Other
Scientific paper
Oct 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...217..244h&link_type=abstract
Astrophysical Journal, Part 1, vol. 217, Oct. 1, 1977, p. 244-247.
Other
13
Neutron Stars, Relativistic Effects, Stellar Mass, Stellar Rotation, Damping, Equations Of State, Relativity, Stellar Models
Scientific paper
It is shown that any significant amount of differential rotation initially present in a neutron star will be damped out within a few days. Consequently, differential rotation need not be considered in determining the upper mass limit for neutron stars. This limit is determined with the fewest possible assumptions. Without rotation the mass may not exceed 8 solar masses. Rigid body rotation may increase the mass by no more than 30% according to calculations by others. Thus the upper mass limit, including rotation, is found to be 11 solar masses. This limit requires no assumptions about the equation of state above a density of 2 by 10 to the 14th power g/cu cm and cannot be violated in any plausible way other than the breakdown of general relativity. If one is willing to accept specific constraint imposed by causality on static equations of state, the upper mass limit would be reduced by solar masses.
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