Gamma ray emission and stochastic particle acceleration in galaxy clustersFERMI (formely GLAST) will shortly provide crucial information on relativistic particles in galaxy clusters. We discuss non-thermal emission in the context of general calculations in which…G. Brunetti, P. Blasi, R. Cassano et al.·Nov 6, 2008SaveLearn
On the opacity change required to compensate for the revised solar compositionRecent revisions of the determination of the solar composition have resulted in solar models in marked disagreement with helioseismic inferences. The effect of the composition change on the model is…Jørgen Christensen-Dalsgaard, Maria Pia Di Mauro, Günter Houdek et al.·Nov 6, 2008SaveLearn
Hunting for Magnetars in High Mass X-ray Binaries. The Case of SuperGiant Fast X-Ray TransientsIn this paper we summarize some aspects of the wind accretion theory in high mass X-ray binaries hosting a magnetic neutron star and a supergiant companion. In particular, we concentrate on the…E. Bozzo, M. Falanga, L. Stella·Nov 6, 2008SaveLearn
Probing the complex environments of GRB host galaxies and intervening systems: high resolution spectroscopy of GRB050922CThe aim of this paper is to investigate the environment of gamma ray bursts (GRBs) and the interstellar matter of their host galaxies. We use to this purpose high resolution spectroscopic…S. Piranomonte, P. A. Ward, F. Fiore et al.·Nov 6, 2008SaveLearn
INTEGRAL and XMM-Newton observations of AX J1845.0-0433AX J1845.0-0433 is a transient high-mass X-ray binary discovered by ASCA. The source displays bright and short flares observed recently with INTEGRAL. The transient behaviour and the bright and short…J. A. Zurita Heras, R. Walter·Nov 6, 2008SaveLearn
Studying the properties of the radio emitter in LS 5039LS 5039 is an X-ray binary that presents non-thermal radio emission. The radiation at 5 GHz is quite steady and optically thin, consisting on a dominant core plus an extended jet-like…V. Bosch-Ramon·Nov 6, 2008SaveLearn
The accretion powered spin-up of GRO J1750-27The timing properties of the 4.45 s pulsar in the Be X-ray binary system GRO J1750-27 are examined using hard X-ray data from INTEGRAL and Swift during a Type II outburst observed during 2008. The…S. E. Shaw, A. B. Hill, E. Kuulkers et al.·Nov 6, 2008SaveLearn
Very High Energy Gamma-Ray Observations of the Galactic Centre RegionRecent progress in pushing the sensitivity of the Imaging Atmospheric Cherenkov Technique into the 10 mCrab regime has enabled first sensitive observations of the innermost few 100 pc of the Milky…Christopher van Eldik·Nov 6, 2008SaveLearn
SMA CO(J=6-5) and 435 micron interferometric imaging of the nuclear region of Arp 220We have used the Submillimeter Array (SMA) to make the first interferometric observations (beam size ~1") of the 12CO J=6-5 line and 435 micron (690 GHz) continuum emission toward the central…Satoki Matsushita, Daisuke Iono, Glen R. Petitpas et al.·Nov 6, 2008SaveLearn
The Stromlo Missing Satellites SurveyThe Stromlo Missing Satellites (SMS) program is a critical endeavor to investigate whether cold dark matter cosmology is flawed in its ability to describe the matter distribution on galaxy scales or…Helmut Jerjen·Nov 6, 2008SaveLearn
A parameter study of self-consistent disk models around Herbig AeBe starsWe present a parameter study of self-consistent models of protoplanetary disks around Herbig AeBe stars. We use the code developed by Dullemond and Dominik, which solves the 2D radiative transfer…J. Meijer, C. Dominik, A. de Koter et al.·Nov 6, 2008SaveLearn
INTEGRAL monitoring of unusually long X-ray burstsX-ray bursts are thermonuclear explosions on the surface of accreting neutron stars in low mass X-ray binaries. As most of the known X-ray bursters are frequently observed by INTEGRAL, an…J. Chenevez, M. Falanga, E. Kuulkers et al.·Nov 6, 2008SaveLearn
Absorption Phenomena and a Probable Blast Wave in the 13 July 2004 Eruptive EventWe present a case study of the 13 July 2004 solar event, in which disturbances caused by eruption of a filament from an active region embraced a quarter of the visible solar surface. Remarkable are…V. V. Grechnev, A. M. Uralov, V. A. Slemzin et al.·Nov 6, 2008SaveLearn
