Geomagnetism and Aeronomy, 2016, Vol. 56, № 7, pp. 1
... solar side, which is invisible from the Earth, will allow to better imagine three-dimensional structure of the solar magnetic field and the solar atmosphere. Precision local measurements in the inner heliosphere (within 1 AU) in and out of the ecliptic plane will allow to obtain new detailed informa ...
... solar side, which is invisible from the Earth, will allow to better imagine three-dimensional structure of the solar magnetic field and the solar atmosphere. Precision local measurements in the inner heliosphere (within 1 AU) in and out of the ecliptic plane will allow to obtain new detailed informa ...
The imprint of the crustal magnetic field on the thermal
... however, that 2D models have shown the importance of tangential heat conduction in limiting the anisotropy, compared with plane-parallel 1D models. The degree of anisotropy is controlled by the ratio between thermal conductivity along and across the field lines, which in a classical (non-quantizing) ...
... however, that 2D models have shown the importance of tangential heat conduction in limiting the anisotropy, compared with plane-parallel 1D models. The degree of anisotropy is controlled by the ratio between thermal conductivity along and across the field lines, which in a classical (non-quantizing) ...
The fuelling of local supermassive black holes
... Local SMBHs are not [all] bright AGNs because accretion follows activity cycles : this solution seems unavoidable (from numerical simulations) is the only one that can account for a variety of observational evidence (Chandra) does not imply large amounts of cooled off gas as long-lasting inflo ...
... Local SMBHs are not [all] bright AGNs because accretion follows activity cycles : this solution seems unavoidable (from numerical simulations) is the only one that can account for a variety of observational evidence (Chandra) does not imply large amounts of cooled off gas as long-lasting inflo ...
Driving downsizing with galaxy groups
... the disk requires high velocities and ICM densities • The hot halo can perhaps be stripped more easily (Larson, Tinsley & Caldwell 1980) ...
... the disk requires high velocities and ICM densities • The hot halo can perhaps be stripped more easily (Larson, Tinsley & Caldwell 1980) ...
What powers luminous infrared galaxies?
... fluxes to derive an average extinction using Galactic conversion factors from CO flux to H2 column density and visual extinction. Since the average extinction is somewhat uncertain due to the adopted conversion factors, and not identical to the extinction along a particular line of sight, it is not ...
... fluxes to derive an average extinction using Galactic conversion factors from CO flux to H2 column density and visual extinction. Since the average extinction is somewhat uncertain due to the adopted conversion factors, and not identical to the extinction along a particular line of sight, it is not ...
The Solar Tachocline: A Self-Consistent Model of Magnetic
... high pressure and temperature cause hydrogen nuclei to fuse into helium, releasing the energy that powers the Sun (and all life on Earth). The thermal energy released in the core is carried outward by photon radiation. Throughout the solar interior, pressure, density and temperature all decrease out ...
... high pressure and temperature cause hydrogen nuclei to fuse into helium, releasing the energy that powers the Sun (and all life on Earth). The thermal energy released in the core is carried outward by photon radiation. Throughout the solar interior, pressure, density and temperature all decrease out ...
New Frontiers in Nuclear Physics Kai Hebeler (OSU)
... that does not account for general-relativistic effects. data set. ...
... that does not account for general-relativistic effects. data set. ...
The slow-neutron capture process at low metallicity
... We present models for the slow neutron capture (s-process) in AGB stars of metallicity, Z = 0.0001 [Fe/H] = -2.3 Mass range from 0.9Msun to 6Msun, where we have explored model uncertainties by using two independent stellar evolution codes We encountered 4 regimes of neutron-capture nucleosynthesis M ...
... We present models for the slow neutron capture (s-process) in AGB stars of metallicity, Z = 0.0001 [Fe/H] = -2.3 Mass range from 0.9Msun to 6Msun, where we have explored model uncertainties by using two independent stellar evolution codes We encountered 4 regimes of neutron-capture nucleosynthesis M ...
ppt - lenac
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
SN 2011dh and the progenitors of Type IIb supernovae Mattias Ergon
... nearby galaxy M51, and images covering the location where supernova (SN) 2011dh would later occur are obtained. Examining the position of the SN reveals an anonymous yellow star, seemingly similar to millions of other stars in this galaxy. However, beneath the surface, in the interior of the star, t ...
