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1974•Symposium - International Astronomical UnionOpen access

Neutron Star Structure from Pulsar Observations

David Pines, J. Shaham, Malvin A. Ruderman

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Abstract

We examine what inferences can be made regarding neutron star structure from observations of micro- and macroglitch behavior. After considering various theories it seems plausible that crustquakes offer an explanation for the Crab microglitches, while corequakes can explain the Vela macroglitches. It is concluded that the Crab pulsar has a mass of less than 0.5 M⊙ and is ∼ 90% superfluid neutrons while the Vela pulsar may possess a solid neutron core and have a mass of ∼ 0.7 M⊙ with a superfluid neutron abundance of ∼ 15%.

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We examine what inferences can be made regarding neutron star structure from observations of micro- and macroglitch behavior. After considering various theories it seems plausible that crustquakes offer an explanation for the Crab microglitches, while corequakes can explain the Vela macroglitches. It is concluded that the Crab pulsar has a mass of less than 0.5 M⊙ and is ∼ 90% superfluid neutrons while the Vela pulsar may possess a solid neutron core and have a mass of ∼ 0.7 M⊙ with a superfluid neutron abundance of ∼ 15%.

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Available abstract

We examine what inferences can be made regarding neutron star structure from observations of micro- and macroglitch behavior. After considering various theories it seems plausible that crustquakes offer an explanation for the Crab microglitches, while corequakes can explain the Vela macroglitches. It is concluded that the Crab pulsar has a mass of less than 0.5 M⊙ and is ∼ 90% superfluid neutrons while the Vela pulsar may possess a solid neutron core and have a mass of ∼ 0.7 M⊙ with a superfluid neutron abundance of ∼ 15%.

Key concepts: Vela, Physics, Pulsar, Neutron star, Crab Pulsar, Astrophysics, X-ray pulsar, r-process

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