Does or Did the Supernova Remnant Cassiopeia A Operate as a PeVatron?

被引：3

作者：

Cao, Zhen ^{[1
,2
,3
,4
,5
]}

Aharonian, F. ^{[6
,7
]}

An, Q. ^{[8
,9
]}

Axikegu ^{[10
,11
]}

Bai, Y. X. ^{[1
,2
,3
,5
]}

Bao, Y. W. ^{[12
]}

Bastieri, D. ^{[13
]}

Bi, X. J. ^{[1
,2
,3
,4
,5
]}

Bi, Y. J. ^{[1
,2
,3
,5
]}

Cai, J. T. ^{[13
]}

Cao, Q. ^{[14
]}

Cao, W. Y. ^{[9
]}

Cao, Zhe ^{[8
,9
]}

Chang, J. ^{[15
,16
]}

Chang, J. F. ^{[1
,2
,3
,5
,8
]}

Chen, A. M. ^{[17
,18
]}

Chen, E. S. ^{[1
,2
,3
,4
,5
]}

Chen, Liang ^{[19
]}

Chen, Lin ^{[10
,11
]}

Chen, Long ^{[10
,11
]}

Chen, M. J. ^{[1
,2
,3
,5
]}

Chen, M. L. ^{[1
,2
,3
,5
,8
]}

Chen, Q. H. ^{[10
,11
]}

Chen, S. H. ^{[1
,2
,3
,4
,5
]}

Chen, S. Z. ^{[1
,2
,3
,5
]}

Chen, T. L. ^{[20
]}

Chen, Y. ^{[12
]}

Cheng, N. ^{[1
,2
,3
,5
]}

Cheng, Y. D. ^{[1
,2
,3
,5
]}

Cui, M. Y. ^{[15
,16
]}

Cui, S. W. ^{[14
]}

Cui, X. H. ^{[21
]}

Cui, Y. D. ^{[22
,23
,24
,25
]}

Dai, B. Z. ^{[26
]}

Dai, H. L. ^{[1
,2
,3
,5
,8
]}

Dai, Z. G. ^{[9
]}

Danzengluobu ^{[20
]}

della Volpe, D. ^{[27
]}

Dong, X. Q. ^{[1
,2
,3
,4
,5
]}

Duan, K. K. ^{[15
,16
]}

Fan, J. H. ^{[13
]}

Fan, Y. Z. ^{[15
,16
]}

Fang, J. ^{[26
]}

Fang, K. ^{[1
,2
,3
,5
]}

Feng, C. F. ^{[28
]}

Feng, L. ^{[15
,16
]}

Feng, S. H. ^{[1
,2
,3
,5
]}

Feng, X. T. ^{[28
]}

Feng, Y. L. ^{[20
]}

Gabici, S. ^{[29
]}

机构：

[1] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China

[2] Chinese Acad Sci, Inst High Energy Phys, Expt Phys Div, Beijing 100049, Peoples R China

[3] Chinese Acad Sci, Comp Ctr, Inst High Energy Phys, Beijing 100049, Peoples R China

[4] Univ Chinese Acad Sci, Beijing 100049, Peoples R China

[5] Tianfu Cosm Ray Res Ctr, Chengdu 610000, Sichuan, Peoples R China

[6] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[7] Max Planck Inst Nucl Phys, POB 103980, D-69029 Heidelberg, Germany

[8] State Key Lab Particle Detect & Elect, Hefei, Peoples R China

[9] Univ Sci & Technol China, Hefei 230026, Anhui, Peoples R China

[10] Southwest Jiaotong Univ, Sch Phys Sci & Technol, Chengdu 610031, Sichuan, Peoples R China

[11] Southwest Jiaotong Univ, Sch Informat Sci & Technol, Chengdu 610031, Sichuan, Peoples R China

[12] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210023, Jiangsu, Peoples R China

