We developed a code for galactic star-counts making use of suitable assumptions on the evolutionary status, initial mass function (IMF) and star formation history of the various Galactic populations. Predicted results are obtained by randomly generating star masses according to the adopted IMF and by using stellar models (evolutionary tracks up to the white dwarf phase) to derive luminosities in the selected bands for each given value of the stellar mass and age. Star counts from solar neighborhood are used to give constraints on star formation rate and IMF.
Galactic structure and white dwarf populations
CIGNONI, MICHELE;PRADA MORONI, PIER GIORGIO;DEGL'INNOCENTI, SCILLA
2004-01-01
Abstract
We developed a code for galactic star-counts making use of suitable assumptions on the evolutionary status, initial mass function (IMF) and star formation history of the various Galactic populations. Predicted results are obtained by randomly generating star masses according to the adopted IMF and by using stellar models (evolutionary tracks up to the white dwarf phase) to derive luminosities in the selected bands for each given value of the stellar mass and age. Star counts from solar neighborhood are used to give constraints on star formation rate and IMF.File in questo prodotto:
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