C. External Shocks
Consider the situation when a cold relativistic shell (whose internal energy is negligible compared to the rest mass) moves into the cold ISM. Generally, two shocks form: an outgoing shock that propagates into the ISM or into the external shell, and a reverse shock that propagates into the inner shell, with a contact discontinuity between the shocked material (see Fig. 22).
There dual shocks system is divided to four distinct regions (see Fig. 22): the ambient matter at rest (denoted by the subscript 1), the shocked ambient matter which has passed through the forward shock (subscript 2 or f), the shocked shell material which has passed through the reverse shock (subscript 3 or r), and the unshocked material of the shell (subscript 4). The nature of the emitted radiation and the efficiency of the cooling processes depend on the conditions in the shocked regions 2 and 3. Both regions have the same energy density e. The particle densities n2 and n3 are, however, different and hence the effective "temperatures," i.e. the mean Lorentz factors of the random motions of the shocked protons and electrons, are different.
![]() |
Figure 22. The Lorentz factor
|
Two quantities determine the shocks' structure:
, the Lorentz
factor of the motion of the inner expanding matter (denoted 4)
relative to the outer matter (the ISM or the outer shell in the
case of internal collisions - denoted 1) , and the ratio between
the particle number densities in these regions, n4 /
n1.
Initially the density contrast between the spherically expanding
shell and the ISM is large. Specifically
n4 / n1 >
2. This
happens during the early phase of an external shock when the shell
is small and dense. This configuration is denoted "Newtonian"
because the reverse shock is non-relativistic at most (or mildly
relativistic). In this case all the energy conversion takes place
in the forward shock. Only a negligible fraction of the energy is
converted to thermal energy in the reverse shock if it is Newtonian
[368].
Let
2 be
the Lorentz factor of the motion of the shocked fluid relative to the
rest frame of the fluid at 1 and let
3
be the Lorentz factor of the motion of this fluid relative to the rest
frame of the relativistic shell (4):
![]() |
(52) |
The particle and energy densities (n, e) in the shocked regions satisfy:
![]() |
(53) |
Later, the shell expands and the density ratio decreases (like
R-2 if the width of the shell is constant and like
R-3 if the shell is spreading) and
n4 / n1 <
2 (but
n4 / n1 > 1). In this case both
the forward and the reverse shocks
are relativistic. The shock equations between regions 1 and 2
combined with the contact discontinuity between 3 and 2 yield
[30,
31,
305]:
![]() |
(54) |
Similar relations hold for the reverse shock:
![]() |
(55) |
Additinally,
![]() |
(56) |
which follow from the equality of pressures and velocity on the contact discontinuity. Comparable amounts of energy are converted to thermal energy in both shocks when both shocks are relativistic.
The interaction between a relativistic flow and an external medium depends on the Sedov length that is defined generally as:
![]() |
(57) |
The rest mass energy within the Sedov sphere equals the energy of the explosion. For a homogeneous ISM:
![]() |
(58) |
Note that in this section E stands for the isotropic equivalent
energy. Because of the very large Lorentz factor angular
structure on a scale larger than
-1 does
not influence
the evolution of the system and it behaves as if it is a part of
a spherical system. A second length scale that appears in the
problem is
, the
width of the relativistic shell in the observer's rest frame.
Initially the reverse shocks is Newtonian and only a negligible
amount of energy is extracted from the shell. At this stage the
whole shell acts "together". Half of the shell's kinetic energy
is converted to thermal energy when the collected external mass is
M/, where
M is the shell's mass
[184,
333].
This takes place at a distance:
![]() |
(59) |
where E52 is the equivalent isotropic energy in 1052ergs, n1 = nism / 1 particle / cm3.
However, the reverse shock might become relativistic before
R. Now energy extraction from the shell is efficient
and one passage of the reverse shock through the shell is sufficient
for complete conversion of the shell's energy to thermal energy.
The energy of the shell will be extracted during a single passage
of the reverse shock across the shell. Using the expression for
the velocity of the reverse shock into the shell (Eq.
55) one finds that the reverse shock reaches the inner edge of the shell at
R
[368]:
![]() |
(60) |
The reverse shock becomes relativistic at RN, where
n4 / n1 =
2:
![]() |
(61) |
Clearly, if RN >
R then the energy of the shell is
dissipated while the shocks are still "Newtonain". If
RN <
R
the reverse shock becomes relativistic. In this case
R
looses its meaning as the radius where the energy is
dissipated. The energy of the shell is dissipated in this
"relativistic" case at
r
. The question which of the two
conditions is relevant depends on the parameter
[368]:
![]() |
(62) |
I have used a canonical value for
as 1012
cm. It will be shown later that within the internal-external scenario
/ c
corresponds to the duration of the bursts and
1012 cm corresponds to a typical burst of 30 sec.
Using one can
express the different radii as:
![]() |
(63) |
For completeness I have added to this equation RInt, where
internal shocks take place (see Eq. 42). The dimensionless
quantity :
/
. Thus:
![]() |
(64) |
I have marked in bold face the location where the effective energy
extraction does take place. With typical values for l,
and
is around
unity. The radius where energy extraction takes place is marked in bold
face!
Expanding shell: A physical shell is expected to expand
during as it propagates with
=
0 +
R
2
[315].
