Spin exchange interaction with tunable range between graphene quantum dots

We study the spin exchange between two electrons localized in separate quantum dots in graphene. The electronic states in the conduction band are coupled indirectly by tunneling to a common continuum of delocalized states in the valence band. As a model, we use a two-impurity Anderson Hamiltonian which we subsequently transform into an effective spin Hamiltonian by way of a two-stage Schrieffer-Wolff transformation. We then compare our result to that from a Coqblin-Schrieffer approach as well as to fourth order perturbation theory.Comment: 8 pages, 3 figure

Simple Models for Turbulent Self-Regulation in Galaxy Disks

We propose that turbulent heating, wave pressure and gas exchanges between different regions of disks play a dominant role in determining the preferred, quasi-equilibrium, self-similar states of gas disks on large-scales. We present simple families of analytic, thermohydrodynamic models for these global states, which include terms for turbulent pressure and Reynolds stresses. Star formation rates, phase balances, and hydrodynamic forces are all tightly coupled and balanced. The models have stratified radial flows, with the cold gas slowly flowing inward in the midplane of the disk, and with the warm/hot phases that surround the midplane flowing outward. The models suggest a number of results that are in accord with observation, as well as some novel predictions, including the following. 1) The large-scale gas density and thermal phase distributions in galaxy disks can be explained as the result of turbulent heating and spatial couplings. 2) The turbulent pressures and stresses that drive radial outflows in the warm gas also allow a reduced circular velocity there. This effect was observed by Swaters, Sancisi and van der Hulst in NGC 891, a particularly turbulent edge-on disk. The models predict that the effect should be universal in such disks. 3) They suggest that a star formation rate like the phenomenological Schmidt Law is the natural result of global thermohydrodynamical balance, and may not obtain in disks far from equilibrium. (Abridged)Comment: 37 pages, 1 gif figure, accepted for publication in the Astrophysical Journa

