Effect of magnetic field decay on the chemical heating of cooling neutron stars

ZHOU Xia; KANG Miao; WANG Na

doi:10.1088/1674-1137/37/8/085102

Chinese Physics C> 2013, Vol. 37> Issue(8) : 085102 DOI: 10.1088/1674-1137/37/8/085102

Effect of magnetic field decay on the chemical heating of cooling neutron stars

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Abstract：
The effect of magnetic field decay on the chemical heating and thermal evolution of neutron stars is discussed in this paper. Our main goal is to study how the chemical heating mechanism and thermal evolution are changed by the field decay and how the magnetic field decay is modified by the thermal evolution. We compare stars cooling with chemical heating with one without chemical heating and find that the decay of the magnetic field is delayed significantly by the chemical heating. We find that the effect of chemical heating has been suppressed through the decaying magnetic field by the spin-down of the stars at a later stage. Compared with typical chemical heating, we find the decay of the magnetic field can even cause the surface temperature to turn down at an older age. When we discuss the cooling of neutron stars, we should consider the coupling effect of the magnetic field and the rotational evolution of neutron stars on the heating mechanisms.

References

[1]

Becker W. Vol. 357. eds. Astrophys. Space Sci. Library, Neutron Stars and Pulsars, New-York: Springer, 2008[2] Glendenning N K. Compact Stars: Nuclear Physics, Particle Physics, and General Relativity. New-York: Springer, 2000[3] Yakovlev D G, Kaminker A D, Gnedin O Y, Haensel P. Phys. Rep., 2001, 354: 1[4] ZHENG X P, ZHOU X. Mon. Not. R. Astron. Soc., 2006, 371: 1659[5] ZHOU X, WANG L Z, ZHOU A Z. Publ. Astron. Soc. Pac., 2007, 119: 1367[6] Becker W, Trümper J. Astron. Astrophys, 1997, 326: 682[7] Kargaltsev O, Pavlov G G, Romani R W. Astrophys. J, 2004, 602: 327[8] Mignani R, Caraveo P A, Bignami G F. Astron. Astrophys, 1997, 323: 797[9] Pavlov G G, Stringfellow G S, Córdova F A. Astrophys. J, 1996, 467: 370[10] Page D, Geppert U, Weber F. Nucl. Phys. A, 2006, 777: 497[11] CHENG K S, DAI Z G. Astrophys. J, 1996, 468: 819[12] Fernández R, Reisenegger A. Astrophys. J, 2005, 625: 291[13] Reisenegger A. Astrophys. J, 1995, 442: 749[14] Iida K, Sato K. Astrophys. J, 1997, 477: 294[15] CHENG K S, CHAU W Y, ZHANG J L, CHAU H F. Astrophys. J, 1992, 396: 135[16] YANG S H, ZHENG X P, PI C M, YU Y W. Mon. Not. R. Astron. Soc., 2010, 403: 2007[17] ZHENG X P, YU Y W. Astron. Astrophys, 2006, 445: 627[18] KANG M, WANG X D, ZHENG X P. New Astron, 2010, 15: 515[19] Goldreich P, Reisenegger A. Astrophys. J, 1992, 395: 250[20] Heyl J S, Hernquist L. Astrophys. J, 1997, 491: L95[21] Heyl J S, Kulkarni S R. Astrophys. J, 1998, 506: L61[22] Miralles J A, Urpin V, Konenkov D. Astrophys. J, 1998, 503: 368[23] Aguilera D N, Pons J A, Miralles J A. Astron. Astrophys, 2008, 486: 255[24] Paula J, Reisenegger A, Fernández R. Phys. Rev. Lett., 2006, 97: 131102[25] Petrovichand C, Reisenegger A. Astron. Astrophys, 2010, 521: A77[26] Urpin V, Konenkov D. Astron. Astrophys, 2008, 483: 223[27] Tsuruta S. Phys. Rep., 1998, 292: 1[28] Yakovlev D G, Pethick C J. Annu. Rev. Astron. Astrophys, 2004, 42: 169[29] Gudmundsson E H, Pethick C J, Epstein R I. Astrophys. J, 1983, 272: 286[30] Gnedin O Y, Yakovlev D G, Potekhin A Y. Mon. Not. R. Astron. Soc., 2001, 324: 725[31] Wiringa R B, Fiks V, Fabrocini A. Phys. Rev. C, 1988, 38: 1010[32] Glampedakis K, Jones D I, Samuelsson L. Mon. Not. R. Astron. Soc., 2011, 413: 2021

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ZHOU Xia, KANG Miao and WANG Na. Effect of magnetic field decay on the chemical heating of cooling neutron stars[J]. Chinese Physics C, 2013, 37(8): 085102. doi: 10.1088/1674-1137/37/8/085102

ZHOU Xia, KANG Miao and WANG Na. Effect of magnetic field decay on the chemical heating of cooling neutron stars[J]. Chinese Physics C, 2013, 37(8): 085102. doi: 10.1088/1674-1137/37/8/085102 shu

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Received: 2012-09-03
Revised: 1900-01-01

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通讯作者: 陈斌, bchen63@163.com

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沈阳化工大学材料科学与工程学院沈阳 110142

Effect of magnetic field decay on the chemical heating of cooling neutron stars

Corresponding author: ZHOU Xia,

Received Date: 2012-09-03

Accepted Date: 1900-01-01

Available Online: 2013-08-05

Abstract: The effect of magnetic field decay on the chemical heating and thermal evolution of neutron stars is discussed in this paper. Our main goal is to study how the chemical heating mechanism and thermal evolution are changed by the field decay and how the magnetic field decay is modified by the thermal evolution. We compare stars cooling with chemical heating with one without chemical heating and find that the decay of the magnetic field is delayed significantly by the chemical heating. We find that the effect of chemical heating has been suppressed through the decaying magnetic field by the spin-down of the stars at a later stage. Compared with typical chemical heating, we find the decay of the magnetic field can even cause the surface temperature to turn down at an older age. When we discuss the cooling of neutron stars, we should consider the coupling effect of the magnetic field and the rotational evolution of neutron stars on the heating mechanisms.

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Effect of magnetic field decay on the chemical heating of cooling neutron stars

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