The new millisecond pulsar PSR 1957+20 and neutron star equations of state

Details The new millisecond pulsar PSR 1957+20 and neutron star equations of state The new millisecond pulsar PSR 1957+20 and neutron star equations of state

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...206l..15l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 206, no. 1, Nov. 1988, p. L15, L16.

Astronomy and Astrophysics

Astronomy

4

Equations Of State, Neutron Stars, Pulsars, Stellar Rotation, Eclipsing Binary Stars, Radio Sources (Astronomy), Stellar Evolution, Stellar Magnetic Fields, Stellar Mass Accretion

Scientific paper

It is argued that the proximity of the rotational periods of millisecond pulsars PSR 1937+21 and PSR 1957+20 and their low dP/dt may point to the hardest equation of state for neutron star (NS) matter. If the argument is correct, then the lower boundary of NS rotational periods lies at about 1 ms, and the estimated lower limits for the masses of the two pulsars are about 1.38 and 1.3 solar masses, respectively. The new questions posed for stellar evolutionary theory by the discovery of PSR 1957+20 are considered.

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