Physics
Scientific paper
Mar 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.302..124b&link_type=abstract
Nature, vol. 302, Mar. 10, 1983, p. 124, 125.
Physics
18
Pulsars, Spin Dynamics, Stellar Evolution, Stellar Magnetic Fields, Stellar Rotation, Angular Momentum, Magnetic Dipoles, Neutron Stars, Red Giant Stars, Stellar Envelopes, Stellar Mass Ejection, Stellar Radiation, Supernova Remnants, White Dwarf Stars
Scientific paper
Formation mechanisms for fast rotating pulsars are considered, with attention given to the pulsar 4C21.53, which has a period of 1.6 msec. During late stages of stellar evolution, the process of magnetic field lines transporting angular momentum from a contracting red-giant core to the envelope to form slowly rotating white dwarfs and neutron stars can also be the way fast rotating pulsars form. The progenitor red-giant core would have had a weaker field, and thus slowed down less. A field less than a billion gauss is calculated. Gravitational radiation, magnetic braking due to mass loss, and magnetic dipole radiation are discussed for a neutron star spinning down to periods much greater than 1 msec after being formed with a period of up to 1 msec. Magnetic dipole radiation is found to produce a star with a spin down of about 100 million yr, or at least 10,000 yr since no supernova remnant has been associated with 4C21.53. Observational predictions are made for the optical emissions of the Crab and Vela pulsars, and more short-period pulsars are expected, unless they have only formed from binary configurations.
Brecher Kenneth
Chanmugam G.
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