Evolution of close binaries after the burst of starformation for different IMFs

Details Evolution of close binaries after the burst of starformation for different IMFs Evolution of close binaries after the burst of starformation for different IMFs

1997-11-28

arxiv.org/abs/astro-ph/9711352v1

Astronomy and Astrophysics

Astrophysics

12 pages, 4 PostScript figures, to be presented as a poster at the conference "Cosmology: from COBE to galaxy formation", 1-7

Scientific paper

We use "Scenario Machine" -- the population synthesis simulator -- to calculate the evolution of populations of selected types of X-ray sources after a starformation burst with the total mass in binaries (1--1.5) \cdot 10^6 M_{\odot}$ during the first 20 Myr after a burst. We present here the results of two sets of runs of the program. In the first set we examined the following types of close binaries: transient sources-- neutron stars with Be- stars; ``X-ray pulsars''-- neutron stars in pairs with supergiants; Cyg X-1-like sources-- black holes with supergiants; ``SS443-like sources''-- superaccreting black holes. We used two values of the exponent $\alpha$ in the initial mass function: 2.35 (Salpeter's function) and 1 (``flat spectrum''). The calculations were made for the folowing values of the upper limit of the mass function: 120 and 30 $M_{\odot}$. For the ``flat spectrum'', suggested in (Contini et al, 1995), the number of sources of all types significantly increased. With the ``flat spectrum'' and with the upper mass limit 120 $M_{\odot}$ we obtained hundreds of sources of all calculated types. Decreasing of the upper mass limit below the critical mass of a black hole formation increase the number of transient sources with neutron stars up to $\approx 300$. In the second set we examined the evolution of of 12 other types of X-ray sources for $\alpha=1$, $\alpha=1.35$ and $\alpha=2.35$ and for three upper mass limits: 120 $M_{\odot}$, 60 $M_{\odot}$, 40 $M_{\odot}$ (see Perez-Olia & Colina 1995 for the reasons for such upper limits) on the same time scale 20 Myr after a star formation burst.

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