Surface gravity of neutron stars and strange stars

M. Bejger; P. Haensel

doi:10.1051/0004-6361:20034538

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Volume 420 / No 3 (June IV 2004)

A&A, 420 3 (2004) 987-991

Abstract

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Issue		A&A Volume 420, Number 3, June IV 2004


Page(s)		987 - 991
Section		Stellar structure and evolution
DOI		https://doi.org/10.1051/0004-6361:20034538
Published online		04 June 2004

A&A 420, 987-991 (2004)

Surface gravity of neutron stars and strange stars

M. Bejger¹ and P. Haensel¹^,2

¹ N. Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland
² LUTH du CNRS, Observatoire de Paris, 92195 Meudon Cedex, France e-mail: haensel@camk.edu.pl

Corresponding author: M. Bejger, bejger@camk.edu.pl

Received: 20 October 2003
Accepted: 28 February 2004

Abstract

The upper bound on the value of the surface gravity, g_s, for neutron stars with equations of state respecting $v_{\rm sound}\le c$ , is derived. This bound is inversely proportional to the maximum allowable mass M_max, and it reads $g_{\rm s}\le 1.411 \times 10^{15}\;({M_{\rm max} /{ M}_\odot})^{-1}~{\rm cm~s^{-2}}$ . It implies an absolute upper bound $7.4\times 10^{14}~{\rm cm\, s^{-2}}$ if one uses the $2\sigma$ lower bound on the neutron mass measured recently in 4U1700-37, $1.9 ~M_{\odot}$ . A correlation between g_s and the compactness parameter $2GM/Rc^2$ for baryonic stars is analyzed. The properties of g_s of strange quark stars and its upper bounds are discussed using the scaling properties of the strange-star models.

Key words: dense matter / equation of state / stars: neutron

© ESO, 2004

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