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Theoretical Constraint on Purely Kinetic k-Essence |
YANG Rong-Jia1;ZHANG Shuang-Nan1,2 |
1Department of Physics and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 1000842Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, PO Box 918-3, Beijing 100049 |
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Cite this article: |
YANG Rong-Jia, ZHANG Shuang-Nan 2008 Chin. Phys. Lett. 25 344-346 |
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Abstract Purely kinetic k-essence models in which the Lagrangian contains only a kinetic factor and does not depend explicitly on the field itself are considered, and a theoretical constraint is obtained: Fx=F0a-3. Under this theoretical constraint, we discuss a kind of purely k-essence with form F(X)=-(1+2Xn)1/2n, which can be considered as the generalized tachyon field, and find that this kind of k-essence is not likely a candidate of dark energy to describe the present accelerated expansion of the Universe. This is contrary to a previous suggestion that k-essence with such a form may be used to describe phantom cosmologies.
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Keywords:
95.36.+x
98.80.-k
98.80.Jk
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Received: 13 October 2007
Published: 27 December 2007
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[1] Tegmark M et al 2004 Phys. Rev. D 69 103501 Tegmark M et al 2004 Astrophys. J. 606 702 [2] Spergel D N et al 2003 Astrophys. J. Suppl. 148 175 [3] Riess A G et al 1998 Astron. J. 116 1009 [4] Perlmutter S et al 1999 Astrophys. J. 517 565 [5] Armendariz-Picon C, Mukhanov V and Steinhardt P J 2000 Phys. Rev. Lett. 85 4438 Armendariz-Picon C, Mukhanov V and Steinhardt P J 2001 Phys. Rev. D 63 103510 [6] Chiba T, Okabe T and Yamaguchi M 2000 Phys. Rev. D 62 023511 [7] Malquarti M, Copeland E J, Liddle A R and Troden M 2003 Phys.Rev. D 67 123503 [8] Padmanabhan T 2002 Phys. Rev. D 66 021301 [9] Aguirregabiria J M, Chimento L P and Lazkoz R 2004 Phys.Rev. D 70 023509 [10] Scherrer R J 2004 Phys. Rev. Lett. 93 011301 [11] Guendelman E I and Kaganovich A B 2007 Phys. Rev. D 75 083505 [12] Armendariz-Picon C and Lim E A 2005 J. Cosmol.Astropart. Phys. JCAP08(2005)007 [13] Garriga J and Mukhanov V F 1999 Phys. Lett. B 458219 [14] Chimento L P 2004 Phys. Rev. D 69 123517 [15] Sen A 2002 Mod. Phys. Lett. A 17 1797 Sen A 2005 Int. J. Mod. Phys. A 20 5513 [16] Gao C J and Zhang S N 2004 Phys. Rev. D 70 124019 Gao C J and Zhang S N 2006 Gen. Rel. Grav. 38 23 Yang R J and Jing J L 2004 Chin. Phys. 5 13 Yang R J and Jing J L 2004 Chin. Phys. Lett. 3 21 [17] Gerasimov A A and Shatashvili S L 2000 J. High EnergyPhys. JHEP10(2000)034 [18] Sen A 2002 J. High Energy Phys. JHEP04(2002)048 Feinstein A 2002 Phys. Rev. D 66 063511 [19] Bergshoeff E A, de Roo M, de Witt T C, Eyras E and Panda S2000 J. High Energy Phys. 5 9 [20] Kamenshchik A, Moschella U and Pasquier V 2001 Phys. Lett. B 511 265 Gorini V, Kamenshchik A and Moschella U 2003 Phys.Rev. D 67 063509 [21] Frolov A, Kofman L and Starobinsky A 2002 Phys. Lett. B 545 8 [22] Wu P and Yu H 2007 J. Cosmol. Astropart. Phys. 03015 Wu P and Yu H 2007 Astrophys. J. 658 663 Yang R J and Zhang S N 2007 J. Cosmol. Astropart.Phys. (accepted) [23] de la Macorra A and Vucetich H 2004 J. Cosmol. Astropart.Phys. 09 012 [24] Abramo L R and Pinto-Neto N 2006 Phys. Rev. D 73063522 |
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