Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source

PI Chun-Mei; YANG Shu-Hua; ZHOU Xia; ZHOU Ai-Zhi

doi:10.1088/1674-1137/34/12/006

Chinese Physics C> 2010, Vol. 34> Issue(12) : 1818-1822 DOI: 10.1088/1674-1137/34/12/006

Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source

Abstract
HTML
Reference
Related

PDF

Abstract：
Employing phenomenological density-dependent critical temperatures of strong singlet-state proton pairing and of moderate triplet-state neutron pairing, we investigate the effects of rotochemical heating on the thermal evolution of superfluid neutron stars whose cores
consist of npe matter with the Akmal-Pandharipande-Ravenhall equation of state. Since the star is not quite in the weak interaction equilibrium state during spin-down, the departure from the chemical equilibrium leads to the rotochemical heating in a rotating NS which will increase the stellar's temperature. Our calculations show that the rotochemical heating delays the cooling of superfluid neutron stars considerably and makes the previous classification of NS cooling ambiguous. What's more, our model is currently consistent with all the observational data, and in particular some middle-aged and cold NSs (PRS J0205+6449 in 3C 58, PRS J1357-6429, RX J007.0+7303 in CTA 1, Vela) can be better explained when taking into account rotochemical heating.

References

[1]

Haensel P,Potekhin A Y,Yakovlev D G.Neutron Stars.1.Equation of State and Structure.New York:Springer,2007[2] Lattimer J M,Prakash M.Phys.Rep.,2007,442:109-165[3] Lattimer J M,Pethick C J,Prakash M,Haensel P.Phys.Rev.Lett.,1991,66:2701-2704[4] Lombardo U,Schulze H-J.Superfluidity in Neutron Star matter,in Physics of Neutron Star Interiors.Edited by Blaschke D,Glendenning N,Sedrakian A.Springer,Berlin,2001,30-53[5] Page D,Lattimer J M,Prakash M,Steiner A W.ApJSS,2004,155:623[6] Reisenegger A.ApJ,1995,442:749[7] Gusakov M E,Kaminker A D,Yakovlev D G,Gnedin O Y.MNRAS,2005,363:555[8] Yakovlev D G,Pethick C J.Ann.Rev.Astron.Astrophys.,2004,42:169[9] Kaminker A D,Haensel P,Yakovlev D G.AA,2001,373:L17[10] Flowers E G,Ruderman M,Sutherland P G.ApJ,1979,205:541[11] Haensel P.A A,1992,262:131[12] Yakovlev D G,Kaminker A D,Gnedin O Y,Haensel P.Phys.Rep.,2001,354:1[13] Fern(a)dez F,Reisenegger A.ApJ,2005,625:291[14] Akmal A,Pandharipande V R,Ravenhall D G.Phys.Rev.C,1998,58:1804[15] Heiselberg H,Hjorth-Jensen M.ApJ,1999,525:L45[16] Potekhin A Y,Yakovlev D G,Chabrier G,Gnedin O Y.ApJ,2003,594:404[17] Yakovlev D G,Gnedin O Y,Kaminker A D,Potekhin A Y.AIP Conf.Proc,2008,983:379

