Article ID | Journal | Published Year | Pages | File Type |
---|---|---|---|---|
5487772 | New Astronomy | 2017 | 11 Pages |
Abstract
The recent fast growth of a population of millisecond pulsars with precisely measured mass provides an excellent opportunity to characterize these compact stars at an unprecedented level. This is because the stellar parameter values can be accurately computed for known mass and spin rate and an assumed equation of state (EoS) model. For each of the 16 such pulsars and for a set of EoS models from nucleonic, hyperonic, strange quark matter and hybrid classes, we numerically compute fast spinning stable stellar parameter values considering the full effect of general relativity. This first detailed catalogue of the computed parameter values of observed millisecond pulsars provides a testbed to probe the physics of compact stars, including their formation, evolution and EoS. We estimate uncertainties on these computed values from the uncertainty of the measured mass, which could be useful to quantitatively constrain EoS models. We note that the largest value of the central density Ïc in our catalogue is â¼5.8 times the nuclear saturation density Ïsat, which is much less than the expected maximum value 13Ïsat. We argue that the Ïc-values of at most a small fraction of compact stars could be much larger than 5.8Ïsat. Besides, we find that the constraints on EoS models from accurate radius measurements could be significantly biased for some of our pulsars, if stellar spinning configurations are not used to compute the theoretical radius values.
Related Topics
Physical Sciences and Engineering
Physics and Astronomy
Astronomy and Astrophysics
Authors
Sudip Bhattacharyya, Ignazio Bombaci, Debades Bandyopadhyay, Arun V. Thampan, Domenico Logoteta,