Within the recent paper by E. Verlinde, hep-th/0008140, an incredible formula remains submit, which relates the entropy in the conformal formal field in arbitrary dimensions for the total energy and Casimir energy. This formula remains proven to hold for the conformal field theories which have antide Sitter (AdS) duals within the cases of AdS Schwarzschild black holes and AdS Kerr black holes. During this paper we further take a look formula with a few other black holes with AdS asymptotics. For the hyperbolic AdS black holes, the Cardy-Verlinde formula can be found to carry once we choose the ’’massless’’ black holemore because the ground condition, however in this case, the Casimir energy is negative. For the AdS Reissner-Nordstro’’m black holes in arbitrary dimensions and billed black holes in D&#615, D&#614, and D&#617 maximally supersymmetric gauged supergravities, the Cardy-Verlinde formula holds too, however a highly effective internal energy, which inserts the mass of supersymmetric backgrounds, needs to be subtracted inside the total energy. We do not rewrite the entropy of corresponding conformal field theories based on the Cardy-Verlinde formula for the AdS black holes in Lovelock gravity. less

June 2001. The American Physical Society

Hu, Jian-Wei Cai, Rong-Gen Guo, Zong-Kuan Hu, Bin, E-mail: jwhu@itp.ac.cn, E-mail: cairg@itp.ac.cn, E-mail: guozk@itp.ac.cn, E-mail: hu@lorentz.leidenuniv.nl

We investigate constraints on cosmological parameters in three 8-parameter models while using the summed neutrino mass as being a free parameter, getting some pot analysis of CCCP X-ray cluster data, the recently released Planck CMB data and many exterior data sets including baryon acoustic oscillation measurements inside the 6dFGS, SDSS DR7 and BOSS DR9 surveys, and Hubble Space Telescope H measurement.

We identify the combined data strongly favor a non-zero neutrino masses at greater than 3 amount of confidence of these non-vanilla models. Allowing the CMB lensing amplitude A to alter, we uncover A 1 atmore 3 amount of confidence. For dark energy obtaining a ongoing equation of condition w, we have w 1 at 3 amount of confidence. The estimate within the matter power spectrum amplitude is discrepant while using the Planck value at 2 amount of confidence, which reflects some tension between X-ray cluster data and Planck data of these non-vanilla models. The strain may be alleviated with the aid of a 9% systematic alternation in the cluster mass function. less

Cai, Rong-Gen Tuo, Zhong-Liang, E-mail: cairg@itp.ac.cn, E-mail: tuozhl@itp.ac.cn

During this paper we see the possibly existing anisotropy within the speeding up expansion World by technique full sample of Union2 data. When using the hemisphere comparison approach to think about a regular direction, we make deceleration parameter q because the diagnostic to evaluate the anisotropy level within the wCDM model. We identify the utmost speeding up expansion direction is (l,b) &#61 (314deg ,28deg ), while using the maximum anisotropy quantity of q/ q-bar &#61 .79, the anisotropy is much more prominent when only low redshift data (z more .2) are utilized.

We discuss this trouble inside the CPL parameterized model, showing exactly the same result. less

Gong, Yungui Wang, Bin Cai, Rong-Gen, E-mail: gongyg@cqupt.edu.cn, E-mail: wangb@fudan.edu.cn, E-mail: cairg@itp.ac.cn

We examine inside a couple of detail the influence within the systematics in a number of data sets including type Ia supernova sample, baryon acoustic oscillation data along with the cosmic microwave websites the fitting link between the Chevallier-Polarski-Linder parametrization. We identify the systematics within the data sets does influence the fitting leads to cause different evolutional behavior of dark energy. To discover the versatility of Chevallier-Polarski-Linder parametrization, we perform analysis across the Wetterich parametrization of dark energy. The outcome show both parametrization of dark energy along with the systematics in data sets influence the evolutional behavior ofmore dark energy. less

