Dark Matter and Chemical Evolution of dSph Galaxies

Details Dark Matter and Chemical Evolution of dSph Galaxies Dark Matter and Chemical Evolution of dSph Galaxies

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002ap%26ss.281..533c&link_type=abstract

Astrophysics and Space Science, v. 281, Issue 1, p. 533-534 (2002).

Astronomy and Astrophysics

Astrophysics

Scientific paper

We calculate chemical evolution models for 4 dwarf spheroidal satellites of the Milky Way (Carina, Ursa Minor, Leo I and Leo II) for which reliable non-parametric star formation histories have been derived. We find that galaxies showing one single burst of star formation (Ursa Minor and Leo II) require a dark halo slightly larger that the current estimates for their tidal radii for the gas heated by supernovae to be retained until the observed stellar population has formed. Systems showing extended star formation histories however (Carina and Leo I), are consistent with the idea that their tidally limited dark haloes provide the necessary gravitational potential wells to retain their gas.

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