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
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.
Fund: 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).
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 2021 Chin. Phys. B 30 068703
[1] Lorimer D R, Stairs I H, Freire P C, Cordes J M, Camilo F, Faulkner A J, Lyne A G, Nice D J, Ransom S M, Arzoumanian Z, Manchester R N, Champion D J, van Leeuwen J, Mclaughlin M A, Ramachandran R, Hessels J W, Vlemmings W, Deshpande A A, Bhat N D, Chatterjee S, Han J L, Gaensler B M, Kasian L, Deneva J S, Reid B, Lazio T J, Kaspi V M, Crawford F, Lommen A N, Backer D C, Kramer M, Stappers B W, Hobbs G B, Possenti A, D'Amico N and Burgay M 2006 ApJ640 428 [2] van Leeuwen J, Kasian L, Stairs I H, Lorimer D R, Camilo F, Chatterjee S, Cognard I, Desvignes G, Freire P C C, Janssen G H, Kramer M, Lyne A G, Nice D J, Ransom S M, Stappers B W and Weisberg J M 2015 ApJ798 118 [3] Yang Y Y, Zhang C M, Li D, Wang D H, Pan Y Y, Lingfu R F and Zhou Z W 2017 ApJ835 185 [4] Huang Y F and Yu Y B 2017 ApJ848 115 [5] Kuerban A, Geng J J, Huang Y F, Zong H S and Gong H 2020 ApJ890 41 [6] Kargaltsev O and Pavlov G G 2009 ApJ702 433 [7] Kramer M and Stairs I H Freire 2008 Ann. Rev. Astron. Astrophys.46 541 [8] Abbott B P, Abbott R, Abbott T D, et al. 2017 Phys. Rev. Lett.119 161101 [9] Pol N, McLaughlin M and Lorimer D R 2019 ApJ870 71 [10] Suzuki T, Toki H and Nomoto K. 2016 ApJ817 163 [11] van den Heuvel E P J 2017 JApA38 45 [12] Nomoto K 1984 ApJ277 791 [13] Dewi J D M, Podsiadlowski P and Sena A 2006 MNRAS368 1742 [14] De K, Kasliwal M M, Ofek E O, Moriya T J, Burke J, Cao Y, Cenko S B, Doran G B, Duggan G E, Fender R P, Fransson C, Gal-Yam A, Horesh A, Kulkarni S R, Laher R R, Lunnan R, Manulis I, Masci F, Mazzali P A, Nugent P E, Perley D A, Petrushevska T, Piro A L, Rumsey C, Sollerman J, Sullivan M and Taddia F 2018 Science362 201 [15] Manchester R N, Hobbs G B, Teoh A and Hobbs M 2005 AJ129 1993 [16] Ferrand G and Safi-Harb S 2012 Advances in Space Research49 1313 [17] Bhattacharya D and van den Heuvel E. P J 1991 Phys. Rep.203 1 [18] Tauris T M, Langer N, Moriya T J, Podsiadlowski P, Yoon S C and Blinnikov S I 2013 ApJL778 L23 [19] Tauris T M, Langer N and Podsiadlowski P 2015 MNRAS451 2123 [20] Tauris T M, Kramer M, Freire P C C, Wex N, Janka H T, Langer N, Podsiadlowski P, Bozzo E, Chaty S, Kruckow M U, van den Heuvel E P J, Antoniadis J, Breton R P and Champion D J 2017 ApJ846 170 [21] Dewi J D M, Podsiadlowski P and Pols O R 2005 MNRAS363 L71 [22] Zhang C. M and Kojima Y. 2006 MNRAS366 137 [23] Ng C, Kruckow M U, Tauris T M, Lyne A G, Freire P C C, Ridolfi A, Caiazzo I, Heyl J, Kramer M, Cameron A D, Champion D J and Stappers B 2018 MNRAS476 4315 [24] Burgay M, D'Amico N, Krame M, et al. 2003 Science426 531 [25] Lyne A G, Burgay M, Kramer M, Possenti A, Manchester RN, Camilo F, McLaughlin M A, Lorimer D R, D'Amico N, Joshi B C, Reynolds J and Freire P C C 2004 Science303 1153 [26] Gessner A and Janka H T 2018 ApJ865 61 [27] Hobbs G, Lorimer D R, Lyne A G and Kramer M 2005 MNRAS360 974 [28] Podsiadlowski Ph, Dewi J D M, Lesaffre P, Miller J C, Newton W G and Stone J R 2005 MNRAS361 1243 [29] Beniamini P and Piran T 2016 Mon. Not. R. Astron. Soc.456 4089 [30] Shao Y and Li X D 2018 ApJ867 124 [31] Janka H T 2017 ApJ837 84 [32] Andrews J J, Zezas A and Fragos T 2018 ApJS237 1 [33] Wong T W, Willems B and Kalogera V 2010 ApJ721 1689 [34] Lattimer J M and Yahil A 1989 ApJ340 426 [35] Kargaltsev O, Pavlov G G, Klingler N and Rangelov B 2017 J. Plasma Phys.83 635830501 [36] Klingler N, Kargaltsev O, Rangelov B, Pavlov G G, Posselt B and Ng C Y 2016 ApJ828 70 [37] Chevalier R A 1977 ApJ213 52 [38] Woosley S and Janka T 2005 Nat. Phys.1 147
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.
