Holographic tachyon model

doi:10.1016/j.physletb.2007.06.019

Physics Letters B

Volume 651, Issues 2–3, 26 July 2007, Pages 84-88

https://doi.org/10.1016/j.physletb.2007.06.019 Get rights and content

Abstract

We propose in this Letter a holographic model of tachyon dark energy. A connection between the tachyon scalar-field and the holographic dark energy is established, and accordingly, the potential of the holographic tachyon field is constructed. We show that the holographic evolution of the universe with $c ⩾ 1$ can be described completely by the resulting tachyon model in a certain way.

Section snippets

Acknowledgements

This work is supported by the China Postdoctoral Science Foundation, the K.C. Wong Education Foundation (Hong Kong), the National Natural Science Foundation of China, as well as the National Basic Research Program of China (2003CB716300).

References (28)

A.G. Riess
Astron. J.
(1998)
S. Perlmutter
Astrophys. J.
(1999)
D.N. Spergel
Astrophys. J. Suppl.
(2003)
D.N. Spergel
M. Tegmark
Phys. Rev. D
(2004)
K. Abazajian
Astron. J.
(2004)
K. Abazajian
Astron. J.
(2005)
A. Einstein
Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys.)
(1917)
S. Weinberg
Rev. Mod. Phys.
(1989)
V. Sahni et al.
Int. J. Mod. Phys. D
(2000)
S.M. Carroll
Living Rev. Rel.
(2001)
P.J.E. Peebles et al.
Rev. Mod. Phys.
(2003)
T. Padmanabhan
Phys. Rep.
(2003)
E.J. Copeland et al.
Int. J. Mod. Phys. D
(2006)
P.J.E. Peebles et al.
Astrophys. J.
(1988)
B. Ratra et al.
Phys. Rev. D
(1988)
C. Wetterich
Nucl. Phys. B
(1988)
J.A. Frieman et al.
Phys. Rev. Lett.
(1995)
M.S. Turner et al.
Phys. Rev. D
(1997)
R.R. Caldwell et al.
Phys. Rev. Lett.
(1998)
A.R. Liddle et al.
Phys. Rev. D
(1999)
I. Zlatev et al.
Phys. Rev. Lett.
(1999)
P.J. Steinhardt et al.
Phys. Rev. D
(1999)
R.R. Caldwell
Phys. Lett. B
(2002)
R.R. Caldwell et al.
Phys. Rev. Lett.
(2003)
C. Armendariz-Picon et al.
Phys. Rev. Lett.
(2000)
C. Armendariz-Picon et al.
Phys. Rev. D
(2001)
A. Sen
JHEP
(2002)
A. Sen
JHEP
(2002)
N. Arkani-Hamed et al.
JHEP
(2004)
S. Mukohyama
JCAP
(2006)
F. Piazza et al.
JCAP
(2004)
J.F. Zhang et al.

B. Feng et al.

Phys. Lett. B

(2005)

Z.K. Guo et al.

Phys. Lett. B

(2005)

X. Zhang

Commun. Theor. Phys.

(2005)

H. Wei et al.

Class. Quantum Grav.

(2005)

H.S. Zhang et al.

Phys. Rev. D

(2007)

L. Amendola

Phys. Rev. D

(2000)

D. Comelli et al.

Phys. Lett. B

(2003)

X. Zhang

Mod. Phys. Lett. A

(2005)

X. Zhang

Phys. Lett. B

(2005)

C. Deffayet et al.

Phys. Rev. D

(2002)

V. Sahni et al.

JCAP

(2003)

A.Y. Kamenshchik et al.

Phys. Lett. B

(2001)

M.C. Bento et al.

Phys. Rev. D

(2002)

X. Zhang et al.

JCAP

(2006)

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Holographic tachyon model

Abstract

Section snippets

Acknowledgements

Astron. J.

Astrophys. J.

Astrophys. J. Suppl.

Phys. Rev. D

Astron. J.

Astron. J.

Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys.)

Rev. Mod. Phys.

Int. J. Mod. Phys. D

Living Rev. Rel.

Rev. Mod. Phys.

Phys. Rep.

Int. J. Mod. Phys. D

Astrophys. J.

Phys. Rev. D

Nucl. Phys. B

Phys. Rev. Lett.

Phys. Rev. D

Phys. Rev. Lett.

Phys. Rev. D

Phys. Rev. Lett.

Phys. Rev. D

Phys. Lett. B

Phys. Rev. Lett.

Phys. Rev. Lett.

Phys. Rev. D

JHEP

JHEP

JHEP

JCAP

JCAP

Phys. Lett. B

Phys. Lett. B

Commun. Theor. Phys.

Class. Quantum Grav.

Phys. Rev. D

Phys. Rev. D

Phys. Lett. B

Mod. Phys. Lett. A

Phys. Lett. B

Phys. Rev. D

JCAP

Phys. Lett. B

Phys. Rev. D

JCAP