[13] Guangzhou Univ, Ctr Astrophys, Guangzhou 510006, Guangdong, Peoples R China

[14] Hebei Normal Univ, Shijiazhuang 050024, Hebei, Peoples R China

[15] Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Nanjing 210023, Jiangsu, Peoples R China

[16] Chinese Acad Sci, Purple Mt Observ, Key Lab Radio Astron, Nanjing 210023, Jiangsu, Peoples R China

[17] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shanghai 200240, Peoples R China

[18] Shanghai Jiao Tong Univ, Sch Phys & Astron, Shanghai 200240, Peoples R China

[19] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China

[20] Tibet Univ, Key Lab Cosm Rays, Minist Educ, Lhasa 850000, Tibet, Peoples R China

[21] Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China

[22] Sun Yat Sen Univ, Sch Phys & Astron, Zhuhai 519000, Peoples R China

[23] Sun Yat Sen Univ, Sch Phys, Guangzhou 510275, Guangdong, Peoples R China

[24] Sun Yat Sen Univ, Sino French Inst Nucl Engn & Technol, Zhuhai 519000, Peoples R China

[25] Sun Yat Sen Univ, Sino French Inst Nucl Engn & Technol, Guangzhou 510275, Guangdong, Peoples R China

[26] Yunnan Univ, Sch Phys & Astron, Kunming 650091, Yunnan, Peoples R China

[27] Univ Geneva, Fac Sci, Dept Phys Nucl & Corpusculaire, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[28] Shandong Univ, Inst Frontier & Interdisciplinary Sci, Qingdao 266237, Shandong, Peoples R China

[29] Univ Paris Cite, CEA IRFU, Observ Paris, APC,CNRS IN2P3, F-75205 Paris, France

[30] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China

[31] Zhengzhou Univ, Sch Phys & Microelect, Zhengzhou 450001, Henan, Peoples R China

[32] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China

[33] Sichuan Univ, Coll Phys, Chengdu 610065, Sichuan, Peoples R China

[34] Russian Acad Sci, Inst Nucl Res, Moscow 117312, Russia

[35] Peking Univ, Sch Phys, Beijing 100871, Peoples R China

[36] Guangxi Univ, Sch Phys Sci & Technol, Nanning 530004, Peoples R China

[37] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand

[38] Moscow Inst Phys & Technol, Moscow 141700, Russia

[39] Nanchang Univ, Ctr Relativist Astrophys & High Energy Phys, Sch Phys & Mat Sci, Nanchang 330031, Jiangxi, Peoples R China

[40] Nanchang Univ, Inst Space Sci & Technol, Nanchang 330031, Jiangxi, Peoples R China

[41] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 961卷 / 02期

基金：

中国国家自然科学基金; 国家重点研发计划;

关键词：

COSMIC-RAY ACCELERATION; MAGNETIC-FIELD; SHOCK ACCELERATION; TEV ENERGIES; A SUPERNOVA; SPECTRUM; EMISSION; OBLIQUE; ESCAPE; GAS;

D O I：

10.3847/2041-8213/ad1d62

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

For decades, supernova remnants (SNRs) have been considered the prime sources of Galactic cosmic rays (CRs). But whether SNRs can accelerate CR protons to PeV energies and thus dominate CR flux up to the knee is currently under intensive theoretical and phenomenological debate. The direct test of the ability of SNRs to operate as CR PeVatrons can be provided by ultrahigh-energy (UHE; E-gamma >= 100 TeV) gamma-rays. In this context, the historical SNR Cassiopeia A (Cas A) is considered one of the most promising targets for UHE observations. This paper presents the observation of Cas A and its vicinity by the LHAASO KM2A detector. The exceptional sensitivity of LHAASO KM2A in the UHE band, combined with the young age of Cas A, enabled us to derive stringent model-independent limits on the energy budget of UHE protons and nuclei accelerated by Cas A at any epoch after the explosion. The results challenge the prevailing paradigm that Cas A-type SNRs are major suppliers of PeV CRs in the Milky Way.

引用

页数：7

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