ALBERT

Beschreibung: Author(s): L. X. Han (韩立欣), G. L. Ma (马国亮), Y. G. Ma (马余刚), X. Z. Cai (蔡翔舟), J. H. Chen (陈金辉), S. Zhang (张松), and C. Zhong (钟晨) [Phys. Rev. C 84, 064907] Published Tue Dec 06, 2011

Beschreibung: Author(s): L. X. Han (韩立欣), G. L. Ma (马国亮), Y. G. Ma (马余刚), X. Z. Cai (蔡翔舟), J. H. Chen (陈金辉), S. Zhang (张松), and C. Zhong (钟晨) A potential experimental probe, the forward-backward elliptic anisotropy correlation (C_{FB} ), has been proposed by Liao and Koch to distinguish the jet and true elliptic flow contribution to the measured elliptic flow (v_{2} ) in relativistic heavy-ion collisions. The jet and flow fluctuation cont... [Phys. Rev. C 83, 047901] Published Mon Apr 18, 2011

Beschreibung: Author(s): S. Zhang (张松), L. X. Han (韩立欣), Y. G. Ma (马余刚), J. H. Chen (陈金辉), and C. Zhong (钟晨) The particle production and their ratios for π, K, p, and Λ are studied in Pb + Pb collisions at sNN=2.76 TeV based on a blast-wave model with thermal equilibrium mechanism. The transverse momentum spectra of the above-mentioned particles at the kinetic freeze-out stage are discussed. The modificati... [Phys. Rev. C 89, 034918] Published Mon Mar 31, 2014

Beschreibung: We have monitored the evolution of the transient X-ray source GRO J0422+32 from approximately 2 weeks postdiscovery into its early decline phase at ultraviolet, optical, and radio wavelengths. Optical and ultraviolet spectra exhibit numerous, but relatively weak, high-excitation emission lines such as those arising from He II, N III, N V, and C IV superposed on an intrinsically blue continuum. High-resolution optical spectroscopy reveals line profiles which are double peaked, and in the case of the higher order Balmer lines, superposed on a broad absorption profile. The early outburst optical-ultraviolet continuum energy distribution is well represented by a two power-law fit with a break at approximately equal 4000 A. Radio observations with the Very Large Array (VLA) reveal a flat-spectrum source, slowly increasing in intensity at the earliest epochs observed, followed by an approximate power-law decay light curve with an index of -1. Light curves for each wavelength domain are presented and discussed. Notable are the multiple secondary outbursts seen in the optical more than 1 year postdiscovery, and spectral changes associated with secondary rises seen in the radio and UV. We find that the ultraviolet and optical characteristics of GRO J0422+32 as well as its radio evolution, are similar to other recent well-observed soft X-ray transients (also called X-ray novae) such as Cen X-4, A0620-00 (V616 Mon), and Nova Muscae 1991 (GS 1124-683), suggesting that GRO J0422+32 is also a member of that subclass of low-mass X-ray binaries. We present definitive astrometric determination of the source position, and place an upper limit of R approximately equals 20 from our analysis of the Palomar Observatory Sky Survey (POSS). Additionally, we derive distinct values for color excess from analysis of the optical (E(B-V) = 0.23) and ultraviolet (E(B-V) = 0.4) data, suggesting an intrinsic magnitude of 19-19.5 for the progenitor if it is mid-K dwarf. This leads to a likely range of 2.4-3.0 kpc for the source distance, which is consistent with our separate estimate of 2.4 +/- 0.4 kpc based on measurement of the NaD interstellar line profile. Adopting 2.4 kpc and E(B-V) = 0.23, the outburst absolute magnitude was M approximately equals 0.0, which is a typical value for this class of objects.

Beschreibung: On May 22, 1989, the Japanese Ginga Team discovered a new x ray source that was cataloged as GS 2023+338. This source was subsequently identified as coincident in position with a previously known nova cataloged as V404 Cygni. Its last recorded outburst was in 1938 when it rose to about 12th mag. Spectroscopic data were obtained and confirmed the nature of the outburst. Additional ground based data were obtained by us at CTIO and the VLA. The x ray behavior of this object was reported to be very unusual and it reached a peak of about 17 crab about one week after discovery. Since then it has varied widely in magnitude at all wavelengths at which it has been studied. A brief summary of the observations that were obtained up to the time of the meeting and shortly thereafter is presented.