2,347 research outputs found
Chemical Evolution of M31
We review chemical evolution models developed for M31 as well as the
abundance determinations available for this galaxy. Then we present a recent
chemical evolution model for M31 including radial gas flows and galactic
fountains along the disk, as well as a model for the bulge. Our models are
predicting the evolution of the abundances of several chemical species such as
H, He, C, N, O, Ne, Mg, Si, S, Ca and Fe. From comparison between model
predictions and observations we can derive some constraints on the evolution of
the disk and the bulge of M31. We reach the conclusions that Andromeda must
have evolved faster than the Milky Way and inside-out, and that its bulge
formed much faster than the disk on a timescale 0.5 Gyr. Finally, we
present a study where we apply the model developed for the disk of M31 in order
to study the probability of finding galactic habitable zones in this galaxy.Comment: To be published in:"Lessons from the Local Group: A Conference in
Honour of David Block and Bruce Elmegreen" Editors: Prof. Dr. Kenneth
Freeman, Dr. Bruce Elmegreen, Prof. Dr. David Block, Matthew Woolway,
Springe
Galactic Winds in Irregular Starburst Galaxies
In this paper we present some results concerning the study of the development
of galactic winds in blue compact galaxies. In particular, we model a situation
very similar to that of the galaxy IZw18, the most metal poor and unevolved
galaxy known locally. To do that we compute the chemo-dynamical evolution of a
galaxy in the case of one istantaneous isolated starburst as well as in the
case of two successive instantaneous starbursts. We show that in both cases a
metal enriched wind develops and that the metals produced by the type Ia SNe
are lost more efficiently than those produced by type II SNe. We also find that
one single burst is able to enrich chemically the surrounding region in few
Myr. Both these results are the effect of the assumed efficiency of energy
transfer from SNe to ISM and to the consideration of type Ia SNe in this kind
of problem. The comparison with observed abundances of IZw18 suggests that this
galaxy is likely to have suffered two bursts in its life, with the previous
being less intense than the last one.Comment: 3 pages, 1 figure, to appear in the Proceedings of the Conference
"Cosmic Evolution", Paris, November 200
The two regimes of the cosmic sSFR evolution are due to spheroids and discs
This paper aims at explaining the two phases in the observed specific star
formation rate (sSFR), namely the high (>3/Gyr) values at z>2 and the smooth
decrease since z=2. In order to do this, we compare to observations the
specific star formation rate evolution predicted by well calibrated models of
chemical evolution for elliptical and spiral galaxies, using the additional
constraints on the mean stellar ages of these galaxies (at a given mass). We
can conclude that the two phases of the sSFR evolution across cosmic time are
due to different populations of galaxies. At z>2 the contribution comes from
spheroids: the progenitors of present-day massive ellipticals (which feature
the highest sSFR) as well as halos and bulges in spirals (which contribute with
average and lower-than-average sSFR). In each single galaxy the sSFR decreases
rapidly and the star formation stops in <1 Gyr. However the combination of
different generations of ellipticals in formation might result in an apparent
lack of strong evolution of the sSFR (averaged over a population) at high
redshift. The z<2 decrease is due to the slow evolution of the gas fraction in
discs, modulated by the gas accretion history and regulated by the Schmidt law.
The Milky Way makes no exception to this behaviour.Comment: 8 pages, 5 figures, MNRAS accepte
A possible theoretical explanation of metallicity gradients in elliptical galaxies
Models of chemical evolution of elliptical galaxies taking into account
different escape velocities at different galactocentric radii are presented. As
a consequence of this, the chemical evolution develops differently in different
galactic regions; in particular, we find that the galactic wind, powered by
supernovae (of type II and I) starts, under suitable conditions, in the outer
regions and successively develops in the central ones. The rate of star
formation (SFR) is assumed to stop after the onset of the galactic wind in each
region. The main result found in the present work is that this mechanism is
able to reproduce metallicity gradients, namely the gradients in the
index, in good agreement with observational data. We also find that in order to
honor the constant [Mg/Fe] ratio with galactocentric distance, as inferred from
metallicity indices, a variable initial mass function as a function of
galactocentric distance is required. This is only a suggestion since trends on
abundances inferred just from metallicity indices are still uncertain.Comment: 18 pages, LaTeX file with 4 figures using mn.sty, submitted to MNRA
The Galactic habitable zone around M and FGK stars with chemical evolution models with dust
The Galactic habitable zone is defined as the region with highly enough
metallicity to form planetary systems in which Earth-like planets could be born
and might be capable of sustaining life surviving to the destructive effects of
nearby supernova explosion events. Galactic chemical evolution models can be
useful tools for studying the galactic habitable zones in different systems.
Our aim here is to find the Galactic habitable zone using chemical evolution
models for the Milky Way disc, adopting the most recent prescriptions for the
evolution of dust and for the probability of finding planetary systems around M
and FGK stars. Moreover, for the first time, we will express those
probabilities in terms of the dust-to-gas ratio of the ISM in the solar
neighborhood as computed by detailed chemical evolution models. At a fixed
Galactic time and Galactocentric distance we determine the number of M and FGK
stars having Earths (but no gas giant planets) which survived supernova
explosions, using the formalism of our Paper I. The probabilities of finding
terrestrial planets but not gas giant planets around M stars deviate
substantially from the ones around FGK stars for supersolar values of [Fe/H].
For both FGK and M stars the maximum number of stars hosting habitable planets
is at 8 kpc from the Galactic Centre, if destructive effects by supernova
explosions are taken into account. At the present time the total number of M
stars with habitable planets are 10 times the number of FGK stars.
Moreover, we provide a sixth order polynomial fit (and a linear one but more
approximated) for the relation found with chemical evolution models in the
solar neighborhood between the [Fe/H] abundances and the dust-to-gas ratio.Comment: Accepted for publication in A&A, 10 pages 6 figure
The Chemical Evolution of the Galaxy: the two-infall model
In this paper we present a new chemical evolution model for the Galaxy which
assumes two main infall episodes for the formation of halo-thick disk and thin
disk, respectively. We do not try to take into account explicitly the evolution
of the halo but we implicitly assume that the timescale for the formation of
the halo was of the same order as the timescale for the formation of the thick
disk. The formation of the thin-disk is much longer than that of the thick
disk, implying that the infalling gas forming the thin-disk comes not only from
the thick disk but mainly from the intergalactic medium. The timescale for the
formation of the thin-disk is assumed to be a function of the galactocentric
distance, leading to an inside-out picture for the Galaxy building. The model
takes into account the most up to date nucleosynthesis prescriptions and adopts
a threshold in the star formation process which naturally produces a hiatus in
the star formation rate at the end of the thick disk phase, as suggested by
recent observations. The model results are compared with an extended set of
observational constraints. Among these constraints, the tightest one is the
metallicity distribution of the G-dwarf stars for which new data are now
available. Our model fits very well these new data. We show that in order to
reproduce most of these constraints a timescale Gyr for the
(halo)-thick-disk and of 8 Gyr for the thin-disk formation in the solar
vicinity are required. We predict that the radial abundance gradients in the
inner regions of the disk () are steeper than in the outer
regions, a result confirmed by recent abundance determinations, and that the
inner ones steepen in time during the Galactic lifetime.Comment: 48 pages, 20 Postscript figures, AASTex v.4.0, to be published in
Astrophysical Journa
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