STUCHLÍK, Zdeněk, Martin URBANEC and John MILLER. Quadrupole moments of rotating neutron stars and strange stars. Monthly Notices of the Royal Astronomical Society. GB - Spojené království Velké Británie a, 2013, vol. 433, No 3, p. 1903-1910, 7 pp. ISSN 0035-8711. Available from: https://dx.doi.org/10.1093/mnras/stt858.
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Basic information
Original name Quadrupole moments of rotating neutron stars and strange stars
Authors STUCHLÍK, Zdeněk, Martin URBANEC and John MILLER.
Edition Monthly Notices of the Royal Astronomical Society, GB - Spojené království Velké Británie a, 2013, 0035-8711.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Confidentiality degree is not subject to a state or trade secret
WWW URL
Organization unit Faculty of Philosophy and Science in Opava
Doi http://dx.doi.org/10.1093/mnras/stt858
UT WoS 000322403800010
Keywords in English stars: neutron; stars: rotation
Tags , GPP209-12P740, LC06014, MSM4781305903
Tags International impact, Reviewed
Links GPP209/12/P740, research and development project. LC06014, research and development project. MSM4781305903, plan (intention).
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 14/4/2021 15:34.
Abstract
We present results for models of neutron stars and strange stars constructed using the Hartle-Thorne slow-rotation method with a wide range of equations of state, focusing on the values obtained for the angular momentum J and the quadrupole moment Q, when the gravitational mass M and the rotational frequency are specified. Building on previous work, which showed surprising uniformity in the behaviour of the moment of inertia for neutron-star models constructed with widely different equations of state, we find similar uniformity for the quadrupole moment. These two quantities, together with the mass, are fundamental for determining the vacuum space-time outside neutron stars. We study particularly the dimensionless combination of parameters QM/J(2) (using units for which c = G = 1). This quantity goes to 1 in the case of a Kerr-metric black hole and deviations away from 1 then characterize the difference between neutron-star and black hole space-time. It is found that QM/J(2) for both n
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