Multiplicity-corrected mass function of main-sequence stars in the solar neighborhood

Details Multiplicity-corrected mass function of main-sequence stars in the solar neighborhood Multiplicity-corrected mass function of main-sequence stars in the solar neighborhood

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...393..373b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 393, no. 1, July 1, 1992, p. 373-384.

Astronomy and Astrophysics

Astrophysics

51

Galactic Evolution, Main Sequence Stars, Solar System, Stellar Luminosity, Stellar Mass, Interstellar Magnetic Fields, Neutron Stars, Star Formation Rate, White Dwarf Stars

Scientific paper

A present-day mass function (PDMF) of stars in solar neighborhood with photometric luminosity function corrected for the effects of unresolved multiple stellar systems gives a stellar surface mass density of 39.5 solar masses pc exp -2 as opposed to only 31.3 solar masses pc exp -2 given by the uncorrected PDMF. An initial mass function (IMF) is calculated from the corrected PDMF using a number of star-formation rates with exponential time dependence. Neutron star and white dwarf formation rates restrict the reciprocal of the time constant of star formation to the range between -0.1 and +0.1/Gyr. The IMF for stellar masses greater than 1.4 solar masses can be represented as a power law with an exponent of -1.56 +/- 0.05. For masses greater than 6.5 solar masses, a power of -1.67 fits better. The ratio of the mass of gas returned to the ISM by the stars to the total mass of gas that has ever gone into star formation is found to be a rapidly increasing function of the reciprocal of the time constant of star formation. The fraction of remnants and evolved stars show the same trend, with a less rapid increase. The total surface mass density predicted by the IMF is consistent with the presence of little or no nonbaryonic dark matter in the Galactic disk in the solar neighborhood.

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