[1]	Ting-Ting Sun , Cheng-Jun Xia , Shi-Sheng Zhang , M. S. Smith . Massive neutron stars and Λ-hypernuclei in relativistic mean field models. Chinese Physics C, 2018, 42(2): 025101. doi: 10.1088/1674-1137/42/2/025101
[2]	A. H. Farajian , M. Bigdeli , S. Belbasi . LOCV calculation of the equations of state and properties of rapidly rotating neutron stars. Chinese Physics C, 2018, 42(6): 065102. doi: 10.1088/1674-1137/42/6/065102
[3]	Si-Na Wei , Rong-Yao Yang , Wei-Zhou Jiang . Crust-core properties of neutron stars in the Nambu-Jona-Lasinio model. Chinese Physics C, 2018, 42(5): 054103. doi: 10.1088/1674-1137/42/5/054103
[4]	Fei Wu , Chen Wu , Zhong-Zhou Ren . Neutron stars including the effects of chaotic magnetic fields and anomalous magnetic moments. Chinese Physics C, 2017, 41(4): 045102. doi: 10.1088/1674-1137/41/4/045102
[5]	Nai-Bo Zhang , Shou-Yu Wang , Bin Qi , Jian-Hua Gao , Bao-Yuan Sun . Neutrino emissivity of the nucleon direct URCA process for rotational traditional and hyperonic neutron stars. Chinese Physics C, 2017, 41(7): 075101. doi: 10.1088/1674-1137/41/7/075101
[6]	Cui Zhu , Xia Zhou , Na Wang . Rotational energy conversion and thermal evolution of neutron stars. Chinese Physics C, 2017, 41(12): 125104. doi: 10.1088/1674-1137/41/12/125104
[7]	Danial Salehi , Dariush Sardari , Salehi Jozani . Characteristics of a heavy water photoneutron source in boron neutron capture therapy. Chinese Physics C, 2013, 37(7): 078201. doi: 10.1088/1674-1137/37/7/078201
[8]	DING Wen-Bo , YU Zi , MI Geng , WANG Chun-Yan . Neutron star cooling in various sets of nucleon coupling constants. Chinese Physics C, 2013, 37(5): 055101. doi: 10.1088/1674-1137/37/5/055101
[9]	ZHOU Xia , KANG Miao , WANG Na . Effect of magnetic field decay on the chemical heating of cooling neutron stars. Chinese Physics C, 2013, 37(8): 085102. doi: 10.1088/1674-1137/37/8/085102
[10]	YANG Zhen-Wei , DING Ming-Ming , CHEN Shao-Min , WANG Zhe , ZHANG Feng , GAO Yuan-Ning . Simulation study of neutrino nucleus crosssection measurement in a segmented detectorat a spallation neutron source. Chinese Physics C, 2012, 36(6): 538-543 . doi: 10.1088/1674-1137/36/6/010
[11]	WEI Wei , CHEN Lei-Lei . Rotochemical heating in hybrid stars withmodified Urca reactions in operation. Chinese Physics C, 2012, 36(7): 601-604. doi: 10.1088/1674-1137/36/7/006
[12]	YU Zi , DING Wen-Bo . Effects of the δ meson on the direct Urca processes in neutron stars. Chinese Physics C, 2011, 35(9): 812-816. doi: 10.1088/1674-1137/35/9/004
[13]	WU Qing-Biao , WANG Qing-Bin , WU Jing-Min , MA Zhong-Jian . Study on induced radioactivity of China Spallation Neutron Source. Chinese Physics C, 2011, 35(6): 596-602. doi: 10.1088/1674-1137/35/6/017
[14]	LIU Xiao-Jin , WU Chen , REN Zhong-Zhou . Effects of the density dependence of the symmetry energy on neutron stars. Chinese Physics C, 2010, 34(11): 1709-1713. doi: 10.1088/1674-1137/34/11/008
[15]	WANG Song-Lin , HUANG Han-Xiong , RUAN Xi-Chao , LI Xia , BAO Jie , NIE Yang-Bo , ZHONG Qi-Ping , ZHOU Zu-Ying , KONG Xiang-Zhong . Measurement of the neutron spectrum of a Pu-C source with a liquid scintillator. Chinese Physics C, 2009, 33(5): 378-382. doi: 10.1088/1674-1137/33/5/012
[16]	WEI Jie , FU Shi-Nian , TANG Jing-Yu , TAO Ju-Zhou , WANG Ding-Sheng , WANG Fang-Wei , WANG Sheng . China Spallation Neutron Source - an overview of application prospects. Chinese Physics C, 2009, 33(11): 1033-1042. doi: 10.1088/1674-1137/33/11/021
[17]	LIU Jun , JIA Wen-Zhi , WANG Shun-Jin . Microscopic calculation of the magnetic field of neutron stars. Chinese Physics C, 2009, 33(9): 737-742. doi: 10.1088/1674-1137/33/9/005
[18]	YANG Fang , SHEN Hong . Influence of the nuclear equation of state on the hadron-quark phase transition in neutron stars. Chinese Physics C, 2008, 32(7): 536-542. doi: 10.1088/1674-1137/32/7/005
[19]	LIU Jing-Jing , LUO Zhi-Quan . Neutrino energy loss by electron capture in magnetic field at the crusts of neutron stars. Chinese Physics C, 2008, 32(2): 108-111. doi: 10.1088/1674-1137/32/2/007
[20]	YANG Fang , SHEN Hong . Hadron-quark phase transition in neutron stars. Chinese Physics C, 2008, 32(S2): 77-80.

Access

Get Citation

PI Chun-Mei, YANG Shu-Hua, ZHOU Xia and ZHOU Ai-Zhi. Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source[J]. Chinese Physics C, 2010, 34(12): 1818-1822. doi: 10.1088/1674-1137/34/12/006

RIS(for EndNote,Reference Manager,ProCite)

BibTex

Txt

Milestone

Received: 2010-03-05
Revised: 2010-04-22

Article Metric

Article Views(2666)
PDF Downloads(421)
Cited by(0)

Policy on re-use

To reuse of subscription content published by CPC, the users need to request permission from CPC, unless the content was published under an Open Access license which automatically permits that type of reuse.

通讯作者: 陈斌, bchen63@163.com

1.
沈阳化工大学材料科学与工程学院沈阳 110142

Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source

Corresponding author: PI Chun-Mei,

Received Date: 2010-03-05

Accepted Date: 2010-04-22

Available Online: 2010-12-05

Abstract:

Employing phenomenological density-dependent critical temperatures of strong singlet-state proton pairing and of moderate triplet-state neutron pairing, we investigate the effects of rotochemical heating on the thermal evolution of superfluid neutron stars whose cores
consist of npe matter with the Akmal-Pandharipande-Ravenhall equation of state. Since the star is not quite in the weak interaction equilibrium state during spin-down, the departure from the chemical equilibrium leads to the rotochemical heating in a rotating NS which will increase the stellar's temperature. Our calculations show that the rotochemical heating delays the cooling of superfluid neutron stars considerably and makes the previous classification of NS cooling ambiguous. What's more, our model is currently consistent with all the observational data, and in particular some middle-aged and cold NSs (PRS J0205+6449 in 3C 58, PRS J1357-6429, RX J007.0+7303 in CTA 1, Vela) can be better explained when taking into account rotochemical heating.

HTML

Reference (1)

Cooling of Akmal-Pandharipande-Ravenhall neutron stars with a rotochemical heating source

Abstract：

References

Access

Article Metrics

Metrics

通讯作者: 陈斌, bchen63@163.com

Email This Article