10.1. The connection between thermodynamics and spacetime geometry
The existence of one-way membranes, however, is not necessarily a feature of gravity or curved spacetime and can be induced even in flat Minkowski spacetime. It is possible to introduce coordinate charts in Minkowski spacetime such that regions are separated by horizons, a familiar example being the coordinate system used by a uniformly accelerated frame (Rindler frame) which has a non-compact horizon. The natural coordinate system (t, x, y, z) used by an observer moving with a uniform acceleration g along the x-axis is related to the inertial coordinates (T, X, Y, Z) by
![]() |
(157) |
and Y = y;Z = z. The metric in the accelerated frame will be
![]() |
(158) |
which has the same form as the metric in (153) with
f (x) = (1 + 2gx). This
has a horizon at x = - 1/2g with the surface gravity
= g and
temperature
T = (g / 2
).
All the horizons are implicitly defined with respect to certain class
of observers; for example, a suicidal observer plunging into the
Schwarzschild black hole will describe the physics very differently from
an observer at infinity. From this point of view, which we shall adopt,
there is no need to distinguish between observer dependent and observer
independent horizons. This allows a powerful way of describing the
thermodynamical behaviour of all these spacetimes (Schwarzschild, de
Sitter, Rindler ....) at one go.
The Schwarzschild, de Sitter and Rindler metrics are symmetric under
time reversal and there exists a `natural' definition of a time
symmetric vacuum state in all these cases. Such a vacuum state will
appear to be described a thermal density matrix in a subregion
of spacetime with
the horizon as a boundary. The QFT based on such a state will be
manifestedly time symmetric and will describe an isolated system in
thermal equilibrium in the subregion
.
No time asymmetric phenomena like evaporation, outgoing radiation,
irreversible changes etc can take place in this situation.
We shall now describe how this arises.
Consider a (D+1) dimensional flat Lorentzian manifold
with the signature
(+, - , - ,...) and Cartesian coordinates ZA where
A = (0, 1, 2,..., D).
A four dimensional sub-manifold
in this (D+1)
dimensional space can be defined through a mapping
ZA = ZA(xa) where
xa with a = (0, 1, 2, 3) are the four
dimensional coordinates on the surface. The flat Lorentzian metric in
the (D+1) dimensional space induces a metric
gab(xa) on the four dimensional space
which - for a wide variety of the mappings
ZA = ZA(xa) - will
have the signature
(+ , - , - , -) and will represent, in general, a curved four
geometry. The quantum theory of a free scalar field in
is well defined in terms of the, say, plane wave modes which satisfy the
wave equation in
. A subset of these
modes, which does not depend on the `transverse' directions, will
satisfy the corresponding wave equation in
and will depend only
on xa. These modes induce a natural QFT in
. We are interested
in the mappings
ZA = ZA(xa) which
leads to a horizon in
so that we can
investigate the QFT
in spacetimes with horizons using the free, flat spacetime, QFT in
([294]
[289]).
For this purpose, let us restrict attention to a class of surfaces
defined by the mappings
ZA = ZA(xa)
which ensures the following properties for
: (i) The induced
metric gab has the signature (+ , - , - , -).
(ii) The induced metric is static in the sense that
g0
= 0 and all gabs are independent of x0.
[The Greek indices run over 1,2,3.] (iii) Under the transformation
x0
x0 ±
i(
/g), where
g is a non zero, positive constant, the mapping of the
coordinates changes as Z0
-
Z0, Z1
-
Z1 and ZA
ZA for A = 2,..., D. It will turn out
that the four dimensional manifolds defined by such mappings possess
a horizon and most of the interesting features of the thermodynamics related
to the horizon can be obtained from the above characterization.
Let us first determine the nature of the mapping
ZA = ZA(xa) =
ZA(t,x)
such that the above conditions are satisfied.
The condition (iii) above singles out the spatial coordinate
Z1 from the others. To satisfy this condition we can
take the mapping
ZA = ZA(t, r,
,
) to be of the form
Z0 = Z0(t, r),
Z1 = Z1(t, r),
Z
=
Z
(r,
,
) where
Z
denotes the transverse coordinates ZA with
A = (2,..., D). To impose the condition
(ii) above, one can make use of the fact that
possesses invariance under translations, rotations and Lorentz boosts,
which are characterized by the existence of a set of
N = (1/2)(D + 1)(D + 2)
Killing vector fields
A(ZA). Consider any linear
combination VA
of these Killing vector fields which is time like in a region of
.
