Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..33..265k&link_type=abstract
Astrophysics and Space Science, vol. 33, Apr. 1975, p. 265-293.
Astronomy and Astrophysics
Astrophysics
20
Astronomical Models, Chemical Composition, Galactic Evolution, Galactic Structure, Abundance, Computerized Simulation, Galactic Radiation, Mathematical Models, Radiant Flux Density, Shock Waves, Supernovae, X Rays
Scientific paper
Models for the chemical evolution of the galaxy are constructed in which the temporal evolution is determined by the galactic contraction rate and present observations of stellar metal abundances reflect the metal abundances in the interstellar medium at the time of stellar birth. It is argued that the birth rate for stars exceeding 3.5 solar masses has a power-law relationship to the contracting volume of the main body of the galaxy. The supernova rates are small enough to avoid the problem of collisions between shock waves from neighboring supernovae during the adiabatic expansion stage. It is shown that the assumed power-law birth rate yields suitable chemical evolution models when a dynamic time scale is adopted for galactic contraction only if observed Population II metals are synthesized in stars more massive than 8.5 solar masses, and that collisions between neighboring supernovae shock waves can produce local regions of significantly enhanced density. Values of between 13 and 34 are estimated for the average number of supernova explosions during the final stages of contraction to the galactic disk.
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