Results of 23 yr of Pulsar Timing of PSR J1453-6413

doi:10.1088/1674-4527/acf1e1

XAO OpenIR > 射电天文研究室 > 脉冲星研究团组

	Results of 23 yr of Pulsar Timing of PSR J1453-6413
	Li, Wei 1,2; Dang, Shi-Jun1,2,3 ; Yuan, Jian-Ping4 ; Li, Lin5 ; Wang, Wei-Hua 6; Shang, Lun-Hua 1,2; Wang, Na4 ; Li, Qing-Ying 1,2; Lu, Ji-Guang 7; Kou, Fei-Fei4 ; Wang, Shuang-Qiang4 ; Xiao, Shuo 1,2; Zhi, Qi-Jun 1,2; Liu, Yu-Lan 3,7,8; Zhao, Ru-Shuang 1,2; Dong, Ai-Jun 1,2; Zhang, Bin 1,2; You, Zi-Yi 1,2; Cai, Yan-Qing 1,2; Yang, Ya-Qin 1; Ren, Ying-Ying 1,2; Liu, Yu-Jia 1,2; Xu, Heng 1,2
	2023-10-01
Source Publication	RESEARCH IN ASTRONOMY AND ASTROPHYSICS
ISSN	1674-4527
Volume	23 Issue:10 Pages:105014
Contribution Rank	4
Abstract	In this paper, we presented the 23.3 yr of pulsar timing results of PSR J1456-6413 based on the observations of Parkes 64 m radio telescope. We detected two new glitches at MJD 57093(3) and 59060(12) and confirmed its first glitch at MJD 54554(10). The relative sizes (??/?) of these two new glitches are 0.9 x 10(-9) and 1.16 x 10(-9), respectively. Using the "Cholesky" timing analysis method, we have determined its position, proper motion, and two-dimensional transverse velocities from the data segments before and after the second glitch, respectively. Furthermore, we detected exponential recovery behavior after the first glitch, with a recovery timescale of approximately 200 days and a corresponding exponential recovery factor Q of approximately 0.15(2), while no exponential recovery was detected for the other two glitches. More interestingly, we found that the leading component of the integral pulse profile after the second glitch became stronger, while the main component became weaker. Our results will expand the sample of pulsars with magnetosphere fluctuation triggered by the glitch event.
Keyword	Stars (stars:) pulsars: individual (PSR J1453-6413) stars: neutron
DOI	10.1088/1674-4527/acf1e1
Indexed By	SCI
Language	英语
WOS Keyword	PROPER-MOTION ; CRAB PULSAR ; MAGNETOSPHERIC FLUCTUATIONS ; GLITCH ACTIVITY ; SPIN-DOWN ; IRREGULARITIES ; ASTROMETRY ; EMISSION ; ROTATION ; PACKAGE
Funding Project	This work was supported by the National SKA Program of China (Nos. 2022SKA0130100, 2020SKA0120100 and 2022SKA0130104), Guizhou Province Science and Technology Foundation (No. ZK[2022]304), the Major Science and Technology Program of Xinjiang Uygur Autonomo[2022SKA0130100] ; This work was supported by the National SKA Program of China (Nos. 2022SKA0130100, 2020SKA0120100 and 2022SKA0130104), Guizhou Province Science and Technology Foundation (No. ZK[2022]304), the Major Science and Technology Program of Xinjiang Uygur Autonomo[2020SKA0120100] ; This work was supported by the National SKA Program of China (Nos. 2022SKA0130100, 2020SKA0120100 and 2022SKA0130104), Guizhou Province Science and Technology Foundation (No. ZK[2022]304), the Major Science and Technology Program of Xinjiang Uygur Autonomo[2022SKA0130104] ; National SKA Program of China[ZK[2022]304] ; Guizhou Province Science and Technology Foundation[2022A03013-2] ; Guizhou Province Science and Technology Foundation[2022A03013-4] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region[[2022]132] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region[[2022]123] ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region[[2022]137] ; Scientific Research Project of the Guizhou Provincial Education[11873080] ; Scientific Research Project of the Guizhou Provincial Education[U1731238] ; Scientific Research Project of the Guizhou Provincial Education[11565010] ; Scientific Research