Elliptic flow in Au+Au collisions at sqrt sNN = 130 GeV

Elliptic flow from nuclear collisions is a hadronic observable sensitive to the early stages of system evolution. We report first results on elliptic flow of charged particles at midrapidity in Au+Au collisions at sqrt[sNN] = 130 GeV using the STAR Time Projection Chamber at the Relativistic Heavy Ion Collider. The elliptic flow signal, v2, averaged over transverse momentum, reaches values of about 6% for relatively peripheral collisions and decreases for the more central collisions. This can be interpreted as the observation of a higher degree of thermalization than at lower collision energies. Pseudorapidity and transverse momentum dependence of elliptic flow are also presented.alle Autoren: K. H. Ackermann19, N. Adams28, C. Adler12, Z. Ahammed27, S. Ahmad28, C. Allgower13, J. Amsbaugh34, M. Anderson6, E. Anderssen17, H. Arnesen3, L. Arnold14, G. S. Averichev10, A. Baldwin16, J. Balewski13, O. Barannikova10,27, L. S. Barnby16, J. Baudot14, M. Beddo1, S. Bekele24, V. V. Belaga10, R. Bellwied35, S. Bennett35, J. Bercovitz17, J. Berger12, W. Betts24, H. Bichsel34, F. Bieser17, L. C. Bland13, M. Bloomer17, C. O. Blyth4, J. Boehm17, B. E. Bonner28, D. Bonnet14, R. Bossingham17, M. Botlo3, A. Boucham30, N. Bouillo30, S. Bouvier30, K. Bradley17, F. P. Brady6, E. S. Braithwaite2, W. Braithwaite2, A. Brandin21, R. L. Brown3, G. Brugalette34, C. Byrd2, H. Caines24, M. Calderón de la Barca Sánchez36, A. Cardenas27, L. Carr34, J. Carroll17, J. Castillo30, B. Caylor17, D. Cebra6, S. Chatopadhyay35, M. L. Chen3, W. Chen3, Y. Chen7, S. P. Chernenko10, M. Cherney9, A. Chikanian36, B. Choi31, J. Chrin9, W. Christie3, J. P. Coffin14, L. Conin30, C. Consiglio3, T. M. Cormier35, J. G. Cramer34, H. J. Crawford5, V. I. Danilov10, D. Dayton3, M. DeMello28, W. S. Deng16, A. A. Derevschikov26, M. Dialinas30, H. Diaz3, P. A. DeYoung8, L. Didenko3, D. Dimassimo3, J. Dioguardi3, W. Dominik32, C. Drancourt30, J. E. Draper6, V. B. Dunin10, J. C. Dunlop36, V. Eckardt19, W. R. Edwards17, L. G. Efimov10, T. Eggert19, V. Emelianov21, J. Engelage5, G. Eppley28, B. Erazmus30, A. Etkin3, P. Fachini29, C. Feliciano3, D. Ferenc6, M. I. Ferguson7, H. Fessler19, E. Finch36, V. Fine3, Y. Fisyak3, D. Flierl12, I. Flores5, K. J. Foley3, D. Fritz17, N. Gagunashvili10, J. Gans36, M. Gazdzicki12, M. Germain14, F. Geurts28, V. Ghazikhanian7, C. Gojak14, J. Grabski33, O. Grachov35, M. Grau3, D. Greiner17, L. Greiner5, V. Grigoriev21, D. Grosnick1, J. Gross9, G. Guilloux30, E. Gushin21, J. Hall35, T. J. Hallman3, D. Hardtke17, G. Harper34, J. W. Harris36, P. He5, M. Heffner6, S. Heppelmann25, T. Herston27, D. Hill1, B. Hippolyte14, A. Hirsch27, E. Hjort27, G. W. Hoffmann31, M. Horsley36, M. Howe34, H. Z. Huang7, T. J. Humanic24, H. Hümmler19, W. Hunt13, J. Hunter17, G. J. Igo7, A. Ishihara31, Yu. I. Ivanshin11, P. Jacobs17, W. W. Jacobs13, S. Jacobson17, R. Jared17, P. Jensen31, I. Johnson17, P. G. Jones4, E. Judd5, M. Kaneta17, M. Kaplan8, D. Keane16, V. P. Kenney23*, A. Khodinov21, J. Klay6, S. R. Klein17, A. Klyachko13, G. Koehler17, A. S. Konstantinov26, V. Kormilitsyne7,26, L. Kotchenda21, I. Kotov24, A. D. Kovalenko10, M. Kramer22, P. Kravtsov21, K. Krueger1, T. Krupien3, P. Kuczewski3, C. Kuhn14, G. J. Kunde36, C. L. Kunz8, R. Kh. Kutuev11, A. A. Kuznetsov10, L. Lakehal-Ayat30, J. Lamas-Valverde28, M. A. C. Lamont4, J. M. Landgraf3, S. Lange12, C. P. Lansdell31, B. Lasiuk36, F. Laue24, A. Lebedev3, T. LeCompte1, W. J. Leonhardt3, V. M. Leontiev26, P. Leszczynski33, M. J. LeVine3, Q. Li35, Q. Li17, Z. Li3, C.