The Lower Limit for Masses of Progenitors of Supernova Remnants and Radio Pulsars

Details The Lower Limit for Masses of Progenitors of Supernova Remnants and Radio Pulsars The Lower Limit for Masses of Progenitors of Supernova Remnants and Radio Pulsars

2003-06-05

arxiv.org/abs/astro-ph/0306117v1

Astronomy and Astrophysics

Astrophysics

15 pages of text, 1 table, 4 figures

Scientific paper

We examined correlations between young radio pulsars (PSRs), Supernova remnants (SNRs) which have different surface brightness values and young star formation regions (SFRs). Angular correlation of PSRs with SFRs is reliable up to 4 kpc and considerably strong up to 3 kpc from the Sun. On average this correlation is stronger for Galactic anticenter directions compared to Galactic central directions. Angular correlation of SNRs with SFRs is weaker and depends on the surface brightness of the SNR. Spatial correlation of PSRs with SFRs is also stronger than spatial correlation of SNRs with SFRs. Dim SNRs show weak spatial correlation with SFRs. These investigations and analysis of various data show that the lower limit for masses of progenitors of PSRs is about 9 M$_{\odot}$ and of SNRs (or supernovae) is about 7 M$_{\odot}$.

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