Stable ultracompact objects and an upper bound on neutron star masses

Details Stable ultracompact objects and an upper bound on neutron star masses Stable ultracompact objects and an upper bound on neutron star masses

Jan 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...353..641n&link_type=abstract

Astronomy and Astrophysics, v.353, p.641-645 (2000)

Astronomy and Astrophysics

Astrophysics

6

Dense Matter, Equation Of State, Stars: Neutron

Scientific paper

We have proposed a core-envelope model with stiffest equation of state [speed of sound equal to that of light] in the core and a polytropic equation with constant adiabatic index Gamma_1 = [dlnP/dln rho ] in the envelope and obtained a stable configuration with a maximum value of u =~ 0.3574 when the ratio of pressure to density at the core-envelope boundary reaches about 0.014. The maximum mass of neutron star based upon this model comes out to be 7.944 M_sun, if the (average) density of the configuration is constrained by fastest rotating pulsar, with rotation period, Prot =~ 1.558 ms, known to date. The average density of the configuration turns out to be 1.072 x 1014 g cm-3. The model gives dynamically stable configurations with compaction parameter u [equiv (M/R) , where M equiv mass and R equiv radius of the structure] > (1/3) which are important to study Ultra-Compact Objects [UCOs]. The theoretically obtained maximum value of u is also important regarding millisecond oscillations seen during X-Ray burst (if they are produced due to spin modulation) from a rotating neutron star, because the maximum modulation amplitude depends only upon the compaction parameter and the observed value of this amplitude provides a tool for testing theoretical models of neutron stars. The M(envelope)/M(star) ratio corresponds to a value ~ 10-2 which may be relevant in explaining the rotational irregularities in pulsars known as the timing noise and glitches.

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