-J. Liaw3, J. Lin9, S. J. Lindenbaum22, V. Lindenstruth5, P. J. Lindstrom5, M. A. Lisa24, H. Liu16, T. Ljubicic3, W. J. Llope28, G. LoCurto19, H. Long7, R. S. Longacre3, M. Lopez-Noriega24, D. Lopiano1, W. A. Love3, J. R. Lutz14, D. Lynn3, L. Madansky15§, R. Maier19, R. Majka36, A. Maliszewski33, S. Margetis16, K. Marks17, R. Marstaller19, L. Martin30, J. Marx17, H. S. Matis17, Yu. A. Matulenko26, E. A. Matyushevski10, C. McParland17, T. S. McShane9, J. Meier9, Yu. Melnick26, A. Meschanin26, P. Middlekamp3, N. Mikhalin7,26, B. Miller3, Z. Milosevich8, N. G. Minaev26, B. Minor17, J. Mitchell15, E. Mogavero3, V. A. Moiseenko11, D. Moltz17, C. F. Moore31, V. Morozov17, R. Morse17, M. M. de Moura29, M. G. Munhoz29, G. S. Mutchler28, J. M. Nelson4, P. Nevski3, T. Ngo7, M. Nguyen3, T. Nguyen3, V. A. Nikitin11, L. V. Nogach26, T. Noggle17, B. Norman16, S. B. Nurushev26, T. Nussbaum28, J. Nystrand17, G. Odyniec17, A. Ogawa25, C. A. Ogilvie18, K. Olchanski3, M. Oldenburg19, D. Olson17, G. A. Ososkov10, G. Ott31, D. Padrazo3, G. Paic24, S. U. Pandey35, Y. Panebratsev10, S. Y. Panitkin16, A. I. Pavlinov26, T. Pawlak33, M. Pentia10, V. Perevotchikov3, W. Peryt33, V. A Petrov11, W. Pinganaud30, S. Pirogov7, E. Platner28, J. Pluta33, I. Polk3, N. Porile27, J. Porter3, A. M. Poskanzer17, E. Potrebenikova10, D. Prindle34, C. Pruneau35, J. Puskar-Pasewicz13, G. Rai17, J. Rasson17, O. Ravel30, R. L. Ray31, S. V. Razin10,13, D. Reichhold9, J. Reid34, R. E. Renfordt12, F. Retiere30, A. Ridiger21, J. Riso35, H. G. Ritter17, J. B. Roberts28, D. Roehrich12, O. V. Rogachevski10, J. L. Romero6, C. Roy30, D. Russ8, V. Rykov35, I. Sakrejda17, R. Sanchez7, Z. Sandler7, J. Sandweiss36, P. Sappenfield28, A. C. Saulys3, I. Savin11, J. Schambach31, R. P. Scharenberg27, J. Scheblien3, R. Scheetz3, R. Schlueter17, N. Schmitz19, L. S. Schroeder17, M. Schulz3,19, A. Schüttauf19, J. Sedlmeir3, J. Seger9, D. Seliverstov21, J. Seyboth19, P. Seyboth19, R. Seymour34, E. I. Shakaliev10, K. E. Shestermanov26, Y. Shi7, S. S. Shimanskii10, D. Shuman17, V. S. Shvetcov11, G. Skoro10, N. Smirnov36, L. P. Smykov10, R. Snellings17, K. Solberg13, J. Sowinski13, H. M. Spinka1, B. Srivastava27, E. J. Stephenson13, R. Stock12, A. Stolpovsky35, N. Stone3, R. Stone17, M. Strikhanov21, B. Stringfellow27, H. Stroebele12, C. Struck12, A. A. P. Suaide29, E. Sugarbaker24, C. Suire14, T. J. M. Symons17, J. Takahashi29, A. H. Tang16, A. Tarchini14, J. Tarzian17, J. H. Thomas17, V. Tikhomirov21, A. Szanto de Toledo29, S. Tonse17, T. Trainor34, S. Trentalange7, M. Tokarev10, M. B. Tonjes20, V. Trofimov21, O. Tsai7, K. Turner3, T. Ullrich36, D. G. Underwood1, I. Vakula7, G. Van Buren3, A. M. VanderMolen20, A. Vanyashin17, I. M. Vasilevski11, A. N. Vasiliev26, S. E. Vigdor13, G. Visser5, S. A. Voloshin35, C. Vu17, F. Wang27, H. Ward31, D. Weerasundara34, R. Weidenbach17, R. Wells17, R. Wells24, T. Wenaus3, G. D. Westfall20, J. P. Whitfield8, C. Whitten, Jr.7, H. Wieman17, R. Willson24, K. Wilson35, J. Wirth17, J. Wisdom7, S. W. Wissink13, R. Witt16, J. Wolf17, L. Wood6, N. Xu17, Z. Xu36, A. E. Yakutin26, E. Yamamoto7, J. Yang7, P. Yepes28, A. Yokosawa1, V. I. Yurevich10, Y. V. Zanevski10, J. Zhang17, W. M. Zhang16, J. Zhu34, D. Zimmerman17, R. Zoulkarneev11, and A. N. Zubare

