|
|
Effects of the symmetry energy slope on the axial oscillations of neutron stars |
Wen De-Hua (文德华), Zhou Ying (周颖) |
Department of Physics, South China University of Technology, Guangzhou 510641, China |
|
|
Abstract The impact of symmetry energy slope L on the axial w-mode oscillations is explored, where the range of the constrained slope L of symmetry energy at saturation density is adopted from 25 MeV to 115 MeV while keeping the equation of state (EOS) of symmetric nuclear matter fixed. Based on the range of the symmetry energy slope, a constraint on the frequency and damping time of the wI-mode of the neutron star is given. It is found that there is a perfect linear relation between the frequency and the stellar mass for a fixed slope L, and the softer symmetry energy corresponds to a higher frequency. Moreover, it is confirmed that both the frequencies and damping times have a perfect universal scaling behavior for the EOSs with different symmetry energy slopes at saturation density.
|
Received: 28 November 2012
Revised: 26 February 2013
Accepted manuscript online:
|
PACS:
|
04.40.Dg
|
(Relativistic stars: structure, stability, and oscillations)
|
|
26.60.-c
|
(Nuclear matter aspects of neutron stars)
|
|
97.60.Jd
|
(Neutron stars)
|
|
Fund: Project supported by the National Natural Science Foundation of China (Grant Nos. 10947023 and 11275073), the Fundamental Research Funds for the Central Universities (Grant No. 2012ZZ0079), and sponsored by SRF for ROCS, SEM. This research has made use of NASA's Astrophysics Data System. |
Corresponding Authors:
Wen De-Hua
E-mail: wendehua@scut.edu.cn
|
Cite this article:
Wen De-Hua (文德华), Zhou Ying (周颖) Effects of the symmetry energy slope on the axial oscillations of neutron stars 2013 Chin. Phys. B 22 080401
|
[1] |
Thorne K S and Campolattaro A 1967 ApJ 149 591
|
[2] |
Lindblom L and Detweiler S 1983 ApJS 53 73
|
[3] |
Chandrasekhar S and Ferrari V 1991 Proc. R. Soc. Lond. A 432 247
|
[4] |
Chandrasekhar S and Ferrari V 1991 Proc. R. Soc. Lond. A 434 449
|
[5] |
Kokkotas K D and Schutz B F 1992 MNRAS 255 119
|
[6] |
Andersson N and Kokkotas K D 1998 MNRAS 299 1059
|
[7] |
Benhar O, Berti E and Ferrari V 1999 MNRAS 310 797
|
[8] |
Wen D H, Li B A and Krastev P G 2009 Phys. Rev. C 80 025801
|
[9] |
Lattimer J M and Prakash M 2004 Science 304 536
|
[10] |
Lattimer J M and Prakash M 2007 Phys. Rep. 442 109
|
[11] |
Li B A, Chen L W and Ko C M 2008 Phys. Rep. 464 113
|
[12] |
Wen D H and Chen W 2011 Chin. Phys. B 20 029701
|
[13] |
Wen D H 2010 Chin. Phys. Lett. 27 010401
|
[14] |
Xiao Z G, Li B A, Chen L W, Yong G C and Zhang M 2009 Phys. Rev. Lett. 102 062502
|
[15] |
Tsang M B, Zhang Y X, Danielewicz P, Famiano M, Li Z X, Lynch W G and Steiner A W 2009 Phys. Rev. Lett. 102 122701
|
[16] |
Centelles M, Roca-Maza X, Vinas X and Warda M 2009 Phys. Rev. Lett. 102 122502
|
[17] |
Lehaut G, Gulminelli F and Lopez O 2009 Phys. Rev. Lett. 102 142503
|
[18] |
Chen L W, Ko C M and Li B A 2005 Phys. Rev. Lett. 94 032701
|
[19] |
Li B A and Chen L W 2005 Phys. Rev. C 72 064611
|
[20] |
Shetty D V, Yennello S J and Souliotis G A 2007 Phys. Rev. C 76 024606
|
[21] |
Klimkiewicz A et al. 2007 Phys. Rev. C 76 051603
|
[22] |
Danielewicz P and Lee J 2007 AIPC Conf. Proc. 947 301
|
[23] |
Chen L W, Ko C M, Li B A and Xu J 2010 Phys. Rev. C 82 024321
|
[24] |
Xu C, Li B A and Chen L W 2010 Phys. Rev. C 82 054607
|
[25] |
Newton W G, Gearheart M and Li B A 2011 arXiv: 1110.4043v1
|
[26] |
Wen D H, Newton W G and Li B A 2012 Phys. Rev. C 85 025801
|
[27] |
Chen L W, Cai B J, Ko C M, Li B A, Shen C and Xu J 2009 Phys. Rev. C 80 014322
|
[28] |
Liu M, Wang N, Li Z X and Zhang F S 2012 Phys. Rev. C 82 064306
|
[29] |
Roca-Maza X, Centelles M, Vinas X and Warda M 2011 Phys. Rev. Lett. 106 252501
|
[30] |
Steiner A W and Gandolfi S 2012 Phys. Rev. Lett. 108 081102
|
[31] |
Hebeler K, Lattimer J M, Pethick C J and Schwenk A 2010 Phys. Rev. Lett. 105 161102
|
[32] |
Gandolfi S, Carlson J and Reddy S 2012 Phys. Rev. C 85 032801
|
[33] |
Demorest P B, Pennucci T, Ransom S M, Roberts M S E and Hessels J W T 2010 Nature 467 1081
|
[34] |
Steiner A W, Lattimer J M and Brown E F 2010 Astrophys. J. 722 33
|
[35] |
Leins Nollert H P and Soffel M H 1993 Phys. Rev. D 48 3467
|
[36] |
Wen D H, Yan J and Liu X M 2012 Chin. Phys. B 21 060402
|
[37] |
Tsui L K and Leung P T 2005 MNRAS 357 1029
|
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
|
|
|