Cai, Rong-Gen Hu, Bin Zhang, Hong-Bo, E-mail: cairg@itp.ac.cn, E-mail: hubin@itp.ac.cn, E-mail: hbzhang@itp.ac.cn

When using the full radiation transfer function, we numerically calculate the CMB angular bispectrum seeded using the compensated magnetic scalar density mode. We uncover that, for the string inspired primordial magnetic fields characterised by index n &#61 2.9 and mean-field amplitude B &#61 9nG, the angular bispectrum is incorporated with two primordial magnetic shapes. The first magnetic shape looks like the one from local-type primordial curvature perturbations, so both amplitude and profile within the Komatsu-Spergel estimator (reduced bispectrum) seeded using this shape are virtually just like individuals however CMB anisotropies. However, for several parametermore sets (l,l), this ’’local-type’’ reduced bispectrum oscillates around different asymptotic values within the high-l regime due to the aftereffect in the Lorentz pressure, that’s exerted using the primordial magnetic fields across the billed baryons. This selection differs from the standard situation where all modes method of zero asymptotically within the high-l limit. However, the 2nd magnetic shape seems only within the primordial magnetic field model. The amplitude within the Komatsu-Spergel estimator sourced using the second shape diverges within the low-l regime due to the negative slope of shape. Within the high-l regime, this amplitude is roughly much like individuals from the very first estimator, though a reversal phase. less

Cai, Rong-Gen Su, Qiping Zhang, Hong-Bo, E-mail: cairg@itp.ac.cn, E-mail: sqp@itp.ac.cn, E-mail: hbzhang@itp.ac.cn

We investigate dynamical behavior within the equation of condition of dark energy w while using straight line-spline method around low redshifts from observational data (SnIa, BAO, CMB and 12 H(z) data). The redshift is binned and w is approximated getting an upright line growth and development of redshift in every single bin. We leave the divided points of redshift bins as free parameters within the model, the very best-fitted values of divided points will represent the turning positions of w where w changes its evolving direction considerably (if there is such turnings within our considered region). These turningmore points are natural divided points of redshift bins, and w between two nearby divided points may be well approximated getting an upright line growth and development of redshift. We uncover two turning points of w in z component of (,1.8) the other level in z component of (,.9), and w(z) might be oscillating around w &#61 1. Additionally, we uncover that you’ve a couple deviation of w from around z &#61 .9 in correlated and uncorrelated estimates. less

Gong, Yungui Cai, Rong-Gen Chen, Yun Zhu, Zong-Hong, E-mail: gongyg@cqupt.edu.cn, E-mail: cairg@itp.ac.cn, E-mail: chenyun@mail.bnu.edu.cn, E-mail: zhuzh@bnu.edu.cn

We make use of the Metabolic process supernova, the baryon acoustic oscillation, the cosmic microwave background, along with the Hubble parameter data to evaluate the evolution property of dark energy. We have spun sentences after we fit different baryon acoustic oscillation data along with Metabolic process supernova data for that Chevallier-Polarski-Linder model. We identify the primary difference arises from the various values of . We fit the observational data for that model independent piecewise constant parametrization. Four redshift bins with limitations at z &#61 .22, .53, .85 and 1.8 were selected for the piecewise constant parametrization within the equation of condition parametermore w(z) of dark energy. We uncover no significant evidence for evolving w(z). Using the Hubble parameter, the constraint across the equation of condition parameter at high redshift continues to be enhanced by 70%. The marginalization within the nuisance parameter attached to the supernova distance modulus is discussed. less

Kim, Hyeong-Chan Cai, Rong-Gen

Rotating billed Gauss-Bonnet black hole solutions in greater dimensional (d4), asymptotically anti-de Sitter spacetime are acquired within the small angular momentum limit. The angular momentum, magnetic dipole moment, along with the gyromagnetic ratio within the black holes are calculated and apparently , the Gauss-Bonnet term does not have effect on the gyromagnetic ratio.