THE MASS AND RADIUS OF THE NEUTRON STAR IN EXO 1745-248


Ozel F., Guver T. , Psaltis D.

ASTROPHYSICAL JOURNAL, vol.693, no.2, pp.1775-1779, 2009 (Peer-Reviewed Journal) identifier identifier

  • Publication Type: Article / Article
  • Volume: 693 Issue: 2
  • Publication Date: 2009
  • Doi Number: 10.1088/0004-637x/693/2/1775
  • Journal Name: ASTROPHYSICAL JOURNAL
  • Journal Indexes: Science Citation Index Expanded, Scopus
  • Page Numbers: pp.1775-1779
  • Keywords: stars: neutron, X-rays: individual (EXO 1745-248), X-RAY-BURSTS, GLOBULAR-CLUSTER TERZAN-5, EQUATION-OF-STATE, SPECTRA, EXO-0748-676, CONSTRAINTS, PHOTOMETRY, DISCOVERY, MATTER

Abstract

Bursting X-ray binaries in globular clusters are ideal sources for measuring neutron star masses and radii, and hence, for determining the equation of state of cold, ultradense matter. We use time-resolved spectroscopic data from EXO 1745-248 during thermonuclear bursts that show strong evidence for photospheric radius expansion to measure the Eddington flux and the apparent surface area of the neutron star. We combine this with the recent measurement of the distance to the globular cluster Terzan 5, where this source resides, to measure the neutron star mass and radius. We find tightly constrained pairs of values for the mass and radius, which are centered around M = 1.4 M sun and R = 11 km or around M = 1.7 Msun and R = 9 km. These values favor nucleonic equations of state with symmetry energy that is relatively low and has a weak dependence on density.

Bursting X-ray binaries in globular clusters are ideal sources for measuring neutron star masses and radii, and hence, for determining the equation of state of cold, ultradense matter. We use time-resolved spectroscopic data from EXO 1745-248 during thermonuclear bursts that show strong evidence for photospheric radius expansion to measure the Eddington flux and the apparent surface area of the neutron star. We combine this with the recent measurement of the distance to the globular cluster Terzan 5, where this source resides, to measure the neutron star mass and radius. We find tightly constrained pairs of values for the mass and radius, which are centered around M = 1.4 M(circle dot) and R = 11 km or around M = 1.7 M(circle dot) and R = 9 km. These values favor nucleonic equations of state with symmetry energy that is relatively low and has a weak dependence on density.