Magnetic Structures and Turbulence in SN 1006 Revealed with Imaging X-Ray Polarimetry

被引：11

作者：

Zhou, Ping ^{[1
]}

Prokhorov, Dmitry ^{[2
,3
]}

Ferrazzoli, Riccardo ^{[4
]}

Yang, Yi-Jung ^{[5
,6
]}

Slane, Patrick ^{[7
]}

Vink, Jacco ^{[2
,3
]}

Silvestri, Stefano ^{[5
]}

Bucciantini, Niccolo ^{[9
,10
,11
]}

Reynoso, Estela ^{[12
]}

Moffett, David ^{[13
]}

Soffitta, Paolo ^{[4
]}

Swartz, Doug ^{[14
]}

Kaaret, Philip ^{[15
]}

Baldini, Luca ^{[8
,16
]}

Costa, Enrico ^{[4
]}

Ng, C. -Y. ^{[5
]}

Kim, Dawoon E. ^{[4
,17
,18
]}

Doroshenko, Victor ^{[19
]}

Ehlert, Steven R. ^{[15
]}

Heyl, Jeremy ^{[20
]}

Marin, Frederic ^{[21
]}

Mizuno, Tsunefumi ^{[22
]}

Pesce-Rollins, Melissa ^{[8
]}

Sgro, Carmelo ^{[8
]}

Tamagawa, Toru ^{[23
]}

Weisskopf, Martin C. ^{[15
]}

Xie, Fei ^{[4
,24
]}

Agudo, Ivan ^{[25
]}

Antonelli, Lucio A. ^{[26
,27
]}

Bachetti, Matteo ^{[28
]}

Baumgartner, Wayne H. ^{[15
]}

Bellazzini, Ronaldo ^{[8
]}

Bianchi, Stefano ^{[29
]}

Bongiorno, Stephen D. ^{[15
]}

Bonino, Raffaella ^{[30
,31
]}

Brez, Alessandro ^{[8
]}

Capitanio, Fiamma ^{[4
]}

Castellano, Simone ^{[8
]}

Cavazzuti, Elisabetta ^{[32
]}

Chen, Chien-Ting ^{[14
]}

Ciprini, Stefano ^{[18
,27
]}

De Rosa, Alessandra ^{[4
]}

Del Monte, Ettore ^{[4
]}

Di Gesu, Laura ^{[32
]}

Di Lalla, Niccolo ^{[33
,34
]}

Di Marco, Alessandro ^{[4
]}

Donnarumma, Immacolata ^{[32
]}

Dovciak, Michal ^{[35
]}

Enoto, Teruaki ^{[23
]}

Evangelista, Yuri ^{[4
]}

机构：

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

[2] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[3] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[4] INAF Ist Astrofis & Planetol Spaziali, Via Fosso Cavaliere 100, I-00133 Rome, Italy

[5] Univ Hong Kong, Dept Phys, Pokfulam, Hong Kong, Peoples R China

[6] Univ Hong Kong, Lab Space Res, Hong Kong, Peoples R China

[7] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[8] Ist Nazl Fis Nucl, Sez Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[9] INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy

[10] Univ Firenze, Dipartimento Fis & Astron, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy

[11] Ist Nazl Fis Nucl, Sez Firenze, Via Sansone 1, I-50019 Sesto Fiorentino, FI, Italy

[12] Inst Astron & Fis Espacio IAFE, Ave Int Guiraldes 2620,Ciudad Univ, RA-1428 Buenos Aires, Argentina

[13] Furman Univ, Dept Phys, Greenville, SC 29613 USA

[14] Univ Space Res Assoc, Sci & Technol Inst, Huntsville, AL 35805 USA

[15] NASA Marshall Space Flight Ctr, Huntsville, AL 35812 USA

[16] Univ Pisa, Dipartimento Fis, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[17] Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 5, I-00185 Rome, Italy

[18] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[19] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany

[20] Univ British Columbia, Vancouver, BC V6T IZ4, Canada

[21] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France

[22] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, HigashiHiroshima, Hiroshima 7398526, Japan

[23] RIKEN Cluster Pioneering Res, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[24] Guangxi Univ, Sch Phys Sci & Technol, Guangxi Key Lab Relativist Astrophys, Nanning 530004, Peoples R China

[25] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain

[26] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone RM, RM, Italy

[27] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

[28] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy

[29] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy

[30] Ist Nazl Fis Nucl, Sez Torino, Via Pietro Giuria 1, I-10125 Turin, Italy

[31] Univ Torino, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy

[32] ASI Agenzia Spaziale Italiana, Via Politecn Snc, I-00133 Rome, Italy

[33] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

[34] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[35] Czech Acad Sci, Astron Inst, Bocni 2 1401-1, Prague 14100 4, Czech Republic

[36] CALTECH, Pasadena, CA 91125 USA

[37] Yamagata Univ, 1-4-12 Kojirakawa Machi, Yamagata 9908560, Japan

[38] Osaka Univ, 1-1 Yamadaoka, Suita, Osaka 5650871, Japan

[39] Chiba Univ, Int Ctr Hadron Astrophys, Chiba 2638522, Japan

[40] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA

[41] St Petersburg State Univ, Dept Astrophys, Univ Sky Pr 28, St Petersburg 198504, Russia

[42] Univ New Hampshire, Dept Phys & Astron, Durham, NH 03824 USA

[43] Univ New Hampshire, Space Sci Ctr, Durham, NH 03824 USA

[44] Washington Univ St Louis, Phys Dept, St Louis, MO 63130 USA

[45] Washington Univ St Louis, McDonnell Ctr Space Sci, St Louis, MO 63130 USA

[46] Univ Turku, Finnish Ctr Astron ESO, Turku 20014, Finland

[47] Ist Nazl Fis Nucl, Sez Napoli, Str Comunale Cinthia, I-80126 Naples, Italy

[48] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[49] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Furo Cho,Chikusa Ku, Nagoya, Aichi 4648602, Japan

[50] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 957卷 / 01期

基金：

美国国家航空航天局;

关键词：

SUPERNOVA-REMNANTS; FIELD AMPLIFICATION; SHOCK ACCELERATION; PARTICLE-ACCELERATION; NONTHERMAL EMISSION; CASSIOPEIA-A; COSMIC-RAYS; RADIO; EXPANSION; SN-1006;

D O I：

10.3847/1538-4357/acf3e6

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Young supernova remnants strongly modify the surrounding magnetic fields, which in turn play an essential role in accelerating cosmic rays (CRs). The X-ray polarization measurements probe magnetic field morphology and turbulence at the immediate acceleration site. We report the X-ray polarization distribution in the northeastern shell of SN 1006 from a 1 Ms observation with the Imaging X-ray Polarimetry Explorer. We found an average polarization degree of 22.4% +/- 3.5% and an average polarization angle of -45.degrees 4 +/- 4.degrees 5 (measured on the plane of the sky from north to east). The X-ray polarization angle distribution reveals that the magnetic fields immediately behind the shock in the northeastern shell of SN 1006 are nearly parallel to the shock normal or radially distributed, similar to that in the radio observations, and consistent with the quasi-parallel CR acceleration scenario. The X-ray emission is marginally more polarized than that in the radio band. The X-ray polarization degree of SN 1006 is much larger than that in Cas A and Tycho, together with the relatively tenuous and smooth ambient medium of the remnant, favoring that CR-induced instabilities set the magnetic turbulence in SN 1006, and CR acceleration is environment-dependent.

引用

页数：12

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