×
Khodam-Mohammadi, A.

Power-law entropy corrected new holographic scalar field models of dark energy with modified IR-cutoff. (English) Zbl 1274.83159

Mod. Phys. Lett. A 26, No. 33, 2487-2499 (2011).
Summary: In this work, the PLECHDE model with Granda-Oliveros (G-O) IR-cutoff is studied. The evolution of dark energy density, deceleration and EoS parameters are calculated. I demonstrate that under a condition, our universe can accelerate near the phantom barrier at present time. We calculate these parameters also in PLECHDE at Ricci scale, when \(\alpha\) = 2 and \(\beta\) = 1, and a comparison between Ricci scale, G-O cutoff and non-corrected HDE without matter field with G-O cutoff is done. The correspondence between this model and some scalar field of dark energy models is established. By this method, the evolutionary treatment of kinetic energy and potential for quintessence, tachyon, \(K\)-essence and dilaton fields, are obtained. I show that the results has a good compatibility with previous work in the limiting case of flat, dark dominated and non-corrected holographic dark energy.

Cited in 5 Documents

MSC:

83F05 Relativistic cosmology
81P40 Quantum coherence, entanglement, quantum correlations
81T10 Model quantum field theories

Keywords:

entanglement of quantum field; Ricci scale; power law entropy correction; holographic DE
Cite Review PDF
Full Text: DOI arXiv

References:

