Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...318..485h&link_type=abstract
Astronomy and Astrophysics, v.318, p.485-489
Astronomy and Astrophysics
Astrophysics
6
Pulsars: General, Stars: Evolution, Stars: Magnetic Fields
Scientific paper
Two dozen long period pulsars are separated from the swarm of ordinary pulsars by an obvious gap in the P versus Sd diagram (where Sd=log˙(P)+21.0), with a plausible upper boundary for ordinary pulsars. Possible pulsar evolutionary tracks are discussed to explain the diagram in terms of previously suggested scenarios of magnetic field decay. The (P-Sd) diagram is difficult to understand if there is no magnetic field decay during the active life of pulsars. However, if the magnetic fields of neutron stars decay exponentially, almost all slowly rotating pulsars must have been injected with a very long initial spin period of about 2 seconds, which seems impossible. Based on qualitative analyses, it is concluded that magnetic fields of neutron stars decay as a power-law, with a time scale related to the initial field strengths. The plausible boundary and the gap are suggested to naturally divide pulsars with distinct magnetic "genes", ie. pulsars which were born from strongly magnetized progenitors -- such as Bp stars, and pulsars born from normal massive stars. The possibility remains open that a fraction of slowly rotating pulsars were injected with long initial spin periods, while others would have a classical pulsar evolution history. It is suggested that PSR B1849+00 was born in the supernova remnant Kes-79 with an initial period of about 2 seconds.
No associations
LandOfFree
Slowly rotating pulsars and magnetic field decay does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Slowly rotating pulsars and magnetic field decay, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Slowly rotating pulsars and magnetic field decay will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1772007