KS0, Λ and ≡ production at intermediate to high pT from Au+Au collisions at $\sqrt {s_{NN} } $ = 39, 11.5 and 7.7 GeV

• Authors: Xianglei Zhu
• Languages of publication: EN

Abstracts

EN

We report on the p
T dependence of nuclear modification factors (R
CP) for KS0, Λ, ≡ and the $\bar NK_S^0 $ ratios at mid-rapidity from Au+Au collisions at $\sqrt {s_{NN} } $ = 39, 11.5 and 7.7 GeV. At $\sqrt {s_{NN} } $ = 39 GeV, the R
CP data show a baryon/meson separation at intermediate p
T and a suppression for KS0 for p
T up to 4.5 GeV/c; the $\bar \Lambda K_S^0 $ shows baryon enhancement in the most central collisions. However, at $\sqrt {s_{NN} } $ = 11.5 and 7.7 GeV, R
CP shows less baryon/meson separation and $\bar NK_S^0 $ shows almost no baryon enhancement. These observations indicate that the matter created in Au+Au collisions at $\sqrt {s_{NN} } $ = 11.5 or 7.7 GeV might be distinct from that created at $\sqrt {s_{NN} } $ = 39 GeV.

Keywords

EN

strangeness production; heavy ion collisions; QCD phase transition; onset of deconfinement

• Publisher: De Gruyter Open
• Journal: Open Physics
• Year: 2012
• Volume: 10
• Issue: 6
• Pages: 1345-1348

Dates

published

1 - 12 - 2012

online

4 - 12 - 2012

Contributors

author

Xianglei Zhu

• Department of Engineering Physics, Tsinghua University, Beijing, 100084, China

References

• [1] M. A. C. Lamont (for the STAR Collaboration), J. Phys. Conf. Ser. 50, 192 (2006) http://dx.doi.org/10.1088/1742-6596/50/1/022[Crossref]
• [2] C. Alt et al. (NA49 Collaboration), Phys. Rev. C 77, 034906 (2008) http://dx.doi.org/10.1103/PhysRevC.77.034906[Crossref]
• [3] M. M. Aggarwal et al. (WA98 Collaboration), Phys. Rev. Lett. 100, 242301 (2008) http://dx.doi.org/10.1103/PhysRevLett.100.242301[Crossref]
• [4] M. M. Aggarwal et al. (STAR Collaboration), arXiv:1007.2613
• [5] K. Adcox et al. (PHENIX Collaboration), Phys. Rev. C 69, 024904 (2004) http://dx.doi.org/10.1103/PhysRevC.69.024904[Crossref]
• [6] B. I. Abelev et al. (STAR Collaboration), Phys. Lett. B 655, 104 (2007) http://dx.doi.org/10.1016/j.physletb.2007.06.035[Crossref]
• [7] B. I. Abelev et al. (STAR Collaboration), Phys. Rev. Lett. 97, 152301 (2006) http://dx.doi.org/10.1103/PhysRevLett.97.152301[Crossref]
• [8] R. C. Hwa, C. B. Yang, Phys. Rev. C 66, 025205 (2002) http://dx.doi.org/10.1103/PhysRevC.66.025205[Crossref]
• [9] V. Greco, C. M. Ko, P. Levai, Phys. Rev. Lett. 90, 202302 (2003) http://dx.doi.org/10.1103/PhysRevLett.90.202302[Crossref]
• [10] R. J. Fries, B. Muller, C. Nonaka, S. A. Bass, Phys. Rev. Lett. 90, 202303 (2003) http://dx.doi.org/10.1103/PhysRevLett.90.202303[Crossref]
• [11] D. Molnar, S. A. Voloshin, Phys. Rev. Lett. 91, 092301 (2003) http://dx.doi.org/10.1103/PhysRevLett.91.092301[Crossref]
• [12] X. Zhu (for the STAR Collaboration), Acta Phys. Pol. B Proc. Sup. 5, 213 (2012) http://dx.doi.org/10.5506/APhysPolBSupp.5.213[Crossref]
• [13] J. W. Cronin et al., Phys. Rev. D 11, 3105 (1975) http://dx.doi.org/10.1103/PhysRevD.11.3105[Crossref]
• [14] B. Hippolyte (for the ALICE Collaboration), Acta Phys. Pol. B 43, 645 (2012) http://dx.doi.org/10.5506/APhysPolB.43.645[Crossref]

Identifiers

DOI

10.2478/s11534-012-0102-3