2004/02/06 by H. Ogelman, H. gelman, M. A. Alpar · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Binary pulsar #Dipole #Gamma-ray bursts and supernovae #Luminosity #Magnetic dipole #Magnetic field #Millisecond pulsar #Pulsar #Pulsars and Gravitational Waves Research #Rotation (mathematics) #astro-ph
paper · pdf · doi:10.1086/383085
published as Astrophys.J. 603 (2004) L33-L36 · Accepted for publication in ApJ Letters
arxiv created 2004/02/06 · openalex publication_date 2004/02/09 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We assume that all the energy loss of the putative pulsar in SN 1987A would contribute to the luminosity of the remnant, which acts like a bolometer. The bolometric luminosity of SN 1987A provides an upper bound on the pulsar's rate of energy loss. An isolated pulsar spinning down by magnetic dipole radiation alone with initial rotation periods of 10-30 ms, as extrapolated for galactic young pulsars, can have a luminosity below the bolometric bound if either the magnetic field is weak, B ~ 10 9 -10 10 G, or if it is so strong that the pulsar luminosity decays rapidly, B ~ 10 16 G.