... nearby galaxy M51, and images covering the location where supernova (SN) 2011dh would later occur are obtained. Examining the position of the SN reveals an anonymous yellow star, seemingly similar to millions of other stars in this galaxy. However, beneath the surface, in the interior of the star, t ...
Accretion Processes of Binaries of White Dwarfs
... There are two branches of equation of state between the surface mass density of disk and temperature (or accretion rate). High temperature state corresponds to high viscosity state. In cold disk state, material piles up in the disk, because accretion is inefficient and secondary keeps dumping mass. ...
... There are two branches of equation of state between the surface mass density of disk and temperature (or accretion rate). High temperature state corresponds to high viscosity state. In cold disk state, material piles up in the disk, because accretion is inefficient and secondary keeps dumping mass. ...
Modelling the atmosphere of the carbon
... well as in the observations. The presence of a companion star and/or a disk or a decrease in mass loss within the past few hundred years cannot be excluded, but these explanations are considered unlikely. Key words. techniques: interferometric – instrumentation: high angular resolution – circumstell ...
... well as in the observations. The presence of a companion star and/or a disk or a decrease in mass loss within the past few hundred years cannot be excluded, but these explanations are considered unlikely. Key words. techniques: interferometric – instrumentation: high angular resolution – circumstell ...
Pulsar slow glitches in a solid quark star model
... which state of matter really exists in pulsar-like stars due to the difficulty of calculation from the first principles of the elementary strong interaction, even 40 years after the discovery of pulsars. Nuclear matter (related to neutron stars) is one of the speculations even from the Landau’s time ...
... which state of matter really exists in pulsar-like stars due to the difficulty of calculation from the first principles of the elementary strong interaction, even 40 years after the discovery of pulsars. Nuclear matter (related to neutron stars) is one of the speculations even from the Landau’s time ...
A forming disk at z 0.6: collapse of a gaseous disk or major merger
... Fig. 4. As expected, this additional old population influences the resulting SED only above 4000 Å, and particularly in the NIR. One might wonder whether this additional old population is real, given that the resulting combined SED does not seem to improve the global fit in this region, where the ad ...
... Fig. 4. As expected, this additional old population influences the resulting SED only above 4000 Å, and particularly in the NIR. One might wonder whether this additional old population is real, given that the resulting combined SED does not seem to improve the global fit in this region, where the ad ...
The star formation history of galaxies in 3D: CALIFA perspective
... (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main physical parameters that produce the Hubble sequence, increasing from late to early spirals. In this scheme, S0 galaxies are a transition class between the spiral classes and the ...
... (Blanton & Moustakas 2009), following well the Hubble tuning-fork diagram. The bulge fraction seems to be one of the main physical parameters that produce the Hubble sequence, increasing from late to early spirals. In this scheme, S0 galaxies are a transition class between the spiral classes and the ...
EXPLORING STELLAR EVOLUTION MODELS OF sdB STARS
... stars were determined to be significantly less than halfway through their He-burning lifetimes, having consumed only about 20%–40% of the helium fuel in their cores. Standard stellar evolution, without any additional mixing at the boundary of the convective core, predicts a constant convective core m ...
... stars were determined to be significantly less than halfway through their He-burning lifetimes, having consumed only about 20%–40% of the helium fuel in their cores. Standard stellar evolution, without any additional mixing at the boundary of the convective core, predicts a constant convective core m ...
Chapter 2 Simulation Methodology 2.1 The generation of cosmological initial conditions
... Creating a set of initial conditions for simulations of cosmological structure formation is, on the surface, a very straightforward task. One specifies a background cosmological model, typically described as a spatially flat or open Robertson-Walker spacetime. Following that, perturbations are impos ...
... Creating a set of initial conditions for simulations of cosmological structure formation is, on the surface, a very straightforward task. One specifies a background cosmological model, typically described as a spatially flat or open Robertson-Walker spacetime. Following that, perturbations are impos ...
asteroseismological study of massive zz ceti stars with
... cooler temperatures with the discovery of low mass pulsators. The variable low-mass white dwarf stars are characterized by effective temperatures below ∼10,000 K and long periods in the range 1000–4500 s. Over the years, pulsation studies of ZZ Ceti stars through asteroseismology have become a valua ...
... cooler temperatures with the discovery of low mass pulsators. The variable low-mass white dwarf stars are characterized by effective temperatures below ∼10,000 K and long periods in the range 1000–4500 s. Over the years, pulsation studies of ZZ Ceti stars through asteroseismology have become a valua ...