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07 February 2025
 
  » arxiv » astro-ph/0107154

 Article overview



Rotating Skyrmion Stars
Rachid OUYED ;
Date 9 Jul 2001
Subject astro-ph
AffiliationNORDITA, Copenhagen, Denmark
AbstractIn a previous paper, using an equation of state of dense matter representing a fluid of Skyrmions we constructed the corresponding non-rotating compact-star models in hydrostatic equilibrium; these are mostly fluid stars (the Skyrmion fluid) thus naming them {it Skyrmion Stars}. Here we generalize our previous calculations by constructing equilibrium sequences of rotating Skyrmion stars in general relativity using the computer code {it RNS} developed by Stergioulas. We calculated their masses and radii to be 0.4 le M/M_{odot} le 3.45, and 13.0 { m km}le Rle 23.0 { m km}, respectively (R being the circumferential radius of the star). The period of the maximally rotating Skyrmion stars is calculated to be 0.8 { m ms}le P le 2.0 { m ms}. We find that a gap (the height between the star surface and the inner stable circular orbit) starts to appear for Msim 2.0M_{odot}. Specifically, the Skyrmion star mass range with an existing gap is calculated to be 1.8 < M/ M_{odot} < 3.0 with the corresponding orbital frequency 0.8 { m kHz} < u_{ m ISCO} < 1.3 { m kHz}. We apply our model to the 4U 1820-30 low mass X-ray binary and suggest a plausible Skyrmion star candidate in the 4U 1636-53 system. We discuss the difficulties encountered by our model in the 4U 0614+09 case with the highest known Quasi-Periodic Oscillation frequency of 1329 Hz. A comparative study of Skyrmion stars and models of neutron stars based on recent/modern equations of state is also presented.
Source arXiv, astro-ph/0107154
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