[1] DOI: 10.1086/307221 · Zbl 1368.85002 · doi:10.1086/307221
[2] DOI: 10.1086/377253 · doi:10.1086/377253
[3] DOI: 10.1103/PhysRevD.69.103501 · doi:10.1103/PhysRevD.69.103501
[4] DOI: 10.1111/j.1365-2966.2004.08080.x · doi:10.1111/j.1365-2966.2004.08080.x
[5] DOI: 10.1103/PhysRevD.66.063508 · doi:10.1103/PhysRevD.66.063508
[6] DOI: 10.1103/PhysRevD.68.043509 · doi:10.1103/PhysRevD.68.043509
[7] DOI: 10.1103/PhysRevD.72.103503 · doi:10.1103/PhysRevD.72.103503
[8] Zimdahl W., Class. Quantum Grav. 26 pp 5461–
[9] DOI: 10.1103/PhysRevD.82.124041 · doi:10.1103/PhysRevD.82.124041
[10] DOI: 10.1103/PhysRevD.71.103504 · doi:10.1103/PhysRevD.71.103504
[11] DOI: 10.1016/j.physletb.2007.03.025 · Zbl 1248.83179 · doi:10.1016/j.physletb.2007.03.025
[12] Setare M. R., J. Cosmol. Astropart. Phys. 02 pp 010–
[13] DOI: 10.1016/j.physletb.2010.02.075 · doi:10.1016/j.physletb.2010.02.075
[14] DOI: 10.1016/j.physletb.2009.10.011 · doi:10.1016/j.physletb.2009.10.011
[15] Setare M. R., J. Cosmol. Astropart. Phys. 09 pp 011–
[16] DOI: 10.1016/j.physletb.2006.11.033 · Zbl 1248.83178 · doi:10.1016/j.physletb.2006.11.033
[17] DOI: 10.1016/j.physletb.2008.07.013 · Zbl 1328.83216 · doi:10.1016/j.physletb.2008.07.013
[18] DOI: 10.1016/j.physletb.2006.10.014 · Zbl 1248.83177 · doi:10.1016/j.physletb.2006.10.014
[19] DOI: 10.1142/S0218271810018086 · Zbl 1204.85022 · doi:10.1142/S0218271810018086
[20] DOI: 10.1103/PhysRevD.7.2333 · Zbl 1369.83037 · doi:10.1103/PhysRevD.7.2333
[21] DOI: 10.1007/BF02345020 · Zbl 1378.83040 · doi:10.1007/BF02345020
[22] DOI: 10.1103/PhysRevD.13.191 · doi:10.1103/PhysRevD.13.191
[23] DOI: 10.1103/PhysRevD.23.287 · doi:10.1103/PhysRevD.23.287
[24] DOI: 10.1103/PhysRevLett.82.4971 · Zbl 0949.83045 · doi:10.1103/PhysRevLett.82.4971
[25] Li M., J. Cosmol. Astropart. Phys. 0912 pp 14–
[26] Li M., J. Cosmol. Astropart. Phys. 06 pp 036–
[27] DOI: 10.1016/j.physletb.2004.10.014 · doi:10.1016/j.physletb.2004.10.014
[28] Hsu S. D. H., Phys. Lett. B 669 pp 275–
[29] DOI: 10.1016/j.physletb.2005.08.134 · doi:10.1016/j.physletb.2005.08.134
[30] DOI: 10.1088/0264-9381/27/2/025007 · Zbl 1184.83074 · doi:10.1088/0264-9381/27/2/025007
[31] DOI: 10.1007/s10714-006-0301-6 · Zbl 1105.83021 · doi:10.1007/s10714-006-0301-6
[32] DOI: 10.1103/PhysRevD.83.023504 · doi:10.1103/PhysRevD.83.023504
[33] DOI: 10.1016/j.physletb.2008.12.025 · doi:10.1016/j.physletb.2008.12.025
[34] DOI: 10.1016/j.physletb.2008.10.017 · doi:10.1016/j.physletb.2008.10.017
[35] DOI: 10.1007/s10509-010-0550-4 · doi:10.1007/s10509-010-0550-4
[36] DOI: 10.1103/PhysRevD.48.R3427 · Zbl 0942.83512 · doi:10.1103/PhysRevD.48.R3427
[37] DOI: 10.1142/S0218271810018116 · Zbl 1204.83101 · doi:10.1142/S0218271810018116
[38] DOI: 10.1007/s10773-010-0585-x · Zbl 1213.83150 · doi:10.1007/s10773-010-0585-x
[39] DOI: 10.1007/s10714-010-1072-7 · Zbl 1208.83121 · doi:10.1007/s10714-010-1072-7
[40] DOI: 10.1209/0295-5075/93/69001 · doi:10.1209/0295-5075/93/69001
[41] DOI: 10.1209/0295-5075/93/29002 · doi:10.1209/0295-5075/93/29002
[42] Khodam-Mohammadi A., Commun. Theor. Phys. 55 pp 5–
[43] DOI: 10.1088/0031-8949/82/02/025901 · Zbl 1202.83135 · doi:10.1088/0031-8949/82/02/025901
[44] DOI: 10.1103/PhysRevD.77.064013 · doi:10.1103/PhysRevD.77.064013
[45] DOI: 10.1016/j.physletb.2010.06.019 · doi:10.1016/j.physletb.2010.06.019
[46] Karami K., JHEP 03 pp 086–
[47] DOI: 10.1103/PhysRevD.81.083523 · doi:10.1103/PhysRevD.81.083523
[48] DOI: 10.1103/PhysRevD.80.121302 · doi:10.1103/PhysRevD.80.121302
[49] DOI: 10.1142/S021827180600942X · Zbl 1203.83061 · doi:10.1142/S021827180600942X
[50] DOI: 10.1103/PhysRevD.66.021301 · doi:10.1103/PhysRevD.66.021301
[51] DOI: 10.1016/j.physletb.2003.09.065 · Zbl 1027.83526 · doi:10.1016/j.physletb.2003.09.065
[52] Sen A., JHEP 0204 pp 048–
[53] Sen A., JHEP 0207 pp 065–
[54] DOI: 10.1142/S0217732302008071 · Zbl 1083.81578 · doi:10.1142/S0217732302008071
[55] Sen A., JHEP 9910 pp 008–
[56] Bergshoeff E. A., JHEP 0005 pp 009–
[57] DOI: 10.1103/PhysRevD.62.126003 · doi:10.1103/PhysRevD.62.126003
[58] DOI: 10.1016/S0550-3213(03)00498-X · Zbl 1057.81547 · doi:10.1016/S0550-3213(03)00498-X
[59] DOI: 10.1016/S0370-2693(99)00603-6 · Zbl 0992.83096 · doi:10.1016/S0370-2693(99)00603-6
[60] Piazza F., J. Cosmol. Astropart. Phys. 0407 pp 004–
This reference list is based on information provided by the publisher or from digital mathematics libraries. Its items are heuristically matched to zbMATH identifiers and may contain data conversion errors. In some cases that data have been complemented/enhanced by data from zbMATH Open. This attempts to reflect the references listed in the original paper as accurately as possible without claiming completeness or a perfect matching.