首页|Spin Evolution of the Magnetar SGR J1935+2154

Spin Evolution of the Magnetar SGR J1935+2154

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Fast radio bursts(FRBs)are short pulses observed in radio frequencies usually originating from cosmological distances.The discovery of FRB 200428 and its X-ray counterpart from the Galactic magnetar SGR J1935+2154 suggests that at least some FRBs can be generated by magnetars.However,the majority of X-ray bursts from magnetars are not associated with radio emission.The fact that only in rare cases can an FRB be generated raises the question regarding the special triggering mechanism of FRBs.Here we report long time spin evolution of SGR J1935+2154 until the end of 2022.According to v and v,the spin evolution of SGR J1935+2154 could be divided into two stages.The first stage evolves relatively steady evolution until 2020 April 27.After the burst activity in 2020,the spin of SGR J1935+2154 shows strong variations,especially for v.After the burst activity in 2022 October,a new spin-down glitch with Δv/v=(-7.2±0.6)×10-6 is detected around MJD 59876,which is the second event in SGR J1935+2154.At the end,spin frequency and pulse profile do not show variations around the time of FRB 200428 and radio bursts 221014 and 221021,which supply strong clues to constrain the trigger mechanism of FRBs or radio bursts.

(stars:)pulsars:general(stars:)pulsars:individual(SGR J1935+2154)X-rays:bursts

Ming-Yu Ge、Yuan-Pei Yang、Fang-Jun Lu、Shi-Qi Zhou、Long Ji、Shuang-Nan Zhang、Bing Zhang、Liang Zhang、Pei Wang、Kejia Lee、Weiwei Zhu、Jian Li、Xian Hou、Qiao-Chu Li

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Key Laboratory of Particle Astrophysics,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China

South-Western Institute For Astronomy Research,Yunnan University,Kunming 650504,China

Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China

Key Laboratory of Stellar and Interstellar Physics and School of Physics and Optoelectronics,Xiangtan University,Xiangtan 411105,China

School of Physics and Astronomy,Sun Yat-Sen University,Zhuhai 519082,China

University of Chinese Academy of Sciences,Chinese Academy of Sciences,Beijing 100049,China

Nevada Center for Astrophysics,University of Nevada,Las Vegas,NV 89154,USA

Department of Physics and Astronomy,University of Nevada,Las Vegas,NV 89154,USA

National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China

Department of Astronomy,Peking University,Beijing 100871,China

CAS Key Laboratory for Research in Galaxies and Cosmology,Department of Astronomy,University of Science and Technology of China,Hefei 230026,China

School of Astronomy and Space Science,University of Science and Technology of China,Hefei 230026,China

Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China

School of Astronomy and Space Science,Nanjing University,Nanjing 210023,China

Key laboratory of Modem Astronomy and Astrophysics,Nanjing University,Nanjing 210023,China

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National Key Research and Development Program of China from the Minister of Science and Technology of China(MOST)国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金国家自然科学基金International Partnership Program of Chinese Academy of SciencesNational SKA Program of ChinaChina Manned Spaced Project

2021YFA07185001217310312003028U2038101U203810211733009113111KYSB201900202022SKA0130100CMS-CSST-2021-B11

2024

天文和天体物理学研究
中国科学院国家天文台

天文和天体物理学研究

CSTPCD
影响因子:0.406
ISSN:1674-4527
年,卷(期):2024.24(1)
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