A Warp in Progress : H I and Radio Continuum Observations of the Spiral NGC 3145

Date of Acceptance: 16/06/2015We present VLA H I and 6 cm radio continuum observations of the spiral NGC 3145 and H I observations of its two companions, NGC 3143 and PGC 029578. In optical images NGC 3145 has stellar arms that appear to cross, forming "X"-features. Our radio continuum observations rule out shock fronts at 3 of the 4 "X"-features. In the middle-to-outer disk, the H I line-profiles of NGC 3145 are skewed. Relative to the disk, the gas in the skewed wing of the line-profiles has z-motions away from us on the approaching side of the galaxy and z-motions of about the same magnitude (about 40 km/s) towards us on the receding side. These warping motions imply that there has been a perturbation with a sizeable component perpendicular to the disk over large spatial scales. Two features in NGC 3145 have velocities indicating that they are out-of-plane tidal arms. One is an apparent branch of a main spiral arm; the velocity of the branch is 150 km/s greater than the spiral arm where they appear to intersect in projection. The other is an arm that forms 3 of the "X"-features. It differs in velocity by 56 km/s from the disk at the same projected location. Based on its SFR and H I properties, NGC 3143 is the more likely of the two companions to have interacted with NGC 3145 recently. A simple analytic model demonstrates that an encounter between NGC 3143 and NGC 3145 is a plausible explanation for the observed warping motions in NGC 3145.Peer reviewe

Peroxiredoxin 4, a novel circulating biomarker for oxidative stress and the risk of incident cardiovascular disease and all-cause mortality

BACKGROUND: Oxidative stress has been suggested to play a key role in the development of cardiovascular disease (CVD). The aim of our study was to investigate the associations of serum peroxiredoxin 4 (Prx4), a hydrogen peroxide-degrading peroxidase, with incident CVD and all-cause mortality. We subsequently examined the incremental value of Prx4 for the risk prediction of CVD compared with the Framingham risk score (FRS). METHODS AND RESULTS: We performed Cox regression analyses in 8141 participants without history of CVD (aged 28 to 75 years; women 52.6%) from the Prevention of Renal and Vascular End-stage Disease (PREVEND) study in Groningen, The Netherlands. Serum Prx4 was measured by an immunoluminometric assay in baseline samples. Main outcomes were: (1) incident CVD events or CVD mortality and (2) all-cause mortality during a median follow-up of 10.5 years. In total, 708 participants (7.8%) developed CVD events or CVD mortality, and 517 participants (6.3%) died. Baseline serum Prx4 levels were significantly higher in participants with incident CVD events or CVD mortality and in those who died than in participants who remained free of outcomes (both P<0.001). In multivariable models with adjustment for Framingham risk factors, hazard ratios were 1.16 (95% CI 1.06 to 1.27, P<0.001) for incident CVD events or CVD mortality and 1.17 (95% CI 1.06 to 1.29, P=0.003) for all-cause mortality per doubling of Prx4 levels. After the addition of Prx4 to the FRS, the net reclassification improvement was 2.7% (P=0.01) using 10-year risk categories of CVD. CONCLUSIONS: Elevated serum Prx4 levels are associated with a significantly higher risk of incident CVD events or CVD mortality and all-cause mortality after adjustment for clinical risk factors. The addition of Prx4 to the FRS marginally improved risk prediction of future CVD

The Minimum Stellar Mass in Early Galaxies

The conditions for the fragmentation of the baryonic component during merging of dark matter halos in the early Universe are studied. We assume that the baryonic component undergoes a shock compression. The characteristic masses of protostellar molecular clouds and the minimum masses of protostars formed in these clouds decrease with increasing halo mass. This may indicate that the initial stellar mass function in more massive galaxies was shifted towards lower masses during the initial stages of their formation. This would result in an increase of the number of stars per unit halo mass, i.e., the efficiency of star formation.Comment: 18 pages, 7 figure