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From: "Serge Repin"
To: , "Serge Repin"
Subject: Black Holes 2000
Date: Tue, 22 Feb 2000 21:09:52 +0300
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Dear colleagues,

I'd like to participate in the Colloquium BH-2000.=20
I ask you to include my 10-15-minute talk (Alexander Zakharov is a =
co-author)=20
in the Colloquium agenda, if it is not too late.=20
I send you the attached proposal, written in LaTeX.
Let me know if I can help you more.
=20
With best regards,
Serge Repin.

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size=3D2> =20
Dear colleagues,

I'd like to =
participate in the=20
Colloquium BH-2000.

I ask you to include my =
10-15-minute=20
talk (Alexander Zakharov is a co-author) size=3D2>

in the Colloquium agenda, if it is not =
too late.=20

I send you the attached =
proposal,=20
written in LaTeX.

Let me know if I can help =
you=20
more.

With best=20
regards,

size=3D2> &nbs=
p; Serge=20
Repin.

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Observational manifestations of General Relativity
in the accretion disks around the supermassive black holes

Serge V. Repin (IKI)
and
Alexander F. Zakharov (ITEP)

Recent observations of Seyfert galaxies, carried out by
ASCA and RXTE seem to indicate that the broad iron $K_\alpha$
line (6.4 keV) takes its origin in the innermost area of the
accretion disk around a supermassive black hole. In the region
$(1 - 3)r_g$, where the line is assummed to arise the effects
of General Relativity (GR) should be taken into account.

A spectrum of a solitary emission line of a hot spot in the
Kerrian accretion disk has been simulated, depending on the radial
coordinate $r$ and the angular momentum $a=J/M$ of a black hole,
under the assumption of equatorial circular motion of a hot spot.
It is shown that the characteristic two-peak line profile with
the sharp edges arises at a large distance,
(about $r \approx (3-10)r_g$) or large inclination angle. The
inner regions emit the line, which is observed at the infinity
with one maximum and extremely wide red wing. The disk spectrum
is simulated then as a sum of the thin rings spectra.

It is shown also that the angular momentum $a$ is a difficult
parameter for the immediate measurements. Only the high
accuracy future spectral observations, being carried out, could
detect this quantity.

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