Mordecai-Mark Mac Low
Max-Planck-Institut für Astronomie
Andrea Ferrara
Osservatorio Astrofisico di Arcetri
The Astrophysical Journal, 513, in press, 1 March 1999
We model the effects of repeated supernova explosions from starbursts
in dwarf galaxies on the interstellar medium of these
galaxies, taking into account the gravitational potential of their
dominant dark matter haloes. We explore supernova rates from one every
30,000 yr to one every 3 million yr, equivalent to steady mechanical
luminosities of L = 0.1 - 10 x 1038 erg s-1, occurring in
dwarf galaxies with gas masses Mg = 106 -
109 solar masses. We address
in detail, both analytically and numerically, the following three
questions:
- When do the supernova ejecta blow out of the disk of the galaxy?
- When blowout occurs, what fraction of the interstellar gas is
blown away, escaping the potential of the galactic halo?
- What happens to the metals ejected from the massive stars of the
starburst? Are they retained or blown away?
We give quantitative results for when blowout will or will not occur
in galaxies with Mg up to 109 solar masses.
Surprisingly, we find that
the mass ejection efficiency is very low in
outflows for galaxies with mass Mg > 107
solar masses. Only
galaxies with Mg < 106 solar masses have
their interstellar gas
blown away, and then virtually independently of L. On the other
hand, metals from the supernova ejecta are accelerated to velocities
larger than the escape speed from the galaxy far more easily than the
gas. We find that for L38 = 1, only
about 30% of the metals are retained by a 109 solar mass galaxy, and
virtually none by smaller galaxies. We discuss the
implications of our results for the evolution, metallicity and
observational properties of dwarf galaxies.
gzipped tar file with TeX and postscript
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Postscript text (224 K)
Postscript Figures (1.4 Mb each, except for Fig. 1, which is 26 K):
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Mac Low preprints
MPI Astronomy theory group
Mordecai-Mark Mac Low, [email protected]
Last modified: Thurs 8 Oct 1998