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Article: X-ray pulsar GRO J1008−57 as an orthogonal rotator

TitleX-ray pulsar GRO J1008−57 as an orthogonal rotator
Authors
Tsygankov, SSDoroshenko, VMushtukov, AAPoutanen, JDi Marco, AHeyl, JLa Monaca, FForsblom, SVMalacaria, CMarshall, HLSuleimanov, VFSvoboda, JTaverna, RUrsini, FAgudo, IAntonelli, LABachetti, MBaldini, LBaumgartner, WHBellazzini, RBianchi, SBongiorno, SDBonino, RBrez, ABucciantini, NCapitanio, FCastellano, SCavazzuti, EChen, CTCiprini, SCosta, EDe Rosa, ADel Monte, EDi Gesu, LDi Lalla, NDonnarumma, IDovciak, MEhlert, SREnoto, TEvangelista, YFabiani, SFerrazzoli, RGarcia, JAGunji, SHayashida, KIwakiri, WJorstad, SGKaaret, PKaras, VKislat, FKitaguchi, TKolodziejczak, JJKrawczynski, HLatronico, LLiodakis, IMaldera, SManfreda, AMarin, FMarinucci, AMarscher, APMassaro, FMatt, GMitsuishi, IMizuno, TMuleri, FNegro, MNg, CYO'Dell, SLOmodei, NOppedisano, CPapitto, APavlov, GGPeirson, ALPerri, MPesce-Rollins, MPetrucci, POPilia, MPossenti, APuccetti, SRamsey, BDRankin, JRatheesh, ARoberts, OJRomani, RWSgro, CSlane, PSoffitta, PSpandre, GSwartz, DATamagawa, TTavecchio, FTawara, YTennant, AFThomas, NETombesi, FTrois, ATurolla, RVink, JWeisskopf, MCWu, KWXie, FZane, S
KeywordsAccretion
Accretion disks
Magnetic fields
Pulsars: individual: GRO J1008-57
Stars: neutron
X-rays: binaries
Issue Date30-Jun-2023
PublisherEDP Sciences
Citation
Astronomy & Astrophysics, 2023, v. 675, p. 1-11 How to Cite?
DOI: http://dx.doi.org/10.1051/0004-6361/202346134
Abstract

X-ray polarimetry is a unique way to probe the geometrical configuration of highly magnetized accreting neutron stars (X-ray pulsars). GRO J1008􀀀57 is the first transient X-ray pulsar observed at two dierent flux levels by the Imaging X-ray Polarimetry Explorer (IXPE) during its outburst in November 2022. We find the polarization properties of GRO J1008􀀀57 to be independent of its luminosity, with the polarization degree varying between nondetection and about 15% over the pulse phase. Fitting the phase-resolved spectro-polarimetric data with the rotating vector model allowed us to estimate the pulsar inclination (130, which is in good agreement with the orbital inclination), the position angle (75) of the pulsar spin axis, and the magnetic obliquity (74). This makes GRO J1008􀀀57 the first confidently identified nearly orthogonal rotator among X-ray pulsars. We discuss our results in the context of the neutron star atmosphere models and theories of the axis alignment of accreting pulsars.


Persistent Identifierhttp://hdl.handle.net/10722/331976
ISSN
0004-6361
2021 Impact Factor: 6.240
2020 SCImago Journal Rankings: 2.137

 

