X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho's Supernova Remnant

被引：20

作者：

Ferrazzoli, Riccardo ^{[1
]}

Slane, Patrick ^{[2
]}

Prokhorov, Dmitry ^{[3
,4
]}

Zhou, Ping ^{[5
]}

Vink, Jacco ^{[3
,4
]}

Bucciantini, Niccolo ^{[6
,7
,8
]}

Costa, Enrico ^{[1
]}

Di Lalla, Niccolo ^{[9
,10
]}

Di Marco, Alessandro ^{[1
]}

Soffitta, Paolo ^{[1
]}

Weisskopf, Martin C. ^{[11
]}

Asakura, Kazunori ^{[12
]}

Baldini, Luca ^{[13
,14
]}

Heyl, Jeremy ^{[15
]}

Kaaret, Philip E. ^{[11
]}

Marin, Frederic ^{[16
]}

Mizuno, Tsunefumi ^{[17
]}

Ng, C. -Y. ^{[18
]}

Pesce-Rollins, Melissa ^{[13
]}

Silvestri, Stefano ^{[13
]}

Sgro, Carmelo ^{[13
]}

Swartz, Douglas A. ^{[19
]}

Tamagawa, Toru ^{[20
]}

Yang, Yi-Jung ^{[18
]}

Agudo, Ivan ^{[21
]}

Antonelli, Lucio A. ^{[22
,23
]}

Bachetti, Matteo ^{[24
]}

Baumgartner, Wayne H. ^{[11
]}

Bellazzini, Ronaldo ^{[13
]}

Bianchi, Stefano ^{[25
]}

Bongiorno, Stephen D. ^{[11
]}

Bonino, Raffaella ^{[26
,27
]}

Brez, Alessandro ^{[13
]}

Capitanio, Fiamma ^{[1
]}

Castellano, Simone ^{[13
]}

Cavazzuti, Elisabetta ^{[28
]}

Chen, Chien-Ting ^{[19
]}

Ciprini, Stefano ^{[23
,29
]}

De Rosa, Alessandra ^{[1
]}

Del Monte, Ettore ^{[1
]}

Di Gesu, Laura ^{[28
]}

Donnarumma, Immacolata ^{[28
]}

Doroshenko, Victor ^{[30
]}

Dovciak, Michal ^{[31
]}

Ehlert, Steven R. ^{[11
]}

Enoto, Teruaki ^{[20
]}

Evangelista, Yuri ^{[1
]}

Fabiani, Sergio ^{[1
]}

Garcia, Javier A. ^{[32
]}

Gunji, Shuichi ^{[33
]}

机构：

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

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

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

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

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

[6] INAF Osservatorio Astrofis Arcetri, Largo Enr Fermi 5, I-50125 Florence, Italy

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

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

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

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

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

[12] Osaka Univ, Grad Sch Sci, Osaka, Japan

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

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

[15] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada

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

[17] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan

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

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

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

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

[22] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Monte Porzio Catone, Italy

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

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

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

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

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

[28] ASI Agenzia Spaziale Italiana, Via Politecn snc, I-00133 Rome, Italy

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

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

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

[32] CALTECH, Pasadena, CA 91125 USA

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

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

[35] Chuo Univ, Fac Sci & Engn, Dept Phys, 1-13-27 Kasuga,Bunkyo Ku, Tokyo 1128551, Japan

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

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

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

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

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

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

[42] Univ Turku, Finnish Ctr Astron ESO, FI-20014 Turku, Finland

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

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

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

[46] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[47] NASA, Ctr Res & Explorat Space Sci & Technol, GSFC, Greenbelt, MD 20771 USA

[48] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[49] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[50] Univ Turku, Dept Phys & Astron, FI-20014 Turku, Finland

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 945卷 / 01期

基金：

美国国家航空航天局;

关键词：

DIFFUSIVE SHOCK ACCELERATION; RADIO STRUCTURE; AMPLIFICATION; POLARIZATION; EMISSION; INSTABILITY; EXPANSION; SPECTRUM; STRIPES; ORIGIN;

D O I：

10.3847/1538-4357/acb496

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho's supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% +/- 2% averaged over the whole remnant, and 12% +/- 2% at the rim, higher than the value of polarization of 7%-8% observed in the radio band. In the west region, the degree of polarization is 23% +/- 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 +/- 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

引用

页数：14

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