Rotating protoneutron stars: Spin evolution, maximum mass, and I-Love-Q relations

Grégoire Martinon, Andrea Maselli, Leonardo Gualtieri, and Valeria Ferrari
Phys. Rev. D 90, 064026 – Published 12 September 2014

Abstract

Shortly after its birth in a gravitational collapse, a protoneutron star enters in a phase of quasistationary evolution characterized by large gradients of the thermodynamical variables and intense neutrino emission. In a few tens of seconds, the gradients smooth out while the star contracts and cools down, until it becomes a neutron star. In this paper we study this phase of the protoneutron star life including rotation, and employing finite-temperature equations of state. We model the evolution of the rotation rate, and determine the relevant quantities characterizing the star. Our results show that an isolated neutron star cannot reach, at the end of the evolution, the maximum values of mass and rotation rate allowed by the zero-temperature equation of state. Moreover, a mature neutron star evolved in isolation cannot rotate too rapidly, even if it is born from a protoneutron star rotating at the mass-shedding limit. We also show that the I-Love-Q relations are violated in the first second of life, but they are satisfied as soon as the entropy gradients smooth out.

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  • Received 3 July 2014

DOI:https://doi.org/10.1103/PhysRevD.90.064026

© 2014 American Physical Society

Authors & Affiliations

Grégoire Martinon1,2,*, Andrea Maselli1,3,†, Leonardo Gualtieri1,3,‡, and Valeria Ferrari1,3,§

  • 1Dipartimento di Fisica, Sapienza, Università di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy
  • 2Département de Physique, École Normale Supérieure de Cachan, 61 Avenue du Président Wilson, 94235 Cachan, France
  • 3Sezione INFN Roma1, Piazzale Aldo Moro 2, 00185 Roma, Italy

  • *gregoire.martinon@ens-cachan.fr
  • andrea.maselli@roma1.infn.it
  • leonardo.gualtieri@roma1.infn.it
  • §valeria.ferrari@roma1.infn.it

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Vol. 90, Iss. 6 — 15 September 2014

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