G. Generalizations: III. Inhomogeneous density profiles
An interesting possibility that arose with the observation of the variable light curve of the afterglow of GRB 021004 is that the ejecta encounters surrounding matter with an irregular density profile [165, 209, 274]. To explore this situation one can resort to numerical simulation of the propagation of the blast wave into a selected density profile [209]. Instead one can attempt to model this analytically or almost analytically [271]. The key for this analytic model is the approximation of the light curve from an inhomogeneous density profile as a series of emission from instantaneous BM solutions, each with its own external density.
1. The light curve of a BM solution
The observed flux, at an observer time t, from an arbitrary spherically symmetric emitting region is given by [140]:
![]() |
(98) |
where n' is the emitters density and
P'
is the emitted spectral power per emitter, both are measured in the
fluid frame;
is the
angle relative to the line of sight, and
-1 = 1 /
(1 -
v cos
/
c) (v is the emitting matter bulk velocity) is the
blue-shift factor.
Nakar and Piran
[271]
show 7 that using
the self-similar nature of the BM profile (with an external density
r-k) one can reduce Eq. 98 to:
![]() |
(99) |
The integration over R is over the shock front of the BM
solution. The upper limit Rmax corresponds to the shock
position from where photons leaving along the line of sight reach
the observer at t. The factor D is the distance to the
source (neglecting cosmological factors).
is the local
spectral index.
The factor
g is a dimensionless factor that describes
the observed pulse shape of an instantaneous emission from a BM
profile. The instantaneous emission from a thin shell produces a
finite pulse (see Section IVB and
Fig. 14). This is generalized now
to a pulse
from an instantaneous emission from a BM profile. Note that even though
the BM profile extends from 0 to R most of the emission arise
from a narrow regions of width ~ R /
2 behind
the shock front. g
is obtained by integration Eq. 98
over cos
and
r, i.e. over the volume of the BM
profile. It depends only on the radial and angular structure of
the shell. The self-similar profile of the shell enables us to express
g
as a general function that depends only on
the dimensionless parameter
(t -
tlos(R)) / tang(R),
with tlos(R) is the time in
which a photon emitted at R along the line of sight to the center
reaches the observer and
tang
R / 2c
2. The
second function,
A
, depends
only on the conditions of
the shock front along the line-of-sight. It includes only
numerical parameters that remain after the integration over the
volume of the shell.
When all the significant emission from the shell at radius R
is within the same power-law segment,
, (i.e
is far from the break frequencies) then
A
and
g
are given by:
![]() |
(100) |
where R is the radius of the shock front,
next(R) is
the external density, E is the energy in the blast-wave,
M(R) the total collected mass up to radius R and
H is a
numerical factor which depends on the observed power law
segment (see [271]
for the numerical values.
![]() |
(101) |
where
![]() |
(102) |
This set of equations is completed with the relevant relations between the different variables of the blast wave, the observer time and the break frequencies.
These equations describe the light curve within one power law segment of the light curve. Matching between different power laws can be easily done [271]. The overall formalism can be used to calculate the complete light curve of a BM blast wave.
2. The light curve with a variable density or energy
The results of the previous section can be applied to study the effect of variations in the external density or in the energy of the blast-wave by approximating the solution as a series of instantaneous BM solutions whose parameters are determined by the instantaneous external density and the energy. Both can vary with time. This would be valid, of course, if the variations are not too rapid. The light curve can be expressed as an integral over the emission from a series of instantaneous BM solutions.
When a blast wave at radius R propagates into the circumburst
medium, the emitting matter behind the shock is replenished within
R
R(21 / (4
- k) - 1). This is the length scale
over which an external density variation relaxes to the BM
solution. This approximation is valid as long as the density
variations are on a larger length scales than
R. It
fails when there is a sharp density increase over a range of
R. However,
the contribution to the integral from the region on which the solution
breaks is small
(
R / R
<< 1)
and the overall light curve approximation is acceptable.
Additionally the density variation must be mild enough so that it
does not give rise to a strong reverse shock that destroys the BM
profile.
A sharp density decrease is more complicated. Here the length
scale in which the emitting matter behind the shock is
replenished could be of the order of R. As an example we
consider a sharp drop at some radius Rd and a constant
density for R > Rd. In this case the
external density is
negligible at first, and the hot shell cools by adiabatic
expansion. Later the forward shock becomes dominant again.
Kumar and Panaitescu
[204]
show that immediately after the drop
the light curve is dominated by the emission during the adiabatic
cooling. Later the the observed flux is dominated by emission from
R
Rd, and at the end the new forward shock
becomes dominant. Our approximation includes the emission before
the density drop and the new forward shock after the drop, but it
ignores the emission during the adiabatic cooling phase.
As an example for this method Fig 24
depicts the
m <
<
c light curve for a
Gaussian
(
R / R
= 0.1) over-dense region in the ISM. Such a density
profile may occur in a clumpy environment. The emission from a
clump is similar to the emission from a spherically over-dense
region as long as the clump's angular size is much larger than 1 /
. Even a mild short
length-scale, over-dense region
(with a maximal over-density of 2) influences the light curve for
a long duration (mainly due to the angular spreading). This
duration depends strongly on the magnitude of the over-density.
![]() |
Figure 24. The light curves
results from a Gaussian
( |
The calculations presented so far do not account, however, for the
reverse shock resulting from density enhancement and its effect on
the blast-wave. Thus the above models are limited to slowly
varying and low contrast density profiles. Now, the observed flux
depends on the external density, n, roughly as
n1/2. Thus,
a large contrast is needed to produce a significant
re-brightening. Such a large contrast will, however, produce a
strong reverse shock which will sharply decrease the Lorentz
factor of the emitting matter behind the shock,
sh,
causing a sharp drop in the emission below
c and a long
delay in the arrival time of the emitted photons (the observer
time is
sh-2). Both factors combine to
suppresses the flux and to set a strong limit on the steepness of
the re-brightening events caused by density variations.
The method can be applied also to variations in the blast wave's energy. Spherically symmetric energy variations are most likely to occur due to refreshed shocks, when new inner shells arrive from the source and refresh the blast wave [207, 335, 366]. Once more, this approximation misses the effect of the reverse shock that arise in this case [207]. However it enables a simple calculation of the observed light curve for a given energy profile.
7 See [140] for an alternative method for integrating Eq. 98. Back.