55 Cancri: A Laboratory for Testing Numerous Conjectures about Planet FormationFive planets are presently believed to orbit the primary star of 55 Cnc, but there exists a large 5 AU gap in their distribution between the two outermost planets. This gap has attracted considerable…Dimitris M. Christodoulou, Demosthenes Kazanas·Nov 6, 2008SaveLearn
Mergers and Disk Survival in LCDMDisk galaxies are common in our universe and this is a source of concern for hierarchical formation models like LCDM. Here we investigate this issue as motivated by raw merger statistics derived for…James S. Bullock, Kyle R. Stewart, Chris W. Purcell·Nov 6, 2008SaveLearn
High Accuracy Imaging Polarimetry with NICMOSThe ability of NICMOS to perform high accuracy polarimetry is currently hampered by an uncalibrated residual instrumental polarization at a level of 1.2-1.5%. To better quantify and characterize this…D. Batcheldor, G. Schneider, D. C. Hines et al.·Nov 6, 2008SaveLearn
Obtaining Spectra of Turbulent Velocity from ObservationsWe discuss a long-standing problem of how turbulence can be studied using observations of Doppler broadened emission and absorption lines. The focus of the present review is on two new techniques,…A. Lazarian·Nov 6, 2008SaveLearn
Turbulence Spectra from Doppler-broadened Spectral Lines: Tests of the Velocity Channel Analysis and Velocity Coordinate Spectrum TechniquesTurbulent motions induce Doppler shifts of observable emission and absorption lines motivating studies of turbulence using precision spectroscopy. We provide the numerical testing of the two most…A. Chrupnov, A. Lazarian·Nov 5, 2008SaveLearn
The Effective Theory of Quintessence: the w<-1 Side UnveiledWe study generic single-field dark energy models, by a parametrization of the most general theory of their perturbations around a given background, including higher derivative terms. In appropriate…Paolo Creminelli, Guido D'Amico, Jorge Noreña et al.·Nov 5, 2008SaveLearn
Accurate universal models for the mass accretion histories and concentrations of dark matter halosA large amount of observations have constrained cosmological parameters and the initial density fluctuation spectrum to a very high accuracy. However, cosmological parameters change with time and the…D. H. Zhao, Y. P. Jing, H. J. Mo et al.·Nov 5, 2008SaveLearn
Chandra measurements of non-thermal-like X-ray emission from massive, merging, radio-halo clustersWe report the discovery of spatially-extended, non-thermal-like emission components in Chandra X-ray spectra for five of a sample of seven massive, merging galaxy clusters with powerful radio halos.…E. T. Million, S. W. Allen·Nov 5, 2008SaveLearn
LISA parameter estimation using numerical merger waveformsRecent advances in numerical relativity provide a detailed description of the waveforms of coalescing massive black hole binaries (MBHBs), expected to be the strongest detectable LISA sources. We…J. I. Thorpe, S. T. McWilliams, B. J. Kelly et al.·Nov 5, 2008SaveLearn
Properties and selected implications of magnetic turbulence for interstellar medium, Local Bubble and solar windAstrophysical fluids, including interstellar and interplanetary medium, are magnetized and turbulent. Their appearance, evolution, and overall properties are determined by the magnetic turbulence…A. Lazarian, A. Beresnyak, H. Yan et al.·Nov 5, 2008SaveLearn
On the solar nickel and oxygen abundancesDeterminations of the solar oxygen content relying on the neutral forbidden transition at 630 nm depend upon the nickel abundance, due to a Ni I blend. Here we rederive the solar nickel abundance,…Pat Scott, Martin Asplund, Nicolas Grevesse et al.·Nov 5, 2008SaveLearn
Accretion onto the First Stellar Mass Black HolesThe first stars in the universe, forming at redshifts z>15 in minihalos with masses of order 106 Msun, may leave behind black holes as their remnants. These objects could conceivably serve as…Marcelo A. Alvarez, John H. Wise, Tom Abel·Nov 5, 2008SaveLearn