Gravitational waves from low mass neutron stars

C. J. Horowitz
Phys. Rev. D 81, 103001 – Published 3 May 2010

Abstract

Low mass neutron stars may be uniquely strong sources of gravitational waves. The neutron star crust can support large deformations for low mass stars. This is because of the star’s weaker gravity. We find maximum ellipticities ϵ (fractional difference in moments of inertia) that are 1000 times larger, and maximum quadrupole moments Q22 over 100 times larger, for low mass stars than for 1.4M neutron stars. Indeed, we calculate that the crust can support an ϵ as large as 0.005 for a minimum mass neutron star. A 0.12M star, that is maximally strained and rotating at 100 Hz, will produce a characteristic gravitational wave strain of h0=2.1×1024 at a distance of 1 kpc. The gravitational wave detector Advanced LIGO should be sensitive to such objects through out the Milky Way Galaxy. A low mass neutron star could be uniquely identified from a large observed spin down rate and its discovery would have important implications for general relativity, supernova mechanisms, and possibly nucleosynthesis.

  • Figure
  • Figure
  • Figure
  • Received 9 December 2009

DOI:https://doi.org/10.1103/PhysRevD.81.103001

©2010 American Physical Society

Authors & Affiliations

C. J. Horowitz*

  • Department of Physics and Nuclear Theory Center, Indiana University, Bloomington, Indiana 47405, USA

  • *horowit@indiana.edu

Article Text (Subscription Required)

Click to Expand

References (Subscription Required)

Click to Expand
Issue

Vol. 81, Iss. 10 — 15 May 2010

Reuse & Permissions
Access Options
Author publication services for translation and copyediting assistance advertisement

Authorization Required


×
×

Images

×

Sign up to receive regular email alerts from Physical Review D

Log In

Cancel
×

Search


Article Lookup

Paste a citation or DOI

Enter a citation
×