Slowly rotating ultra-compact Schwarzschild star in the gravastar limit

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19630%2F24%3AA0000376" target="_blank" >RIV/47813059:19630/24:A0000376 - isvavai.cz</a>
Result on the web
<a href="https://iopscience.iop.org/article/10.1088/1361-6382/ad1a52" target="_blank" >https://iopscience.iop.org/article/10.1088/1361-6382/ad1a52</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1088/1361-6382/ad1a52" target="_blank" >10.1088/1361-6382/ad1a52</a>

Result language
angličtina
Original language name
Slowly rotating ultra-compact Schwarzschild star in the gravastar limit
Original language description
We reconsider the problem of a slowly rotating homogeneous star, or Schwarzschild star, when its compactness goes beyond the Buchdahl bound and approaches the gravastar limit R -> 2M . We compute surface and integral properties of such configuration by integrating the Hartle-Thorne structure equations for slowly rotating relativistic masses, at second order in angular velocity. In the gravastar limit, we show that the metric of a slowly rotating Schwarzschild star agrees with the Kerr metric, thus, within this approximation, it is not possible to tell a gravastar from a Kerr black hole by any observations from the spacetime exterior to the horizon.
Czech name
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Czech description
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Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)

Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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