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

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dc.creatorTagieva, Sevinc O.
dc.creatorGuseinov, Oktay H.
dc.creatorAnkay, Askin
dc.date2003-06-05
dc.date.accessioned2026-07-07T02:08:43Z
dc.date.available2026-07-07T02:08:43Z
dc.descriptionWe 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$_{\odot}$.
dc.description15 pages of text, 1 table, 4 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0306117
dc.identifierhttp://arxiv.org/abs/astro-ph/0306117
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/6161
dc.subjectAstrophysics
dc.titleThe Lower Limit for Masses of Progenitors of Supernova Remnants and Radio Pulsars
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