摘要The weak gravity conjecture is proposed as a criterion to distinguish the landscape from the swampland in string theory. As an application in cosmology of this conjecture, we use it to impose theoretical constraint on parametersof the Chaplygin-gas-type models. Our analysis indicates that the Chaplygin-gas-type models realized in quintessence field are in the swampland.
Abstract：The weak gravity conjecture is proposed as a criterion to distinguish the landscape from the swampland in string theory. As an application in cosmology of this conjecture, we use it to impose theoretical constraint on parametersof the Chaplygin-gas-type models. Our analysis indicates that the Chaplygin-gas-type models realized in quintessence field are in the swampland.
(Particle-theory and field-theory models of the early Universe (including cosmic pancakes, cosmic strings, chaotic phenomena, inflationary universe, etc.))
[1] Copeland E J, Sami M and Tsujikawa S 2006 Int. J.Mod. Phys. D 15 1753 [hep-th/0603057] [2] Giddings S B, Kachru S and Polchinski J 2002 Phys.Rev. D 66 106006 [3] Kachru S, Kallosh R, Linde A and Trivedi S P 2003 Phys. Rev. D 68 046005 [4] Douglas M R Talk at the Strings 2005 Conference VafaC [hep-th/0509212] [5] Susskind L [hep-th/0302219] [6] Arkani-Hamed N, Motl L, Nicolis A and Vafa C 2007 J.High Energy Phys. 0706 060 [hep-th/0601001] [7] Huang Q G, Li M and Song W 2006 J. High Energy Phys. 0610 059 [hep-th/0603127] [8] Huang Q G 2007 J. High Energy Phys. 0705 096 [astro-ph/0703071] [9] Huang Q G arXiv:0706.2215 [hep-th] [10] Huang Q G, Li M and Wang Y arXiv:0707.3471 [hep-th] [11] Huang Q G arXiv:0708.2760 [astro-ph] [12] Chaplygin S 1904 Sci. Mem. Moscow Univ. Math. Phys. 21 1 [13] Kamenshchik A, Moschella U and Pasquier V 2001 Phys.Lett. B 511 265 [14] Bili$\acute{c$ N, Tupper G B and Viollier R D 2002 Phys. Lett. B 535 17 [15] Bento M C, Bertolami O and Sen A A 2002 Phys. Rev.D 66 043507 Sen A A and Scherrer R J 2005 Phy. Rev. D 72063511 [16] Guo Z K and Zhang Y Z 2007 Phys. Lett. B 645326 [17] Bento M C, Bertolami O and Sen A A 2003 Phys. Rev.D 67 063003 [18] Bertolami O, Sen A A, Sen S, and Silva P T 2004 Mon.Not. R. Astron. Soc. 353 329 [astro-ph/0402387] [19] Gong Y G 2005 JCAP 0503 007 [20] Zhu Z H 2004 Astron. Astronphys. 423 421 [astro-ph/0411039] [21] Sethi G, Singh S K, Kumar P, Jain D and Dev A 2006 Int. J. Mod. Phys. D 15 1089 [22] Guo Z K and Zhang Y Z [astro-ph/0509790] [23] Bili$\acute{c$ N, Tupper G B and Viollier R D 2004 J. Cosmol. Astropart. Phys. 0411 008 [24] Reis R R R, Waga I, Calv$\tilde{a$o M O, andJor$\acute{a$s S E 2003 Phys. Rev. D 68 061302 [25] Tegmark M et al 2004 Phys. Rev. D 69103501 [26] Spergel D N et al 2007 Astrophys. J. Suppl. 170 377
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