Spin-down of Relativistic Stars with Phase Transitions and PSR J0537-6910

Details Spin-down of Relativistic Stars with Phase Transitions and PSR J0537-6910 Spin-down of Relativistic Stars with Phase Transitions and PSR J0537-6910

2002-04-23

arxiv.org/abs/astro-ph/0204380v2

Astron.Astrophys. 395 (2002) 151-160

Astronomy and Astrophysics

Astrophysics

10 pages, 10 figures, additional results and conclusions, matches published version

Scientific paper

10.1051/0004-6361:20021289

Using a highly accurate numerical code, we study the spin down of rotating relativistic stars, undergoing a quark deconfinement phase transition. Such phase transitions have been suggested to yield an observable signal in the braking index of spinning-down pulsars, which is based on a ``backbending'' behaviour of the moment of inertia. We focus on a particular equation of state that has been used before to study this behaviour, and find that for the population of normal pulsars the moment of inertia does not exhibit a backbending behaviour. In contrast, for supramassive millisecond pulsars a very strong backbending behaviour is found. Essentially, once a quark core appears in a spinning-down supramassive millisecond pulsar, the star spins up and continues to do so until it reaches the instability to collapse. This strong spin-up behaviour makes it easier to distinguish a phase transition in such pulsars: a negative first time-derivative of the rotational period suffices and one does not have to measure the braking index. In the spin-up era, the usually adopted spin-down power law fails to describe the evolution of the angular velocity. We adopt a general-relativistic spin-down power law and derive the equations that describe the angular velocity and braking index evolution in rapidly rotating pulsars.

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