Hall magnetohydrodynamics of partially ionized plasmas     

B. P. Pandey  Mark Wardle 《Monthly notices of the Royal Astronomical Society》2008,385(4):2269-2278

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Radiative bubbles blown by slow stellar winds     

Christopher D. Matzner  Ruben Krasnopolsky 《Monthly notices of the Royal Astronomical Society》2008,386(2):903-908

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Molecular line mapping of the giant molecular cloud associated with RCW 106 – II. Column density and dynamical state of the clumps     

T. Wong  E. F. Ladd  D. Brisbin  M. G. Burton  I. Bains  M. R. Cunningham  N. Lo  P. A. Jones  K. L. Thomas  S. N. Longmore  A. Vigan  B. Mookerjea  C. Kramer  Y. Fukui  A. Kawamura 《Monthly notices of the Royal Astronomical Society》2008,386(2):1069-1084

We present a fully sampled C¹⁸O (1–0) map towards the southern giant molecular cloud (GMC) associated with the H  ii region RCW 106, and use it in combination with previous ¹³CO (1–0) mapping to estimate the gas column density as a function of position and velocity. We find localized regions of significant ¹³CO optical depth in the northern part of the cloud, with several of the high-opacity clouds in this region likely associated with a limb-brightened shell around the H  ii region G333.6−0.2. Optical depth corrections broaden the distribution of column densities in the cloud, yielding a lognormal distribution as predicted by simulations of turbulence. Decomposing the ¹³CO and C¹⁸O data cubes into clumps, we find relatively weak correlations between size and linewidth, and a more sensitive dependence of luminosity on size than would be predicted by a constant average column density. The clump mass spectrum has a slope near −1.7, consistent with previous studies. The most massive clumps appear to have gravitational binding energies well in excess of virial equilibrium; we discuss possible explanations, which include magnetic support and neglect of time-varying surface terms in the virial theorem. Unlike molecular clouds as a whole, the clumps within the RCW 106 GMC, while elongated, appear to show random orientations with respect to the Galactic plane.  相似文献   

Formation and evolution of W Ursa Majoris stars: fallacies and corrections     

Z. Eker  O. Demircan  S. Bilir 《Monthly notices of the Royal Astronomical Society》2008,386(3):1756-1758

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Environment and mass dependencies of galactic λ spin parameter: cosmological simulations and observed galaxies compared     

B. Cervantes-Sodi  X. Hernandez  Changbom Park  Juhan Kim 《Monthly notices of the Royal Astronomical Society》2008,388(2):863-872

We use a sample of galaxies from the Sloan Digital Sky Survey (SDSS) to search for correlations between the λ spin parameter and the environment and mass of galaxies. In order to calculate the total value of λ for each observed galaxy, we employed a simple model of the dynamical structure of the galaxies, which allows a rough estimate of the value of λ using only readily obtainable observables from the luminous galaxies. Use of a large volume-limited sample (upwards of 11 000) allows reliable inferences of mean values and dispersions of λ distributions. We find, in agreement with some N -body cosmological simulations, no significant dependence of λ on the environmental density of the galaxies. For the case of mass, our results show a marked correlation with λ, in the sense that low-mass galaxies present both higher mean values of λ and associated dispersions, than high-mass galaxies. These results provide interesting constrain on the mechanisms of galaxy formation and acquisition of angular momentum, a valuable test for cosmological models.  相似文献   

Molecular line profiles as diagnostics of protostellar collapse: modelling the 'blue asymmetry' in inside-out infall     

Y. G. Tsamis  J. M. C. Rawlings  J. A. Yates  S. Viti 《Monthly notices of the Royal Astronomical Society》2008,388(2):898-912

The evolution of star-forming core analogues undergoing inside-out collapse is studied with a multipoint chemodynamical model which self-consistently computes the abundance distribution of chemical species in the core. For several collapse periods the output chemistry of infalling tracer species such as HCO⁺, CS and N₂H⁺ is then coupled to an accelerated Λ-iteration radiative transfer code, which predicts the emerging molecular line profiles using two different input gas/dust temperature distributions. We investigate the sensitivity of the predicted spectral line profiles and line asymmetry ratios to the core temperature distribution, the time-dependent model chemistry, as well as to ad hoc abundance distributions. The line asymmetry is found to be strongly dependent on the adopted chemical abundance distribution. In general, models with a warm central region show higher values of blue asymmetry in optically thick HCO⁺ and CS lines than models with a starless core temperature profile. We find that in the formal context of Shu-type inside-out infall, and in the absence of rotation or outflows, the relative blue asymmetry of certain HCO⁺ and CS transitions is a function of time and, subject to the foregoing caveats, can act as a collapse chronometer. The sensitivity of simulated HCO⁺ line profiles to linear radial variations, subsonic or supersonic, of the internal turbulence field is investigated in the separate case of static cores.  相似文献   

Is AGN feedback necessary to form red elliptical galaxies?     

A. Khalatyan  A. Cattaneo  M. Schramm  S. Gottlöber  M. Steinmetz  L. Wisotzki 《Monthly notices of the Royal Astronomical Society》2008,387(1):13-30

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The first galaxies: assembly, cooling and the onset of turbulence     

Thomas H. Greif †  Jarrett L. Johnson  Ralf S. Klessen  Volker Bromm 《Monthly notices of the Royal Astronomical Society》2008,387(3):1021-1036

We investigate the properties of the first galaxies at   z ≳ 10  with highly resolved numerical simulations, starting from cosmological initial conditions and taking into account all relevant primordial chemistry and cooling. A first galaxy is characterized by the onset of atomic hydrogen cooling, once the virial temperature exceeds  ≃10⁴ K  , and its ability to retain photoheated gas. We follow the complex accretion and star formation history of a  ≃5 × 10⁷ M_⊙  system by means of a detailed merger tree and derive an upper limit on the number of Population III (Pop III) stars formed prior to its assembly. We investigate the thermal and chemical evolution of infalling gas and find that partial ionization at temperatures  ≳10⁴ K  catalyses the formation of  H₂  and hydrogen deuteride, allowing the gas to cool to the temperature of the cosmic microwave background. Depending on the strength of radiative and chemical feedback, primordial star formation might be dominated by intermediate-mass Pop III stars formed during the assembly of the first galaxies. Accretion on to the nascent galaxy begins with hot accretion, where gas is accreted directly from the intergalactic medium and shock heated to the virial temperature, but is quickly accompanied by a phase of cold accretion, where the gas cools in filaments before flowing into the parent halo with high velocities. The latter drives supersonic turbulence at the centre of the galaxy and could lead to very efficient chemical mixing. The onset of turbulence in the first galaxies thus likely marks the transition to Pop II star formation.  相似文献   

Magnetorotational instability in protoplanetary discs: the effect of dust grains     

Raquel Salmeron  Mark Wardle 《Monthly notices of the Royal Astronomical Society》2008,388(3):1223-1238

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Testing the evolutionary link between submillimetre galaxies and quasars: CO observations of QSOs at z∼ 2     

K. E. K. Coppin  A. M. Swinbank  R. Neri  P. Cox  D. M. Alexander  Ian Smail  M. J. Page  J. A. Stevens  K. K. Knudsen  R. J. Ivison  A. Beelen  F. Bertoldi  A. Omont 《Monthly notices of the Royal Astronomical Society》2008,389(1):45-62

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