4 research outputs found
Radial Dependence of Extinction in Parent Galaxies of Supernovae
The problem of extinction is the most important issue to be dealt with in the
process of obtaining true absolute magnitudes of core-collapse supernovae
(SNe). The plane-parallel model which gives absorption dependent on galaxy
inclination, widely used in the past, was shown not to describe extinction
adequately. We try to apply an alternative model which introduces radial
ependence of extinction. A certain trend of dimmer SNe with decreasing radius
from the center of a galaxy was found, for a chosen sample of stripped-envelope
SNe.Comment: 4 pages, 1 table, 2 figures, 6th SCSLSA Pro
Emission Lines in X-ray Spectra of Clusters of Galaxies
Emission lines in X-ray spectra of clusters of galaxies reveal the presence
of heavy elements in the diffuse hot plasma (the Intra Cluster Medium, or ICM)
in virial equilibrium in the dark matter potential well. The relatively simple
physical state of the ICM allows us to estimate, with good accuracy, its
thermodynamical properties and chemical abundances. These measures put strong
constraints on the interaction processes between the galaxies and the
surrounding medium, and have significant impact on models of galaxy formation
as well. This field is rapidly evolving thanks to the X-ray satellites Chandra
and XMM-Newton. Among the most relevant progresses in the last years, we
briefly discuss the nature of cool cores and the measure of the Iron abundance
in high redshift clusters. Future X-ray missions with bolometers promise to
provide a substantial step forward to a more comprehensive understanding of the
complex physics of the ICM.Comment: 8 pages, 3 figures, Proceedings of the VI Serbian Conference on
Spectral Line Shapes in Astrophysics, Sremski Karlovci, Serbia June 11-15
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Alkali Line Profiles in Degenerate Dwarfs
Ultracool stellar atmospheres show absorption by alkali resonance lines
severely broadened by collisions with neutral perturbers. In the coolest and
densest atmospheres, such as those of T dwarfs, Na I and K I broadened by
molecular hydrogen and helium can come to dominate the entire optical spectrum.
Their profiles have been successfully modelled with accurate interaction
potentials in the adiabatic theory, computing line profiles from the first few
orders of a density expansion of the autocorrelation function. The line shapes
in the emergent spectrum also depend on the distribution of absorbers as a
function of depth, which can be modelled with improved accuracy by new models
of dust condensation and settling.
The far red K I wings of the latest T dwarfs still show missing opacity in
these models, a phenomenon similar to what has been found for the Na I line
profiles observed in extremely cool, metal-rich white dwarfs. We show that the
line profile in both cases is strongly determined by multiple-perturber
interactions at short distances and can no longer be reproduced by a density
expansion, but requires calculation of the full profile in a unified theory.
Including such line profiles in stellar atmosphere codes will further improve
models for the coolest and densest dwarfs as well as for the deeper atmosphere
layers of substellar objects in general.Comment: VI Serbian Conference on Spectral Line Shapes in Astrophysics; to be
published by the American Institute of Physics, eds. Milan S. Dimitrijevic
and Luka C. Popovic; 6 pages, 6 figure