130 research outputs found
Two-size approximation: a simple way of treating the evolution of grain size distribution in galaxies
Full calculations of the evolution of grain size distribution in galaxies are
in general computationally heavy. In this paper, we propose a simple model of
dust enrichment in a galaxy with a simplified treatment of grain size
distribution by imposing a `two-size approximation'; that is, all the grain
population is represented by small (grain radius a < 0.03 micron) and large (a
> 0.03 micron) grains. We include in the model dust supply from stellar ejecta,
destruction in supernova shocks, dust growth by accretion, grain growth by
coagulation and grain disruption by shattering, considering how these processes
work on the small and large grains. We show that this simple framework
reproduces the main features found in full calculations of grain size
distributions as follows. The dust enrichment starts with the supply of large
grains from stars. At a metallicity level referred to as the critical
metallicity of accretion, the abundance of the small grains formed by
shattering becomes large enough to rapidly increase the grain abundance by
accretion. Associated with this epoch, the mass ratio of the small grains to
the large grains reaches the maximum. After that, this ratio converges to the
value determined by the balance between shattering and coagulation, and the
dust-to-metal ratio is determined by the balance between accretion and shock
destruction. With a Monte Carlo simulation, we demonstrate that the simplicity
of our model has an advantage in predicting statistical properties. We also
show some applications for predicting observational dust properties such as
extinction curves.Comment: 14 pages, 12 figures, accepted for publication in MNRA
Evolution of dust grain size distribution by shattering in the interstellar medium: robustness and uncertainty
Shattering of dust grains in the interstellar medium is a viable mechanism of
small grain production in galaxies. We examine the robustness or uncertainty in
the theoretical predictions of shattering. We identify (the critical
pressure above which the deformation destroys the original lattice structures)
as the most important quantity in determining the timescale of small grain
production, and confirm that the same ( is the duration of
shattering) gives the same grain size distribution [, where is the
grain radius] after shattering within a factor of 3. The uncertainty in the
fraction of shocked material that is eventually ejected as fragments causes
uncertainties in by a factor of 1.3 and 1.6 for silicate and
carbonaceous dust, respectively. The size distribution of shattered fragments
have minor effects as long as the power index of the fragment size distribution
is less than ~ 3.5, since the slope of grain size distribution
continuously change by shattering and becomes consistent with . The grain velocities as a function of grain radius can have an
imprint in the grain size distribution especially for carbonaceous dust. We
also show that the formulation of shattering can be simplified without losing
sufficient precision.Comment: 12 pages, 7 figures, Accepted for publication in Earth, Planets, and
Space (Special Issue: Cosmic Dust V
Observational Test of Environmental Effects on The Local Group Dwarf Spheroidal Galaxies
In this paper, we examine whether tidal forces exerted by the Galaxy or M31
have an influence on the Local Group dwarf spheroidal galaxies (dSphs) which
are their companions. We focus on the surface brightness profiles of the dSphs,
especially their core radii because it is suggested based on the numerical
simulations that tidal disturbance can make core radii extended. We examine the
correlation for the dSphs between the distances from their parent galaxy (the
Galaxy or M31) and the compactnesses of their surface brightness profiles by
using a parameter ``C'' defined newly in this paper. Consequently, we find no
significant correlation. We make some remarks on the origin of this result by
considering three possible scenarios; tidal picture, dark matter picture, and
heterogeneity of the group of dSphs, each of which has been often discussed to
understand fundamental properties and formation processes of dSphs.Comment: 14 pages LaTeX, 2 PostScript figures, to appear in ApJ Letter
Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments
We propose an updated dust evolution model that focuses on the grain size
distribution in a galaxy. We treat the galaxy as a one-zone object and include
five main processes (stellar dust production, dust destruction in supernova
shocks, grain growth by accretion and coagulation, and grain disruption by
shattering). In this paper, we improve the predictions related to small
carbonaceous grains, which are responsible for the 2175 \AA\ bump in the
extinction curve and the polycyclic aromatic hydrocarbon (PAH) emission
features in the dust emission spectral energy distribution (SED), both of which
were underpredicted in our previous model. In the new model, we hypothesize
that small carbonaceous grains are not involved in interstellar processing.
This avoids small carbonaceous grains being lost by coagulation. We find that
this hypothetical model shows a much better match to the Milky Way (MW)
extinction curve and dust emission SED than the previous one. The following two
additional modifications further make the fit to the MW dust emission SED
better: (i) The chemical enrichment model is adjusted to give a nearly solar
metallicity in the present epoch, and the fraction of metals available for dust
growth is limited to half. (ii) Aromatization for small carbonaceous grains is
efficient, so that the aromatic fraction is unity at grain radii
\AA. As a consequence of our modelling, we succeed in obtaining a dust
evolution model that explains the MW extinction curve and dust emission SED at
the same time.Comment: 11 pages, 7 figures, accepted for publication in MNRA
Evolution of dust content in galaxies probed by gamma-ray burst afterglows
Because of their brightness, gamma-ray burst (GRB) afterglows are viable
targets for investigating the dust content in their host galaxies. Simple
intrinsic spectral shapes of GRB afterglows allow us to derive the dust
extinction. Recently, the extinction data of GRB afterglows are compiled up to
redshift , in combination with hydrogen column densities and
metallicities. This data set enables us to investigate the relation between
dust-to-gas ratio and metallicity out to high redshift for a wide metallicity
range. By applying our evolution models of dust content in galaxies, we find
that the dust-to-gas ratio derived from GRB afterglow extinction data are
excessively high such that they can be explained with a fraction of gas-phase
metals condensed into dust () , while theoretical
calculations on dust formation in the wind of asymptotic giant branch stars and
in the ejecta of Type II supernovae suggest a much more moderate condensation
efficiency (). Efficient dust growth in dense clouds has
difficulty in explaining the excessive dust-to-gas ratio at metallicities
, where is the star formation
efficiency of the dense clouds. However, if is as small as 0.01, the
dust-to-gas ratio at Z can be explained with
cm. Therefore, a dense environment hosting
dust growth is required to explain the large fraction of metals condensed into
dust, but such clouds should have low star formation efficiencies to avoid
rapid metal enrichment by stars.Comment: 7 pages, 3 figures, published in MNRA
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