Heavy Quark Interactions in Finite Temperature QCD

We study the free energy of a heavy quark-antiquark pair in a thermal medium. We constuct a simple ansatz for the free energy for two quark flavors motivated by the Debye-H\"uckel theory of screening.Comment: 4 pages, 4 figures, contribution to the proceedings of the International Conference on Hard and Electromagnetic Probes of High Energy Nuclear Collisions, Ericeira, Portugal, Nov. 4-10, 200

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Gross anatomical features of the brachial plexus of a Pacific white-sided dolphin (Lagenorhynchus obliquidens)

Journal Articleカマイルカの頚椎と腕神経叢を肉眼解剖学的に検討した。7個の頚椎のうち、環椎と軸椎はほぼ完全に融合していたが、第3頚椎以下は分離したままであった。腕神経叢は第3-8頚神経（C3-C8）および第1胸神経（T1）から構成された。これらの7本の神経根が合流しあい、左側で3本、右側で4本の神経幹となった。これらの神経幹が合して、一本の背腹に扁平な帯状の神経束となり、腋窩に達した後、上肢帯筋の筋枝と胸びれの神経を放射状に分岐した。 横隔神経と肩甲上神経は、腕神経叢の頭側縁から分岐した。胸筋神経は神経束の腹側面から分岐した。神経叢の背側面からは、肩甲下神経、腋窩神経、橈骨神経、大円筋枝と広背筋枝が分岐した。正中神経と尺骨神経は共同幹をなし、前腕で多数の皮枝を分岐したのち、掌側指神経となった。この共同幹の近位部から、筋皮神経と思われる枝が分岐した。costo-coracoid筋（小胸筋）には胸筋神経と横隔神経からの枝、あるいは腕神経叢から直接分岐した枝が分布していた。頚部の短縮にともなって、腕神経叢を構成する脊髄神経の分節数が増加することがうかがえた。We observed the cervical vertebrae of a Pacific white-sided dolphin, and examined gross anatomically the brachial plexus of a specimen stranded at Toyama bay in 2003. The atlas and the axis were fused into one unit. The rest of the cervical vertebrae were free. The brachial plexuses on both sides were formed by the union of the ventral rami of the lower six cervical nerves and the first thoracic nerve. These roots fused with each other to form three trunks on the left side and four trunks on the right side. On both sides, these trunks fused into one band-shaped fascicle. At the axilla, the fascicle radially gave off many nerve branches. The phrenic nerve and the suprascapular nerve arose from the cranial margin of the plexus. The pectoral nerves arose from the ventral surface of the brachial plexus. In contrast, the subscapular, the axillar, the radial, and the thoracodorsal nerves arose in turn from the dorsal surface of the brachial plexus. The median and ulnar nerves reached the forearm as a common trunk and gave off many cutaneous branches for the skin of the palmar surface of the flipper, and terminated as the palmar digital nerves. The costo-coracoid muscle was innervated by branches from the pectoral nerve and the phrenic nerve and, on occasion, a branch divided directly from the brachial plexus. The present study and a survey of the literature suggest that the more compressed in length the cervical vertebrae, the greater the increase in number of the ventral rami of the spinal nerves which form the brachial plexus.journal articl

Non-abelian color dielectric - towards the effective model of the low energy QCD

Lattice motivated triplet color scalar field theory is analyzed. We consider non-minimal as well as covariant derivative coupling with SU(2) gauge fields. Field configurations generated by external electric sources are presented. Moreover non-Abelian magnetic monopoles are found. Dependence on the spatial coordinates in the obtained solutions is identical as in the usual Abelian case. We show also that after a decomposition of the fields a modified Faddeev-Niemi action can be obtained. It contains explicit O(3) symmetry breaking term parameterized by the condensate of an isoscalar field. Due to that Goldstone bosons observed in the original Faddeev-Niemi model are removed.Comment: 19 page

The VLT-FLAMES survey of massive stars: Wind properties and evolution of hot massive stars in the LMC

[Abridged] We have studied the optical spectra of 28 O- and early B-type stars in the Large Magellanic Cloud, 22 of which are associated with the young star-forming region N11. Stellar parameters are determined using an automated fitting method, combining the stellar atmosphere code FASTWIND with the genetic-algorithm optimisation routine PIKAIA. Results for stars in the LH9 and LH10 associations of N11 are consistent with a sequential star formation scenario, in which activity in LH9 triggered the formation of LH10. Our sample contains four stars of spectral type O2, of which the hottest is found to be ~49-54 kK (cf. ~45-46 kK for O3 stars). The masses of helium-enriched dwarfs and giants are systematically lower than those implied by non-rotating evolutionary tracks. We interpret this as evidence for efficient rotationally-enhanced mixing, leading to the surfacing of primary helium and to an increase of the stellar luminosity. This result is consistent with findings for SMC stars by Mokiem et al. For bright giants and supergiants no such mass-discrepancy is found, implying that these stars follow tracks of modestly (or non-)rotating objects. Stellar mass-loss properties were found to be intermediate to those found in massive stars in the Galaxy and the SMC, and comparisons with theoretical predictions at LMC metallicity yielded good agreement over the luminosity range of our targets, i.e. 5.0 < log L/L(sun) < 6.1