Statistics
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23..128r&link_type=abstract
Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 128-129
Statistics
Scientific paper
To describe the galaxy formation process we use the SPH simulation method. Associated with this is the star formation rate (SFR). We calculate the SFR adopting a Initial Mass Function (IMF) similar to Salpeter. We divide the IMF in three stellar populations for masses m(M¤) = 0.5,4.0,19.0, at intervals dm = 0.7,6.2,23.0. The stellar lifetimes are also considered. The total number and the total mass are normalized taking account on the three populations. The initial gas mass is divided into gas mass and stellar mass, this is the algorithm test. For every galaxy particle is used the Jeans criteria to test the colapse conditions. In this case, the particle mass will be distributed in agreement on the IMF. The process takes account for each particle and stellar population independently. If the lifetime is completed, the stars die like supernovas, returning to the gas. The statistics involves all the steps and calculates the SFR for each population over all the process. For each population one also obtains the variation in the stellar mass function with time. It can be seen a fast early star formation, which declines next and an increase for the last stage of the galaxy formation.
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