X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?

被引：23

作者：

Mushtukov, A. A. ^{[1
,2
]}

Tsygankov, S. S. ^{[3
]}

Poutanen, J. ^{[3
]}

Doroshenko, V. ^{[4
]}

Salganik, A. ^{[5
,6
]}

Costa, E. ^{[7
]}

Di Marco, A. ^{[7
]}

Heyl, J. ^{[8
]}

La Monaca, F. ^{[7
]}

Lutovinov, A. A. ^{[6
]}

Mereminsky, I. A. ^{[6
]}

Papitto, A. ^{[9
]}

Semena, A. N. ^{[6
]}

Shtykovsky, A. E. ^{[6
]}

Suleimanov, V. F. ^{[4
]}

Forsblom, S. V. ^{[3
]}

Gonzalez-Caniulef, D. ^{[10
]}

Malacaria, C. ^{[11
]}

Sunyaev, R. A. ^{[6
,12
]}

Agudo, I. ^{[13
]}

Antonelli, L. A. ^{[14
,15
]}

Bachetti, M. ^{[16
]}

Baldini, L. ^{[17
,18
]}

Baumgartner, W. H. ^{[19
]}

Bellazzini, R. ^{[17
]}

Bianchi, S. ^{[20
]}

Bongiorno, S. D. ^{[19
]}

Bonino, R. ^{[21
,22
]}

Brez, A. ^{[17
]}

Bucciantini, N. ^{[23
,24
,25
]}

Capitanio, F. ^{[7
]}

Castellano, S. ^{[17
]}

Cavazzuti, E. ^{[26
]}

Chen, C. -T. ^{[27
]}

Ciprini, S. ^{[15
,28
]}

De Rosa, A. ^{[7
]}

Del Monte, E. ^{[7
]}

Di Gesu, L. ^{[26
]}

Di Lalla, N. ^{[29
,30
]}

Donnarumma, I. ^{[26
]}

Dovciak, M. ^{[31
]}

Ehlert, S. R. ^{[19
]}

Enoto, T. ^{[32
]}

Evangelista, Y. ^{[7
]}

Fabiani, S. ^{[7
]}

Ferrazzoli, R. ^{[7
]}

Garcia, J. A. ^{[33
]}

Gunji, S. ^{[34
]}

Hayashida, K. ^{[35
]}

Iwakiri, W. ^{[36
]}

机构：

[1] Univ Oxford, Dept Phys, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[2] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

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

[4] Univ Tubingen, Inst Astron & Astrophy, Sand 1, D-72076 Tubingen, Germany

[5] St Petersburg State Univ, Dept Astron, St Petersburg 198504, Russia

[6] Russian Acad Sci, Space Res Inst, Profsoyuznaya Str 84 32, Moscow 117997, Russia

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

[8] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T IZ1, Canada

[9] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy

[10] CNES, UPS OMP, CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[11] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland

[12] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[13] CSIC, Inst Astrofis Andalucia, Glorieta Astron s-n, E-18008 Granada, Spain

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

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

[16] INAF, Osservatorio Astron Cagliari, Via Scienza 5, I-09047 Selargius, CA, Italy

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[31] Czech Acad Sci, Astron Inst, Bocni 2 1401-1, CZ-141004 Prague, Czech Republic

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

[33] CALTECH, Pasadena, CA 91125 USA

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

[35] Osaka Univ, I-1 Yamadaoka, Suita, Osaka 5650871, Japan

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

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

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

[39] Univ New Hampshire, Dept Phys & Astron, 8 Coll Rd, Durham, NH 03824 USA

[40] Space Sci Ctr, 8 Coll Rd, Durham, NH 03824 USA

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

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

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

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

[45] Univ Strasbourg, CNRS, Observ Astronom Strasbourg, UMR 7550, F-67000 Strasbourg, France

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

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

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 524卷 / 02期

基金：

美国国家航空航天局; 俄罗斯科学基金会; 芬兰科学院;

关键词：

magnetic fields; polarization; stars: neutron; stars: oscillations; pulsars: individual: X Persei; X-rays: binaries; EMISSION; ACCRETION; POLARIZATION; DISCOVERY; SPECTRUM; ABSORPTION; LUMINOSITY; EVOLUTION; RADIATION; MODELS;

D O I：

10.1093/mnras/stad1961

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

X Persei is a persistent low-luminosity X-ray pulsar of period of & AP; 835 s in a Be binary system. The field strength at the neutron star surface is not known precisely, but indirect signs indicate a magnetic field above 10(13) G, which makes the object one of the most magnetized known X-ray pulsars. Here we present the results of observations X Persei performed with the Imaging X-ray Polarimetry Explorer (IXPE). The X-ray polarization signal was found to be strongly dependent on the spin phase of the pulsar. The energy-averaged polarization degree in 3-8 keV band varied from several to & SIM;20 per cent over the pulse with a phase dependence resembling the pulse profile. The polarization angle shows significant variation and makes two complete revolutions during the pulse period, resulting in nearly nil pulse-phase averaged polarization. Applying the rotating vector model to the IXPE data we obtain the estimates for the rotation axis inclination and its position angle on the sky, as well as for the magnetic obliquity. The derived inclination is close to the orbital inclination, reported earlier for X Persei. The polarimetric data imply a large angle between the rotation and magnetic dipole axes, which is similar to the result reported recently for the X-ray pulsar GRO J1008-57. After eliminating the effect of polarization angle rotation over the pulsar phase using the best-fitting rotating vector model, the strong dependence of the polarization degree with energy was discovered, with its value increasing from 0 at & SIM;2 keV to 30per cent at 8 keV.

引用

页码：2004 / 2014

页数：11

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