Project of the Guizhou Provincial Education[12103013] ; Scientific Research Project of the Guizhou Provincial Education[U1838109] ; Scientific Research Project of the Guizhou Provincial Education[U1831120] ; Scientific Research Project of the Guizhou Provincial Education[12273008] ; National Natural Science Foundation of China[U1931101] ; Chinese Academy of Sciences[(2021)303] ; Foundation of Guizhou Provincial Education Department[2023] ; Guizhou Province Science and Technology Support Program[2020D04049] ; Key Laboratory of Xinjiang Uygur Autonomous Region[[2022]B18] ; Academic New Seeding Fund Project of Guizhou Normal University ; CAS - Commonwealth of Australia
WOS Research Area	Astronomy & Astrophysics
WOS Subject	Astronomy & Astrophysics
WOS ID	WOS:001073818800001
Publisher	NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES
Funding Organization	This work was supported by the National SKA Program of China (Nos. 2022SKA0130100, 2020SKA0120100 and 2022SKA0130104), Guizhou Province Science and Technology Foundation (No. ZK[2022]304), the Major Science and Technology Program of Xinjiang Uygur Autonomo ; National SKA Program of China ; Guizhou Province Science and Technology Foundation ; Major Science and Technology Program of Xinjiang Uygur Autonomous Region ; Scientific Research Project of the Guizhou Provincial Education ; National Natural Science Foundation of China ; Chinese Academy of Sciences ; Foundation of Guizhou Provincial Education Department ; Guizhou Province Science and Technology Support Program ; Key Laboratory of Xinjiang Uygur Autonomous Region ; Academic New Seeding Fund Project of Guizhou Normal University ; CAS - Commonwealth of Australia
Citation statistics	Cited Times:1[WOS] [WOS Record] [Related Records in WOS]
Document Type	期刊论文
Identifier	http://ir.xao.ac.cn/handle/45760611-7/5458
Collection	射电天文研究室_脉冲星研究团组
Corresponding Author	Dang, Shi-Jun; Shang, Lun-Hua; Zhi, Qi-Jun
Affiliation	1.Guizhou Normal Univ, Sch Phys & Elect Sci, Guiyang 550001, Peoples R China 2.Guizhou Normal Univ, Guizhou Prov Key Lab Radio Astron & Data Proc, Guiyang 550001, Peoples R China 3.Guizhou Univ, Guizhou Radio Astron Observ, Guiyang 550025, Peoples R China 4.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China 5.Xinjiang Univ, Sch Phys Sci & Technol, Urumqi 830046, Peoples R China 6.Wenzhou Univ, Coll Math & Phys, Wenzhou 325035, Peoples R China 7.Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China 8.Chinese Acad Sci, CAS Key Lab FAST, Natl Astron Observ, Beijing 100101, Peoples R China
Recommended Citation GB/T 7714	Li, Wei,Dang, Shi-Jun,Yuan, Jian-Ping,et al. Results of 23 yr of Pulsar Timing of PSR J1453-6413[J]. RESEARCH IN ASTRONOMY AND ASTROPHYSICS,2023,23(10):105014.
APA	Li, Wei.,Dang, Shi-Jun.,Yuan, Jian-Ping.,Li, Lin.,Wang, Wei-Hua.,...&Xu, Heng.(2023).Results of 23 yr of Pulsar Timing of PSR J1453-6413.RESEARCH IN ASTRONOMY AND ASTROPHYSICS,23(10),105014.
MLA	Li, Wei,et al."Results of 23 yr of Pulsar Timing of PSR J1453-6413".RESEARCH IN ASTRONOMY AND ASTROPHYSICS 23.10(2023):105014.

Files in This Item:
File Name/Size	DocType	Version	Access	License
Li-2023-Results of 2（797KB）	期刊论文	出版稿	开放获取	CC BY-NC-SA	View Application Full Text

File name:	Li-2023-Results of 23 yr of Pulsar Timing of P.pdf
Format:	Adobe PDF

If you have any objections to this item, please fill out the form below and the administrator will contact you as soon as possible.
Content:
Email：	*
Institution:
Verification Code:	Refresh

Any comments and suggestions are welcomed.
Title:	*
Content:
Email：	*
Verification Code:	Refresh

射电天文研究室知识库