GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS |
Prev
|
|
|
Properties of hyperon stars rotating at Keplerian frequency |
Wen De-Hua(文德华)a)† and Chen Wei(陈伟)b) |
a Department of Physics, South China University of Technology, Guangzhou 510641, China; b Department of Physics, Jinan University, Guangzhou 510632, China |
|
|
Abstract The structure and properties of a Keplerian rotating hyperon star with an equation of state (EOS) investigated using the relativistic $\sigma$-$\omega$-$\rho$ model are examined by employing an accurate numerical scheme. It is shown that there is a clear rotating effect on the structure and properties, and that hyperon star matter cannot support a star with a mass larger than 1.9 M$\odot$, even a star rotating at the fastest allowed frequency. The constraints of the two known fastest rotating frequencies (716 Hz and 1122 Hz) on the mass and radius of a hyperon star are also explored. Furthermore, our results indicate that the imprint of the rapid rotation of a hyperon star on the moment of inertia is clear; the backward equatorial redshift, the forward equatorial redshift and the polar redshift can be distinguished clearly, the forward equatorial redshift is always negative; and its figuration is far from a spherical symmetric shape.
|
Received: 08 October 2009
Revised: 28 September 2010
Accepted manuscript online:
|
|
Fund: Project supported by the National Natural Science Foundation of China (Grant No. 10947023), and the Fundamental Research Funds for the Central University, China (Grant No. 2009ZM0193). |
Cite this article:
Wen De-Hua(文德华) and Chen Wei(陈伟) Properties of hyperon stars rotating at Keplerian frequency 2011 Chin. Phys. B 20 029701
|
[1] |
Li B A, Chen L W and Ko C M 2008 Phys. Rep. 464 113
|
[2] |
Wen D H, Li B A and Chen L W 2009 Phys. Rev. Lett. 103 211102
|
[3] |
Lattimer J M and Prakash M 2007 Phys. Rep. 442 109
|
[4] |
Lattimer J M and Prakash M 2004 Science 304 536
|
[5] |
Hessels J W T, Ransom S M, Stairs I H, et al. 2006 Science 311 1901
|
[6] |
Thorsett S E and Chakrabarty D 1999 ApJ 512 288
|
[7] |
Kaaret P, Prieskorn J, In't Z and J J M, et al. 2007 ApJ 657 L97
|
[8] |
Hartle J B 1967 ApJ 150 1005
|
[9] |
Hartle J B and Thorne K S 1968 ApJ 153 807
|
[10] |
Butterworth E M and Ipser J R 1975 ApJL 200 103
|
[11] |
Friedman J L, Ipser J R and Parker L 1986 ApJ 304 115
|
[12] |
Komatsu H, Eriguchi Y and Hachisu I 1989 MNRAS 237 355
|
[13] |
Cook G B, Shapiro S L and Teukolsky S A 1994 ApJ 422 273
|
[14] |
Stergioulas N and Friedman J L 1995 ApJ 444 306
|
[15] |
Krastev P G, Li B A and Worley A 2008 ApJ 676 1170
|
[16] |
Wen D H 2010 Chin. Phys. Lett. 27 010401
|
[17] |
G"uver T, "Ozel F, Lavers A C and Wroblewski P Astro-ph/0811.3979v1
|
[18] |
van der Meer A, Kaper L, van Kerkwijk M H, Heemskerk M H M and van den Heuvel E P J 2007 Astron. Astrophys. 473 523
|
[19] |
Galloway D K, Muno M P, Hartman J M, Psaltis D and Chakrabarty D Astro-ph/0608259v2
|
[20] |
Glendenning N K 1989 Nucl. Phys. A 493 521
|
[21] |
Glendenning N K and Moszkowski S A 1991 Phys. Rev. Lett. 67 2414
|
[22] |
Burgio G, Li A, Mi A J and Zuo W 2007 Chin. Phys. 16 1934
|
[23] |
Li A, Mi A and Zuo W 2007 Chin. Phys. 16 3290
|
[24] |
Glendenning N K 2001 Phys. Rev. C 64 025801
|
[25] |
Shen H 2002 Phys. Rev. C 65 035802
|
[26] |
Panda P K, Menezes D P and Providencia C 2004 Phys. Rev. C 69 025207
|
[27] |
Lackey B D, Nayyar M and Owen B J 2006 Phys. Rev. D 73 024021
|
[28] |
Yue P, Yang F and Shen H 2009 Phys. Rev. C 79 025803
|
[29] |
Chen W, Ai B Q and Liu L G 2001 Commun. Theor. Phys. 36 183
|
[30] |
Pethick C J, Ravenhall D G and Lorenz C P 1995 Nucl. Phys. A 584 675
|
[31] |
Haensel P and Pichon B 1994 Astron. Astrophys. 283 313
|
[32] |
Akmal A, Pandharipande V R and Ravenhall D G 1998 Phys. Rev. C 58 1804
|
[33] |
Tolman R C 1939 Phys. Rev. 55 364
|
[34] |
Oppenheimer J R and Volkoff G M 1939 Phys. Rev. 55 374
|
[35] |
Nozawa T, Stergioulas N, Gourgoulhon E and Eriguchi Y 1998 Astron. Astrophys. 132 431
|
[36] |
Butterworth E M and Ipser J R 1976 ApJ 204 200
|
[37] |
Morrison I A, Baumgarte T W, Shapiro S L and Pandharipande V R 2004 ApJL 617 135
|
[38] |
Lattimer J M and Schutz B F 2005 ApJ 629 979
|
[39] |
Haensel P, Zdunik J L, Bejger M and Lattimer J M Astro-ph/0901.1268V1
|
[40] |
Cottam J, Paerels F and Mendez M 2002 Nature 420 51
|
[41] |
Krastev P G, Li B A and Worley A 2008 Phys. Lett. B 668 1
|
[42] |
Cook G B, Shapiro S L and Teukolsky S A 1994 ApJ 424 823
|
[43] |
Ji P Y and Zhu J Y 2008 Chin. Phys. B 17 356
|
No Suggested Reading articles found! |
|
|
Viewed |
|
|
|
Full text
|
|
|
|
|
Abstract
|
|
|
|
|
Cited |
|
|
|
|
Altmetric
|
blogs
Facebook pages
Wikipedia page
Google+ users
|
Online attention
Altmetric calculates a score based on the online attention an article receives. Each coloured thread in the circle represents a different type of online attention. The number in the centre is the Altmetric score. Social media and mainstream news media are the main sources that calculate the score. Reference managers such as Mendeley are also tracked but do not contribute to the score. Older articles often score higher because they have had more time to get noticed. To account for this, Altmetric has included the context data for other articles of a similar age.
View more on Altmetrics
|
|
|