The massive pulsar PSR J1614-2230: Linking quantum chromodynamics, gamma-ray bursts, and gravitational wave astronomy

Feryal Özel, Dimitrios Psaltis, Scott Ransom, Paul Demorest, Mark Alford

Research output: Contribution to journalArticle

105 Scopus citations

Abstract

The recent measurement of the Shapiro delay in the radio pulsar PSR J1614-2230 yielded amass of 1.97±0.04M, making it the most massive pulsar known to date. Its mass is high enough that, even without an accompanying measurement of the stellar radius, it has a strong impact on our understanding of nuclear matter, gamma-ray bursts (GRBs), and the generation of gravitational waves from coalescing neutron stars. This single high-mass value indicates that a transition to quark matter in neutron-star cores can occur at densities comparable to the nuclear saturation density only if the quarks are strongly interacting and are color superconducting. We further show that a high maximum neutron-star mass is required if short-duration GRBs are powered by coalescing neutron stars and, therefore, this mechanism becomes viable in the light of the recent measurement. Finally, we argue that the low-frequency (≤500 Hz) gravitational waves emitted during the final stages of neutron-star coalescence encode the properties of the equation of state because neutron stars consistent with this measurement cannot be centrally condensed. This will facilitate the measurement of the neutron star equation of state with Advanced LIGO/Virgo.

Original languageEnglish (US)
Pages (from-to)L199-L202
JournalAstrophysical Journal Letters
Volume724
Issue number2 PART 2
DOIs
StatePublished - Dec 1 2010

Keywords

  • Gamma-ray burst:general
  • Pulsars:individual (PSR J1614-2230)
  • Stars:neutron

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Fingerprint Dive into the research topics of 'The massive pulsar PSR J1614-2230: Linking quantum chromodynamics, gamma-ray bursts, and gravitational wave astronomy'. Together they form a unique fingerprint.

  • Cite this