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Thermodynamics of Apparent Horizon & Dynamics of FRW SpacetimePowerPoint Presentation

Thermodynamics of Apparent Horizon & Dynamics of FRW Spacetime

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Thermodynamics of Apparent Horizon &

Dynamics of FRW Spacetime

Rong-Gen Cai （蔡荣根）

Institute of Theoretical Physics

Chinese Academy of Sciences

Einstein’s Equations (1915):

{Geometry matter (energy-momentum)}

Thermodynamics of black holes :

Schwarzschild Black Hole: Mass M

horizon

More general:

Kerr-Newmann Black Holes

M, J, Q

No Hair Theorem

for the de Sitter Space (1917):

+ I

Gibbons and Hawking (1977):

Cosmological event horizons

I-

（S.Hawking, 1974, J.Bekenstein, 1973)

First law：dM =TdS

Questions: why? (T. Jacobson, 1995)

a) From the First Law to the Friedmann Equations

Friedmann-Robertson-Walker Universe:

1) k = -1

open

2) k = 0

flat

3) k =1

closed

Where:

Some related works:

(1) A. Frolov and L. Kofman, JCAP 0305 (2003) 009

(2) Ulf H. Daniesson, PRD 71 (2005) 023516

(3) R. Bousso, PRD 71 (2005) 064024

Suppose that the perfect fluid is the source, then

The energy-supply vector is: The work density is:

（S. A. Hayward et al., 1997,1998)

Then, the amount of energy crossing the apparent horizon within

the time interval dt

By using the continuity equation:

(Cai and Kim, JHEP 0502 (2005) 050 )

This also holds for more general Lovelock gravity!

b) Friedmann equation and the first law of thermodynmaics

Consider a FRW universe

Apparent horizon

And its surface gravity

which is defined by

Consider the Einstein field equations with perfect fluid

One has the Friedmann equation and the continuity equation

Multiplying both side hands by a factor

One has

Now consider the energy inside the apparent horizon

(Unified first law of thermodynamics, Hayward, 1998,1999)

The case with a Gauss-Bonnet term?

Black hole has an entropy of form

Consider the Friedmann equation in GB gravity

c) Thermodynamics of apparent horizon

in brane world scenario

(RGC and L.M. Cao, hep-th/0612144)

( A. Sheykhi, B. Wang and R.G. Cai, hep-th/0701198) (A. Sheykhi, B. Wang and RGC, hep-th/0701261)

The unified first law: ( S. Hayward, 1998,1999)

Projecting this along a trapping horizon, one can get the first law of

Thermodynamics for a dynamical black hole

For a non-Einstein theory, one can do as follows.

Then one has

Using the relation one could obtain the expression

of horizon entropy. (RGC and L.M. Cao, gr-qc/0611071.)

Two motivations to study the thermodynamics of AH

in brane world scenario:

(1) dE = T dS + W dV?

(2) S = ?

(T. Shiromizu, K.I. Maeda and M. Sasaki, PRD, 2000)

The effective equations on an (n-1)-brane:

In the RSII model

Consider a FRW universe on the brane and suppose the matter on the

brane is a perfect fluid with

then

where on the

One has

( on the RGC and L.M. Cao, hep-th/0612144)

3) on the The first law of thermodynamics for the apparent horizon

4) When the bulk Weyl tensor does not vanish?

Bulk geometry and area formula of horizon entropy on the

We obtain

The horizon area on the

And the entropy

d) on the Corrected entropy-area relation and modified Friedmann

equation

RGC, L.M. Cao and Y.P. Hu JHEP 0808, 090 (2008)

Corrected entropy-area relation:

Friedmann equations

Loop quantum cosmology:

Entropy formula

From corrected entropy-area relation to modified Friedmann equation

Friedmann equations

For a FRW universe with a perfect fluid:

The amount of energy crossing the apparent horizon within equationdt

where A is the area of the apparent horizon.

Assume the temperature

and the Clausius relation

Bouncing universe? equation

Loop quantum cosmology

More general case: equation

further

From modified Friedmann equation to corrected entropy-area relation

Entropy formula

The unified first law

The first law of apparent horizon (R.G. Cai and L.M. Cao, hep-th/0612144)

It is easy to show relation

Compare with

e) Hawking radiation of apparent horizon in FRW universe relation

We know Hawking radiation is always associated with event

horizon of spacetime:

(1) Black hole, (2) de Sitter space, (3) Rindler horizon

Question: how about apparent horizon in FRW?

when k=0, it is quite similar to the Painleve-de Sitter metric (M. Parikh,

PLB 546, 189 (2002)

There is a Kodama vector:

Now let us consider a particle with mass m in FRW universe. metric (M. Parikh,

The Hamilton-Jacobi equation:

By use of the Kodama vector, one could define

Then the action:

Consider the incoming mode, the action has a pole at the apparent horizon

(Parikh and Wilczek,2000)

In WKB approximation, the emission rate Gamma is the square of the

tunneling amplitude:

The emission rate can be cast in a form of thermal spectrum

The end

(R.G. Cai et al. arXiv:0809.1554 [hep-th] )

f) Conclusions of the

- From dQ=TdS to Friedmann equations, here S=A/4G and
- 2) The Friedmann equation can be recast to a universal form

3) There is a Hawking radiation for the apparent horizon in FRW universe

4) In Einstein gravity and Lovelock gravity, the expression of S

has a same form as the black hole entropy

5) In brane world scenario, that form still holds, and we can obtain an

expression of horizon entropy associated with apparent horizon, and

expect it also holds for brane world black hole horizon.

My papers on this subject: of the

1) RGC and S.P. Kim, JHEP 0502, 050 (2005)

2) M. Akbar and RGC, PLB 635，7 (2006);

PRD 75, 084003 (2007)；

PLB 648, 243 (2007)

3) RGC and L. M. Cao, PRD 75, 064008 (2007)；

NPB 785, 135 (2007)

4) A. Sheykhi, B. Wang and RGC, NPB 779, 1 (2007),

PRD 76, 023515 (2007)

5) R.G. Cai, L. M. Cao and Y.P. Hu, JHEP0808, 090 (2008)

6) R.G. Cai, Prog.Theor.Phys.Suppl.172:100-109,2008.

7) R.G. Cai, L. M. Cao and Y.P. Hu, arXiv: 0809.1554

Hawking Radiation of Apparent Horizon in a FRW Universe

Thank You of the

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