Moments of inertia for neutron and strange stars: Limits derived for the Crab pulsar

By Michal Bejger, P. Haensel. 2002

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Recent estimates of the properties of the Crab nebula are used to derive constraints on the moment of inertia, mass and radius of the pulsar. To this purpose, we employ an approximate formula combining these three parameters. Our "empirical formula" I ' a(x)MR 2 ,w herex = (M=M)(km=R), is based on numerical results obtained for thirty theoretical equations of state of dense matter. The functions a(x) for neutron stars and strange stars are qualitatively dierent. For neutron stars aNS(x)= x=(0:1+ 2x )f orx 0:1 (valid for M> 0:2 M )a ndaNS(x)= 2 (1+ 5x )f orx> 0:1. For strange stars aSS(x)= 2 (1+ x) (not valid for strange stars with crust and M 1:2 M and RCrab = 10-14 km. Setting the most recent evaluation ("central value") Mneb = 4:6 M rules out most of the existing equations of state, leaving only the stiest ones: MCrab> 1:9 M, RCrab= 14-15 km.

Subfields: Astronomy and Astrophysics, Oceanography, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/360cba7987afa161c15647506935ef3b05a631f3

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Citations in the corpus

Constraining the Equation of State with Moment of Inertia Measurements (2004, background): “…M 1:0 M , this relation can be approximated by I ’ (0:237 0:008)MR2 1þ 4:2M km M R þ 90 M km M R 4" # : ð12Þ An analogous fit has also been suggested by Bejger & Haensel (2002): I ’ 2 9 1þ 5M km R M ð13Þ for M /R > 0:1M km 1; however, this fit underestimates I for the largest neutron star…”
Maximum mass, moment of inertia and compactness of relativistic stars (2016, methodology): “Expressions of this type have been proposed by Lattimer & Prakash (2001), as well as by Bejger & Haensel (2002), with comparable level of precision.”
Born–Infeld inspired modifications of gravity (2017, background): “In particular, a correlation between the scaled moment of inertia I/MR2 and the compactness M/R has been observed [57, 239].”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “A decade later, Bejger and Haensel [62] and then Lattimer and Schutz [67] studied the relation between C and ĪC2 = I/(MR2) (motivated by the fact that I ∝ MR2 for Newtonian polytropes).”