Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

doi:10.1088/1674-1056/abda2c

中国物理B ›› 2021, Vol. 30 ›› Issue (6): 68703-068703.doi: 10.1088/1674-1056/abda2c

• • 上一篇

Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

Yi-Yan Yang(杨佚沿)^1,†, Cheng-Min Zhang(张承民)^2,‡, Jian-Wei Zhang(张见微)³, and De-Hua Wang (王德华)⁴

1 School of Physics and Electronic Sciences, Guizhou Education University, Guiyang 550018, China;
2 CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences(CAS), Beijing 100012, China;
3 Astronomy Department, Beijing Normal University, Beijing 100875, China;
4 School of Physics and Electronic Sciences, Guizhou Normal University, Guiyang 550001, China

收稿日期:2020-06-18 修回日期:2020-12-14 接受日期:2021-01-11 出版日期:2021-05-18 发布日期:2021-05-27
通讯作者: Yi-Yan Yang, Cheng-Min Zhang E-mail:yangyiyan@gznc.edu.cn;zhangcm@bao.ac.cn
基金资助:
Project supported by the National Natural Science Foundation of China (Grant Nos. U1938117, U1731238, 11703003, and 11647114), the International Partnership Program of Chinese Academy of Sciences (Grant No. 114A11KYSB20160008), the National Key Research and Development Program of China (Grant No. 2016YFA0400702), the Guizhou Provincial Science and Technology Foundation (Grant No.[2020]1Y019), and the Project of Guizhou Provincial Education Department (Grant No.[2018]058), the Doctoral Project of Guizhou Education University (Grant No. 2020BS021), and the Key Support Disciplines of Theoretical Physics of Department of Education of Guizhou Province, China (Grant No. ZDXK[2015]38).

Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

Yi-Yan Yang(杨佚沿)^1,†, Cheng-Min Zhang(张承民)^2,‡, Jian-Wei Zhang(张见微)³, and De-Hua Wang (王德华)⁴

1 School of Physics and Electronic Sciences, Guizhou Education University, Guiyang 550018, China;
2 CAS Key Laboratory of FAST, National Astronomical Observatories, Chinese Academy of Sciences(CAS), Beijing 100012, China;
3 Astronomy Department, Beijing Normal University, Beijing 100875, China;
4 School of Physics and Electronic Sciences, Guizhou Normal University, Guiyang 550001, China

Received:2020-06-18 Revised:2020-12-14 Accepted:2021-01-11 Online:2021-05-18 Published:2021-05-27
Contact: Yi-Yan Yang, Cheng-Min Zhang E-mail:yangyiyan@gznc.edu.cn;zhangcm@bao.ac.cn
Supported by:
Project supported by the National Natural Science Foundation of China (Grant Nos. U1938117, U1731238, 11703003, and 11647114), the International Partnership Program of Chinese Academy of Sciences (Grant No. 114A11KYSB20160008), the National Key Research and Development Program of China (Grant No. 2016YFA0400702), the Guizhou Provincial Science and Technology Foundation (Grant No.[2020]1Y019), and the Project of Guizhou Provincial Education Department (Grant No.[2018]058), the Doctoral Project of Guizhou Education University (Grant No. 2020BS021), and the Key Support Disciplines of Theoretical Physics of Department of Education of Guizhou Province, China (Grant No. ZDXK[2015]38).

摘要/Abstract

摘要： So far among the nineteen pairs of detected double neutron star (DNS) systems, it is a usual fact that the first-born recycled pulsar is detected, however the youngest DNS system PSR J1906+0746, with the characteristic age of 113 kyr, is one of the three detected DNS as a non-recycled and second-born NS, which is believed to be formed by an electron capture or a low energy ultra-stripped iron core-collapse supernova (SN) explosion. The SN remnant around PSR J1906+0746 is too dim to be observed by optical telescopes, then its x-ray flux limit has been given by Chandra. A reference pulsar PSR J1509-5850 with the young characteristic age of 154 kyr was chosen as an object of comparison, which has an SN remnant observed by Chandra and is believed to be formed by iron core SN explosion. We impose a restriction on the maximum kinetic energy of electron-capture (EC) SN explosion that induces the formation of PSR J1906+0746. The estimated result is (4-8)×10⁵⁰ erg (1 erg=10^-7 J), which is consistent with that of the published simulations of the EC process, i.e., a lower value than that of the conventional iron core SN explosion of (1-2)×10⁵¹ erg. As suggested, EC process for NS formation is pertained to the subluminous type Ic SN by the helium star with ONeMg core, thus for the first time we derived the kinetic energy of EC SN explosion of DNS, which may be reconciled with the recent observation of type Ic SN 2014ft with kinetic energy of 2×10⁵⁰ erg.

关键词: neutron star, pulsar, astrophysics, high energy astrophysical phenomena

Abstract: So far among the nineteen pairs of detected double neutron star (DNS) systems, it is a usual fact that the first-born recycled pulsar is detected, however the youngest DNS system PSR J1906+0746, with the characteristic age of 113 kyr, is one of the three detected DNS as a non-recycled and second-born NS, which is believed to be formed by an electron capture or a low energy ultra-stripped iron core-collapse supernova (SN) explosion. The SN remnant around PSR J1906+0746 is too dim to be observed by optical telescopes, then its x-ray flux limit has been given by Chandra. A reference pulsar PSR J1509-5850 with the young characteristic age of 154 kyr was chosen as an object of comparison, which has an SN remnant observed by Chandra and is believed to be formed by iron core SN explosion. We impose a restriction on the maximum kinetic energy of electron-capture (EC) SN explosion that induces the formation of PSR J1906+0746. The estimated result is (4-8)×10⁵⁰ erg (1 erg=10^-7 J), which is consistent with that of the published simulations of the EC process, i.e., a lower value than that of the conventional iron core SN explosion of (1-2)×10⁵¹ erg. As suggested, EC process for NS formation is pertained to the subluminous type Ic SN by the helium star with ONeMg core, thus for the first time we derived the kinetic energy of EC SN explosion of DNS, which may be reconciled with the recent observation of type Ic SN 2014ft with kinetic energy of 2×10⁵⁰ erg.

Key words: neutron star, pulsar, astrophysics, high energy astrophysical phenomena

中图分类号: (Energetics)

87.19.ly

87.19.ls (Encoding, decoding, and transformation) 87.19.lc (Noise in the nervous system) 87.16.Vy (Ion channels)

Yi-Yan Yang(杨佚沿), Cheng-Min Zhang(张承民), Jian-Wei Zhang(张见微), and De-Hua Wang (王德华). Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate[J]. 中国物理B, 2021, 30(6): 68703-068703.

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Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

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