This will lead to a monotoneously decreasing
. As the value of
R
is independent of
it
does not vary. However, R
and
RN decrease from their initial values. If
0 <
R
2
(corresponding to
0 >
1) then
= 1 at
R
= R
= RN and all
three radii coincide. Given the fact that with typical parameters
is of order
unity this seems to be the "typical" case. The
reverse shocks becomes mildly relativistic just when the energy
extraction becomes efficient. However, if
0
<< 1 then the
shell won't expand enough and still there will be a relativistic
reverse shock operating at R
. It
is useful to note that
in this case the effective energy extraction takes place at
R
for all initial values of
0. In
the following I denote by
the
value of
at
R
:
0 if
0 <
1 and otherwise
1.
Overall the external shocks take place at:
![]() |
(65) |
Usually I will use the second relation (the spreading shell one)
in the following discussion. Note that in the case of non
spreading shell one uses the maximum of the two possible radii.
For example in the Newtonian case where the extraction is at l /
2/3 the
shocks pass the shall many times and hence l /
2/3 >
l3/4
1/4.
2. Synchrotron Spectrum from External Shocks
The bulk of the kinetic energy of the shell is converted to
thermal energy via the two shocks at around the time the shell
has expanded to the radius R (this
would be the case in either a thick shell with
< 1 or with
an expanding shell that begins with
0 >
1 but reaches
1 due to
expansion of the shell around the time when
R
= R
and
efficient dissipation takes place . At this radius, the
conditions at the forward shock are:
![]() |
(66) |
while at the reverse shock:
![]() |
(67) |
Substitution of
sh =
2 =
3/4 in Eq.
13 yields, for the equipartition magnetic field:
![]() |
(68) |
If the magnetic field in region 2 behind the forward shock is
obtained purely by shock compression of the ISM field, the field
would be very weak, with
B
<< 1. Such low fields are
incompatible with observations of GRBs. I consider, therefore, the
possibility that there may be some kind of a turbulent instability
which brings the magnetic field to approximate equipartition
[108,
386].
In the case of the
reverse shock, i.e. in region 3, magnetic fields of considerable
strength might be present in the pre-shock shell material if the
original exploding fireball was magnetic. The exact nature of
magnetic field evolution during fireball expansion depends on
several assumptions. Thompson
[406]
found that the magnetic
field will remain in equipartition if it started off originally in
equipartition. Mészáros, Laguna & Rees
[257]
on the other hand, estimated that if the magnetic field was initially in
equipartition then it would be below equipartition by a factor of
10-5 by the time the shell expands to R
. It is
uncertain which, if either one, of the estimates is right. As in
the forward shock, an instability could boost the field back to
equipartition. Thus, while both shocks may have
B << 1
with pure flux freezing, both could achieve
B
1 in the presence of
instabilities. In principle,
B could
be different for the two shocks. For simplicity I will consider the same
value in the following discussions.
Following the discussion in Section VB, I
assume that in both regions 2 and 3 the electrons have a power law
distribution with a minimal Lorentz factor
e,min given by Eq. 22 with the corresponding
Lorentz factors for the forward and the reverse shocks.
Forward shock: The typical energy of synchrotron photons as
well as the synchrotron cooling time depend on the Lorentz factor
e
of the relativistic electrons under consideration and
on the strength of the magnetic field. Using Eq. 22 for
e,min and Eq. 16 for the characteristic
synchrotron energy for the forward shock:
![]() |
(69) |
and
![]() |
(70) |
The characteristic frequency and the corresponding cooling time for the "typical" electron are larger and shorter by a factor of [(p - 2) / (p - 1)]2, correspondingly.
The electrons at the forward shock are fast cooling and w the typical cooling frequency is [373]:
![]() |
(71) |
where ts is the time in seconds. The photons from the
early forward shock are in the low
-rays to
X-ray range, but this depends strongly on the various parameters (note
the strong
24
dependence in equation 69). For this set of canonical parameters
m <
c. However, the
ratio of these two frequencies depends on
8! For
slightly larger then
100 the inequality will reverse and the system will be in the fast
cooling regime.
Reverse Shock: The Lorentz factor of the reverse shock,
3
is smaller by a factor of
3/2
than
the Lorentz factor of the forward shock
2.
Similarly the Lorentz factor of a "typical electron" in the reverse
shock is lower by a factor
3/2
. Therefore the
observed energy is lower by a factor
3
2. The
typical synchrotron frequency of the reverse shock is
![]() |
(72) |
This is in the IR regions but note again the strong dependence on
the Lorentz factor and on
e, which
could easily bring
this frequency up to the optical regime. The cooling frequency in
the reverse shock region is the same as the cooling frequency of
the forward shock (if both regions have the same
B)
[373] hence:
![]() |
(73) |
In the forward shock
m is comparable or
larger than
c.
In the reverse shock
m <
c and it is usually
in the slow cooling regime. The reverse shocks exists for a short time
until it reaches the back of the relativistic shell. Then it
turns into a rarefraction wave that propagates forwards. After
some back and forth bounces of these wave all the matter behind
the forward shock organizes itself in the form of the
Blandford-McKee self similar solution discussed latter in
Section VIIA. This above estimates suggest
[236,
371,
372,
373]
that during the short
phase in which the reverse shock exists it should produce a
powerful optical flash. This flash should coincide with the late
part of the GRB. Kobayashi
[192]
calculates the light curves and typical frequencies of the reverse shock
for a variety of conditions.