Abstract
In this paper, we discuss the impact of rotation on the particle composition of rotating neutron stars (pulsars). Particular emphasis is put on the formation of quark matter during stellar spin-down, driven by continuous gravitational compression. Our study is based on modern models for the nuclear equation of state whose parameters are tightly constrained by nuclear data, neutron star masses, and the latest estimates of neutron star radii.
Highlights
Most of the neutron star calculations reported in the literature have been performed for non-rotating, spherically symmetric stellar configurations, whose properties are uniquely determined by the Oppenheimer-Volkoff equation 1,2
The true nature of the matter deep in the cores of rotating neutron stars is still largely unknown despite several decades of intense research on this topic. In this short overview paper, we present the results of recent 3 neutron star calculations performed for a non-local extension of the SU(3) Nambu–Jona-Lasinio (NJL) model to investigate the possible existence of deconfined quarks in the cores of neutron stars
As shown in this paper, the type and structure of the matter in the cores of rotating neutron stars depends sensitively on the star’s spin frequency 2,10,18. Exploring this feature in more details opens up a new window on the type of matter that exists in the central cores of neutron stars
Summary
Most of the neutron star calculations reported in the literature have been performed for non-rotating, spherically symmetric stellar configurations, whose properties are uniquely determined by the Oppenheimer-Volkoff equation 1,2. A steady increase in the number of observed rotating neutron stars with rotational periods in the millisecond range has renewed considerable interest in the influence and implications of rapid rotation on the properties of neutron stars. Details about these equations of state (EoS) can be found in the recent paper by Mellinger et al 3 and in the contribution of Contrera et al 4 contained elsewhere in this volume
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