Probing the QCD critical point by higher moments of net-proton multiplicity distributions at STAR

• Authors: Xiaofeng Luo
• Languages of publication: EN

Abstracts

EN

Higher moments (kurtosis (κ), skewness (S) and variance (σ
2)) of multiplicity distributions are sensitive to the correlation length and can be used to search for the QCD critical point. The moment products κσ
2 and S
σ of net-proton distributions, which are also related to volume independent baryon number susceptibility ratios, can be compared with Lattice QCD and Hadron Resonance Gas (HRG) model calculations. We discuss the recent progress in the higher moments analysis of net-protons multiplicity distributions.

Keywords

EN

QCD critical point; higher moments; net-proton; QGP; heavy ion collisions

• Publisher: De Gruyter Open
• Journal: Open Physics
• Year: 2012
• Volume: 10
• Issue: 6
• Pages: 1372-1374

Dates

published

1 - 12 - 2012

online

4 - 12 - 2012

Contributors

author

Xiaofeng Luo

References

• [1] R. V. Gavai, S. Gupta, Phys. Rev. D 78, 114503 (2008) http://dx.doi.org/10.1103/PhysRevD.78.114503[Crossref]
• [2] M. A. Stephanov, Phys. Rev. Lett. 102, 032301 (2009) http://dx.doi.org/10.1103/PhysRevLett.102.032301[Crossref]
• [3] C. Athanasiou et al., Phys. Rev. D 82 074008 (2010) http://dx.doi.org/10.1103/PhysRevD.82.074008
• [4] R. V. Gavai, S. Gupta, Phys. Lett. B 696, 459 (2011) http://dx.doi.org/10.1016/j.physletb.2011.01.006[Crossref]
• [5] M. Cheng et al., Phys. Rev. D 79, 074505 (2009) http://dx.doi.org/10.1103/PhysRevD.79.074505[Crossref]
• [6] F. Karsch, Cent. Eur. J. Phys., DOI:10.2478/s11534-012-0074-3 [Crossref]
• [7] F. Karsch, K. Redlich, Phys. Lett. B 695, 136 (2011) http://dx.doi.org/10.1016/j.physletb.2010.10.046[Crossref]
• [8] K. Redlich, Cent. Eur. J. Phys., DOI:10.2478/s11534-012-0105-0 [Crossref]
• [9] Y. Hatta, M. A. Stephanov, Phys. Rev. Lett. 91, 102003 (2003) http://dx.doi.org/10.1103/PhysRevLett.91.102003[Crossref]
• [10] X. Luo (for the STAR Collaboration), Acta Phys. Pol. B Proc. Sup. 5, 497 (2012) http://dx.doi.org/10.5506/APhysPolBSupp.5.497[Crossref]
• [11] X. Luo (for the STAR Collaboration), J. Phys. Conf. Ser. 316, 012003 (2011) http://dx.doi.org/10.1088/1742-6596/316/1/012003[Crossref]
• [12] S. Gupta, X. Luo, B. Mohanty, H. G. Ritter, N. Xu, Science 332, 1525 (2011) http://dx.doi.org/10.1126/science.1204621[Crossref]
• [13] X. Luo et al., J. Phys. G Nucl. Part. Phys. 37, 094061 (2010) http://dx.doi.org/10.1088/0954-3899/37/9/094061[Crossref]
• [14] M. M. Aggarwal et al. (STAR Collaboration), Phys. Rev. Lett. 105, 022302 (2010) http://dx.doi.org/10.1103/PhysRevLett.105.022302[Crossref]
• [15] Z. W. Lin et al., Phys. Rev. C 72, 064901 (2005)
• [16] X. Luo et al., Phys. Atom. Nucl. 75, 676 (2012) http://dx.doi.org/10.1134/S1063778812060348[Crossref]
• [17] X. Luo, J. Phys. G Nucl. Part. Phys. 39, 025008 (2012) http://dx.doi.org/10.1088/0954-3899/39/2/025008[Crossref]
• [18] M. A. Stephanov, Phys. Rev. Lett. 107, 052301 (2011) http://dx.doi.org/10.1103/PhysRevLett.107.052301[Crossref]
• [19] B. Friman et al., Eur. Phys. J. C 71, 1694 (2011) http://dx.doi.org/10.1140/epjc/s10052-011-1694-2[Crossref]

Identifiers

DOI

10.2478/s11534-012-0080-5