de.mpg.escidoc.pubman.appbase.FacesBean
English
 
Help Guide Disclaimer Contact us Login
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Gravitational Radiation limit on the Spin of Young Neutron Stars

Andersson, N., Kokkotas, K. D., & Schutz, B. F. (1999). Gravitational Radiation limit on the Spin of Young Neutron Stars. The Astrophysical Journal, 510, 846-853. doi:10.1086/306625.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-7437-1 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0013-743A-C
Genre: Journal Article

Files

show Files
hide Files
:
60232.pdf (Any fulltext), 124KB
Description:
-
Visibility:
Public
MIME-Type / Checksum:
application/pdf
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Andersson, Nils1, Author
Kokkotas, Kostas D.1, Author
Schutz, Bernard F.2, Author              
Affiliations:
1External Organizations, escidoc:persistent22              
2Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, escidoc:24013              

Content

show
hide
Free keywords: -
 Abstract: A newly discovered instability in rotating neutron stars, driven by gravitational radiation reaction acting on the starsœ r-modes, is shown here to set an upper limit on the spin rate of young neutron stars. We calculate the timescales for the growth of linear perturbations due to gravitational radiation reaction, and for dissipation by shear and bulk viscosity, working to second order in a slow-rotation expansion within a Newtonian polytropic stellar model. The results are very temperature-sensitive : in hot neutron stars (T [109 K), the lowest-order r-modes are unstable, while in colder stars they are damped by viscosity. These calculations have a number of interesting astrophysical implications. First, the r-mode instability will spin down a newly born neutron star to a period close to the initial period inferred for the Crab pulsar, probably between 10 and 20 ms. Second, as an initially rapidly rotating star spins down, an energy equivalent to roughly 1% of a solar mass is radiated as gravitational waves, which makes the process an interesting source for detectable gravitational waves. Third, the r-mode instability rules out the scenario in which millisecond pulsars are formed by accretion-induced collapse of a white dwarf; the new star would be hot enough to spin down to much slower rates. Stars with periods less than perhaps 10 ms must have been formed by spin-up through accretion in binary systems, where they remain colder than the Eddington temperature of about 108 K. More accurate calculations will be required to de–ne the limiting spin period more reliably, and we discuss the importance of the major uncertainties in the stellar models, in the initial conditions after collapse, and in the physics of cooling, super—uidity, and the equation of state.

Details

show
hide
Language(s):
 Dates: 1999-01-10
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Method: Peer
 Identifiers: eDoc: 60232
DOI: 10.1086/306625
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: The Astrophysical Journal
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 510 Sequence Number: - Start / End Page: 846 - 853 Identifier: ISSN: 0004-637x