Absolute limit on rotation of gravitationally bound stars

Details Absolute limit on rotation of gravitationally bound stars Absolute limit on rotation of gravitationally bound stars

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994stin...9437049g&link_type=abstract

Presented at the Aspen Winter Conference on Astrophysics: Millisecond Pulsars, a Decade of Surprises, Aspen, CO, 3-7 Jan. 1994

Physics

Neutron Stars, Pulsars, Stellar Mass, Stellar Physics, Stellar Rotation, Equations Of State, Gravitational Effects, Hadrons, Mass Transfer, Nucleons, Relativity

Scientific paper

The authors seek an absolute limit on the rotational period for a neutron star as a function of its mass, based on the minimal constraints imposed by Einstein's theory of relativity, Le Chatelier's principle, causality, and a low-density equation of state, uncertainties which can be evaluated as to their effect on the result. This establishes a limiting curve in the mass-period plane below which no pulsar that is a neutron star can lie. For example, the minimum possible Kepler period, which is an absolute limit on rotation below which mass-shedding would occur, is 0.33 ms for a M = 1.442 solar mass neutron star (the mass of PSR1913+16). If the limit were found to be broken by any pulsar, it would signal that the confined hadronic phase of ordinary nucleons and nuclei is only metastable.

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