DC FieldValueLanguage
dc.contributor.authorTsygankov, SS-
dc.contributor.authorDoroshenko, V-
dc.contributor.authorMushtukov, AA-
dc.contributor.authorPoutanen, J-
dc.contributor.authorDi Marco, A-
dc.contributor.authorHeyl, J-
dc.contributor.authorLa Monaca, F-
dc.contributor.authorForsblom, SV-
dc.contributor.authorMalacaria, C-
dc.contributor.authorMarshall, HL-
dc.contributor.authorSuleimanov, VF-
dc.contributor.authorSvoboda, J-
dc.contributor.authorTaverna, R-
dc.contributor.authorUrsini, F-
dc.contributor.authorAgudo, I-
dc.contributor.authorAntonelli, LA-
dc.contributor.authorBachetti, M-
dc.contributor.authorBaldini, L-
dc.contributor.authorBaumgartner, WH-
dc.contributor.authorBellazzini, R-
dc.contributor.authorBianchi, S-
dc.contributor.authorBongiorno, SD-
dc.contributor.authorBonino, R-
dc.contributor.authorBrez, A-
dc.contributor.authorBucciantini, N-
dc.contributor.authorCapitanio, F-
dc.contributor.authorCastellano, S-
dc.contributor.authorCavazzuti, E-
dc.contributor.authorChen, CT-
dc.contributor.authorCiprini, S-
dc.contributor.authorCosta, E-
dc.contributor.authorDe Rosa, A-
dc.contributor.authorDel Monte, E-
dc.contributor.authorDi Gesu, L-
dc.contributor.authorDi Lalla, N-
dc.contributor.authorDonnarumma, I-
dc.contributor.authorDovciak, M-
dc.contributor.authorEhlert, SR-
dc.contributor.authorEnoto, T-
dc.contributor.authorEvangelista, Y-
dc.contributor.authorFabiani, S-
dc.contributor.authorFerrazzoli, R-
dc.contributor.authorGarcia, JA-
dc.contributor.authorGunji, S-
dc.contributor.authorHayashida, K-
dc.contributor.authorIwakiri, W-
dc.contributor.authorJorstad, SG-
dc.contributor.authorKaaret, P-
dc.contributor.authorKaras, V-
dc.contributor.authorKislat, F-
dc.contributor.authorKitaguchi, T-
dc.contributor.authorKolodziejczak, JJ-
dc.contributor.authorKrawczynski, H-
dc.contributor.authorLatronico, L-
dc.contributor.authorLiodakis, I-
dc.contributor.authorMaldera, S-
dc.contributor.authorManfreda, A-
dc.contributor.authorMarin, F-
dc.contributor.authorMarinucci, A-
dc.contributor.authorMarscher, AP-
dc.contributor.authorMassaro, F-
dc.contributor.authorMatt, G-
dc.contributor.authorMitsuishi, I-
dc.contributor.authorMizuno, T-
dc.contributor.authorMuleri, F-
dc.contributor.authorNegro, M-
dc.contributor.authorNg, CY-
dc.contributor.authorO'Dell, SL-
dc.contributor.authorOmodei, N-
dc.contributor.authorOppedisano, C-
dc.contributor.authorPapitto, A-
dc.contributor.authorPavlov, GG-
dc.contributor.authorPeirson, AL-
dc.contributor.authorPerri, M-
dc.contributor.authorPesce-Rollins, M-
dc.contributor.authorPetrucci, PO-
dc.contributor.authorPilia, M-
dc.contributor.authorPossenti, A-
dc.contributor.authorPuccetti, S-
dc.contributor.authorRamsey, BD-
dc.contributor.authorRankin, J-
dc.contributor.authorRatheesh, A-
dc.contributor.authorRoberts, OJ-
dc.contributor.authorRomani, RW-
dc.contributor.authorSgro, C-
dc.contributor.authorSlane, P-
dc.contributor.authorSoffitta, P-
dc.contributor.authorSpandre, G-
dc.contributor.authorSwartz, DA-
dc.contributor.authorTamagawa, T-
dc.contributor.authorTavecchio, F-
dc.contributor.authorTawara, Y-
dc.contributor.authorTennant, AF-
dc.contributor.authorThomas, NE-
dc.contributor.authorTombesi, F-
dc.contributor.authorTrois, A-
dc.contributor.authorTurolla, R-
dc.contributor.authorVink, J-
dc.contributor.authorWeisskopf, MC-
dc.contributor.authorWu, KW-
dc.contributor.authorXie, F-
dc.contributor.authorZane, S-
dc.date.accessioned2023-09-28T04:59:59Z-
dc.date.available2023-09-28T04:59:59Z-
dc.date.issued2023-06-30-
dc.identifier.citationAstronomy & Astrophysics, 2023, v. 675, p. 1-11-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/331976-
dc.description.abstract<p>X-ray polarimetry is a unique way to probe the geometrical configuration of highly magnetized accreting neutron stars (X-ray pulsars). GRO J1008􀀀57 is the first transient X-ray pulsar observed at two dierent flux levels by the Imaging X-ray Polarimetry Explorer (IXPE) during its outburst in November 2022. We find the polarization properties of GRO J1008􀀀57 to be independent of its luminosity, with the polarization degree varying between nondetection and about 15% over the pulse phase. Fitting the phase-resolved spectro-polarimetric data with the rotating vector model allowed us to estimate the pulsar inclination (130, which is in good agreement with the orbital inclination), the position angle (75) of the pulsar spin axis, and the magnetic obliquity (74). This makes GRO J1008􀀀57 the first confidently identified nearly orthogonal rotator among X-ray pulsars. We discuss our results in the context of the neutron star atmosphere models and theories of the axis alignment of accreting pulsars.<br></p>-
dc.languageeng-
dc.publisherEDP Sciences-
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.subjectAccretion-
dc.subjectAccretion disks-
dc.subjectMagnetic fields-
dc.subjectPulsars: individual: GRO J1008-57-
dc.subjectStars: neutron-
dc.subjectX-rays: binaries-
dc.titleX-ray pulsar GRO J1008−57 as an orthogonal rotator-
dc.typeArticle-
dc.identifier.doi10.1051/0004-6361/202346134-
dc.identifier.scopuseid_2-s2.0-85164535605-
dc.identifier.volume675-
dc.identifier.spage1-
dc.identifier.epage11-
dc.identifier.eissn1432-0746-
dc.identifier.issnl0004-6361-

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