version 2.32.
On 16 Jul 1999, 09:19.