8.3. Synchrotron Self Absorption
An important effect that we have ignored so far is the possibility of
self absorption. This is irrelevant during the GRB itself. One of
the essential features of the GRB spectrum is that it is produced in an
optically thin region. However, self absorption may appear at late
time and typically in radio emission
[18,
247,
25,
248,
249].
When it appears it will cause a steep cutoff of the low energy spectrum,
either as the commonly known
5/2 or as
2.
To estimate the self absorption frequency we need the
optical depth along the line of sight. A simple approximation is:
'
' Rl /
1
where
'
' is the absorption
coefficient
[245]:
![]() |
(67) |
The self absorption frequency
a satisfies:
'
'0 R /
= 1. It
can be estimates
only once we have a model for the hydrodynamics and how do R
and
change
with time
[248,
249].
The spectrum below the
the self-absorption frequency
depends on the electron distribution. One obtaine the well known
[245],
5/2 slop when the
synchrotron frequency of the electron emitting
the self absorbed radiation is inside
the self absorption range. One obtains a slope of
22 if there is self
absorption, but the radiation in that range is
due to the low energy tail of electrons radiating effectively
at higher energies. For this latter case, which is more appropriate for
GRB afterglow we find that
[18,
25]:
![]() |
(68) |
where R is the radius of the radiating shell and the
factor kB Te /
(
mp c2) describes the degree of
electron equipartition in the plasma shock-heated to an internal energy per
particle
mp c2 and moving with Lorentz factor
.