Physics
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..392s&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Physics
Scientific paper
An N-body numerical simulation on the birthplace and birthrate of supernovae in spiral galaxies with a certain thickness is carried out. The fundamental basis is: starbirth takes place mainly in GMCs, in which process a mass spectrum of formed stars is obeyed. The massive stars have short lifetime and their end of lifetime is supernovae and their explosion. The supernovae explosion will disrupt the GMCs where they are embedded. The fragments of disrupted GMCs will form GMCs once again by the aggregation mechanism. In this case, the evolution of molecular clouds in a spiral galaxy is a significant tool for the study of supernovae, when both disruption and formation of GMCs are included. The observed mass spectrum of GMCs and the birthrate of stars in our Galaxy will testify the results of our simulation. And from the simulation, the related information of supernovae can be derived as well. It is shown that supernovae and their remnants are distributed within star disk, but more concentrated in arm regions and disk plane. In our Galaxy there should be (755± 12)τ5 supernovae remnants (SNRs), where τ5 is the ratio of the lifetime of SNRs to 105 yr. Due to the crowding of SNRs in the disk plane, less SNRs could be observed.
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