Equation of state constraints from neutron stars

Details Equation of state constraints from neutron stars Equation of state constraints from neutron stars

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007ap%26ss.308..371l&link_type=abstract

Astrophysics and Space Science, Volume 308, Issue 1-4, pp. 371-379

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

Recent measurements of thermal radiation from neutron stars have suggested a rather broad range of radiation radii ( R_{infty}=R/sqrt{1-2GM/Rc2} ). Sources in M13 and Omega Cen imply R ∞˜12-14 km, but X7 in 47 Tuc implies R ∞˜16-20 km and RX J1856-3754 R ∞>17 km. If these measurements are all correct, only a limited selection of EOS’s could be consistent with them, but a broad range of neutron star masses (up to 2 M&sun;) would also be necessary. The surviving equations of state are incompatible with significant softening above nuclear saturation densities, such as would occur with Boson condensates, a low-density quark-hadron transition, or hyperons. Other potential constraints, such as from QPO’s, radio pulsar mass and moment of inertia measurements, and neutron star cooling, are compared.

Affiliated with

Also associated with

No associations

Rating

Equation of state constraints from neutron stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Equation of state constraints from neutron stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Equation of state constraints from neutron stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1682458