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The origin of polarization in kilonovae and the case of the gravitational-wave counterpart AT 2017gfo
Bulla, M.1; Covino, S.2; Kyutoku, K.3,4,5,6; Tanaka, M.7,8; Maund, J. R.9; Patat, F.10; Toma, K.7,11; Wiersema, K.12,13,14; Bruten, J.9; Jin, Z. P.15; Testa, V16
2019
Source PublicationNATURE ASTRONOMY
ISSN2397-3366
Volume3Issue:1Pages:99-106
Corresponding AuthorBulla, M.(mattia.bulla@fysik.su.se) ; Covino, S.(stefano.covino@inaf.it)
AbstractThe gravitational-wave event GW 170817 was generated by the coalescence of two neutron stars and produced an electromagnetic transient, labelled AT 2017gfo, that was the target of a massive observational campaign. Polarimetry is a powerful diagnostic tool for probing the geometry and emission processes of unresolved sources, and the observed linear polarization for this event was consistent with being mostly induced by intervening dust, suggesting that the intrinsic emission was weakly polarized (P < 0.4-0.5%). Here we present a detailed analysis of the linear polarization expected from a merging neutron-star binary system by means of 3D Monte Carlo radiative transfer simulations assuming a range of possible configurations, wavelengths, epochs and viewing angles. We find that polarization originates from the non-homogeneous opacity distribution within the ejecta and can reach levels of 1% at early times (one to two days after the merger) and in the optical R band. Smaller polarization signals are expected at later epochs and different wavelengths. From the viewing-angle dependence of the polarimetric signal, we constrain the observer orientation of AT 2017gfo to within about 65 degrees from the polar direction. The detection of non-zero polarization in future events will unambiguously reveal the presence of a lanthanide-free ejecta component and unveil its spatial and angular distribution.
DOI10.1038/s41550-018-0593-y
WOS KeywordR-PROCESS NUCLEOSYNTHESIS ; ELECTROMAGNETIC COUNTERPART ; LIGHT CURVES ; MERGER ; SCATTERING ; SIGNATURES ; SPECTRA ; EJECTA ; LINE ; HOLE
Indexed BySCI
Language英语
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000455194000025
PublisherNATURE PUBLISHING GROUP
Citation statistics
Cited Times:4[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/19195
Collection中国科学院紫金山天文台
Corresponding AuthorBulla, M.; Covino, S.
Affiliation1.Stockholm Univ, Oskar Klein Ctr, Dept Phys, Stockholm, Sweden
2.Brera Astron Observ, Ist Nazl Astrofis, Merate, Italy
3.KEK, Inst Particle & Nucl Studies, Theory Ctr, Tsukuba, Ibaraki, Japan
4.Grad Univ Adv Studies Sokendai, Dept Particle & Nucl Phys, Tsukuba, Ibaraki, Japan
5.RIKEN, Interdisciplinary Theoret & Math Sci Program iTHE, Wako, Saitama, Japan
6.Kyoto Univ, Ctr Gravitat Phys, Yukawa Inst Theoret Phys, Kyoto, Japan
7.Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi, Japan
8.Natl Astron Observ Japan, Natl Inst Nat Sci, Mitaka, Tokyo, Japan
9.Univ Sheffield, Dept Phys & Astron, Sheffield, S Yorkshire, England
10.European Southern Observ, Garching, Germany
11.Tohoku Univ, Frontier Res Inst Interdisciplinary Sci, Tohoku, Japan
12.Univ Leicester, Dept Phys, Leicester, Leics, England
13.Univ Leicester, Leicester Inst Space & Earth Observat, Leicester, Leics, England
14.Univ Warwick, Coventry, W Midlands, England
15.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing, Jiangsu, Peoples R China
16.Osserv Astron Roma, Ist Nazl Astrofis, Monte Porzio Catone, Italy
Recommended Citation
GB/T 7714
Bulla, M.,Covino, S.,Kyutoku, K.,et al. The origin of polarization in kilonovae and the case of the gravitational-wave counterpart AT 2017gfo[J]. NATURE ASTRONOMY,2019,3(1):99-106.
APA Bulla, M..,Covino, S..,Kyutoku, K..,Tanaka, M..,Maund, J. R..,...&Testa, V.(2019).The origin of polarization in kilonovae and the case of the gravitational-wave counterpart AT 2017gfo.NATURE ASTRONOMY,3(1),99-106.
MLA Bulla, M.,et al."The origin of polarization in kilonovae and the case of the gravitational-wave counterpart AT 2017gfo".NATURE ASTRONOMY 3.1(2019):99-106.
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