Thermodynamics of Apparent Horizon & Dynamics of FRW Spacetime

1. Thermodynamics of Apparent Horizon & Dynamics of FRW Spacetime Rong-Gen Cai （蔡荣根） Institute of Theoretical Physics Chinese Academy of Sciences

2. Einstein’s Equations (1915): {Geometry matter (energy-momentum)}

3. Thermodynamics of black holes : Schwarzschild Black Hole: Mass M horizon More general: Kerr-Newmann Black Holes M, J, Q No Hair Theorem

4. On the other hand, for the de Sitter Space (1917): + I Gibbons and Hawking (1977): Cosmological event horizons I-

5. Schwarzschild-de Sitter Black Holes: Black hole horizon and cosmological horizon: First law:

6. Thermodynamics of black hole： （S.Hawking, 1974, J.Bekenstein, 1973) First law：dM =TdS Questions: why? (T. Jacobson, 1995)

7. dE =TdS First law： Dynamics of spacetime： Two ansatz in FRW： (R.G. Cai and S.P.Kim, JHEP (2005))

8. 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

9. Friedmann Equations: Where:

10. Our goal : 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

12. Apparent Horizon in FRW Universe:

13. Apply the first law to the apparent horizon: Make two ansatzes: The only problem is to get dE

14. 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

15. By using the continuity equation: (Cai and Kim, JHEP 0502 (2005) 050 )

16. Higher derivative theory: Gauss-Bonnet Gravity Gauss-Bonnet Term:

17. Black Hole Solution: Black Hole Entropy: (R. Myers,1988, R.G. Cai, 2002, 2004)

18. Ansatz:

19. This time: This also holds for more general Lovelock gravity!

20. b) Friedmann equation and the first law of thermodynmaics Consider a FRW universe Apparent horizon And its surface gravity which is defined by

21. Consider the Einstein field equations with perfect fluid One has the Friedmann equation and the continuity equation Multiplying both side hands by a factor

22. Using the definition One has Now consider the energy inside the apparent horizon (Unified first law of thermodynamics, Hayward, 1998,1999)

23. The case with a Gauss-Bonnet term? Black hole has an entropy of form Consider the Friedmann equation in GB gravity

24. Once again, multiplying a factor with Defining It also holds for Lovelock case !

25. 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

26. 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.)

27. 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)

28. The effective equations on an (n-1)-brane: In the RSII model

29. Consider a FRW universe on the brane and suppose the matter on the brane is a perfect fluid with then

30. The Friedmann equations and continuity equation:

31. where One has

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

33. Some remarks: 1) In the limit, 2) In the limit,

34. 3)The first law of thermodynamics for the apparent horizon 4) When the bulk Weyl tensor does not vanish?

35. Bulk geometry and area formula of horizon entropy We obtain

36. The apparent horizon for a fixed z,

37. The function has a simple zero root at z_{max},

38. The horizon area And the entropy

39. d) 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

40. From corrected entropy-area relation to modified Friedmann equation Friedmann equations For a FRW universe with a perfect fluid:

41. The amount of energy crossing the apparent horizon within dt where A is the area of the apparent horizon. Assume the temperature and the Clausius relation

42. Bouncing universe? Loop quantum cosmology

43. More general case: further

44. 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)

45. Rewriting the modified Friedmann equation

46. It is easy to show Compare with

47. e) Hawking radiation of apparent horizon in FRW universe 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?

48. when k=0, it is quite similar to the Painleve-de Sitter metric (M. Parikh, PLB 546, 189 (2002) There is a Kodama vector:

49. Now let us consider a particle with mass m in FRW universe. The Hamilton-Jacobi equation: By use of the Kodama vector, one could define Then the action:

50. Consider the incoming mode, the action has a pole at the apparent horizon (Parikh and Wilczek,2000)