The integral curves to this vector field VA will
define time like curves in
. If one treats these
curves as the trajectories of a hypothetical observer, then one can
set up the proper Fermi-Walker transported coordinate system
for this observer. Since the four velocity of the observer is along the
Killing vector field, it is obvious that the metric
in this coordinate system will be static
[295].
In particular, there
exists a Killing vector which corresponds to Lorentz boosts along the
Z1 direction that can be interpreted as rotation in
imaginary time coordinate allowing a natural realization of (iii)
above. Using the property of Lorentz boosts, it is easy to see that the
transformations of the form
Z0 = lf (r)1/2sinh
gt;Z1 = ± lf
(r)1/2cosh gt
will satisfy both conditions (ii) and (iii) where (l, g)
are constants introduced for dimensional reasons and f (r)
is a given function. This map covers only the two quadrants with
| Z1| > | Z0| with positive sign
for the right quadrant and negative sign
for the left. To cover the entire (Z0,
Z1) plane, we will use the full set
![]() |
(159) |
The inverse transformations corresponding to (159) are
![]() |
(160) |
Clearly, to cover the entire two dimensional plane of
- <
(Z0, Z1) < +
, it is necessary
to have both f (r) > 0 and f (r) < 0.
The pair of points (Z0, Z1) and
(- Z0, - Z1) are mapped to the same
(t, r) making this a 2-to-1 mapping.
The null surface Z0 = ± Z1 is
mapped to the surface f (r) = 0.
The transformations given above with any arbitrary mapping for the
transverse coordinate
Z =
Z
(r,
,
) will give
rise to an induced metric on
of the form
![]() |
(161) |
where dL2 depends on the form of the mapping
Z
=
Z
(r,
,
).
This form of the metric is valid in all the quadrants even though
we will continue to work in the right quadrant and will comment
on the behaviour in other quadrants only when necessary. It is
obvious that the
, in general, is
curved and has a horizon at f (r) = 0.
As a specific example, let us consider the case of (D + 1) = 6 with the
coordinates
(Z0, Z1, Z2,
Z3, Z4, Z5) =
(Z0, Z1, Z2,
R,
,
) and consider a mapping to
4-dimensional subspace in which: (i) The (Z0,
Z1) are mapped to (t, r) as before; (ii)
the spherical coordinates
(R,
,
) in
are mapped to
standard spherical polar coordinates in
:
(r,
,
) and (iii) we
take Z2 to be an arbitrary function of r:
Z2 = q(r). This leads to the metric
![]() |
(162) |
with
![]() |
(163) |
Equation (162) is the form of a general, spherically symmetric, static metric in 4-dimension with two arbitrary functions f (r), q(r). Given any specific metric with A(r) and B(r), equations (163) can be solved to determine f (r), q(r). As an example, let us consider the Schwarzschild solution for which we will take f = 4(1 - (l / r)); the condition g00 = (1 / g11) now determines q(r) through the equation
![]() |
(164) |
That is
![]() |
(165) |
Though the integral cannot be expressed in terms of elementary functions, it
is obvious that q(r) is well behaved everywhere including
at r = l. The transformations
(Z0, Z1)
(t, r);Z2
q(r); (Z3, Z4,
Z5)
(r,
,
)
thus provide the embedding of Schwarzschild metric in a 6-dimensional space.
[This result was originally obtained by Frondsal
[296];
but the derivation in that paper is somewhat obscure and does not bring
out the generality of the situation]. As a corollary, we may note that
this procedure leads to a spherically symmetric Schwarzschild-like
metric in arbitrary dimension, with the 2-sphere in (162) replaced any
N-sphere.
The choice lg = 1, f (r) = [1 - (r /
l)2] will provide an embedding
of the de Sitter spacetime in 6-dimensional space with
Z2 = r, (Z3,
Z4, Z5)
(r,
,
).
Of course, in this case, one of the coordinates is actually redundant
and - as we have seen earlier - one can
achieve the embedding in a 5-dimensional space.
A still more trivial case is that of Rindler metric which can be obtained
with D=3,
lg = 1, f (r) = 1 + 2gr; in this case, the
"embedding" is just a reparametrization within four
dimensional spacetime and - in this case - r runs in the range
(-
,
).
The key point is that the metric in (161) is fairly generic and can
describe a host of spacetimes with horizons located at f = 0.
We shall discuss several features related to the thermodynamics of the
horizon in the next few sections.