The X-ray polarimetry view of the accreting pulsar Cen X-3

Cen X-3 is the first X-ray pulsar discovered 50 years ago. Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in presence of the strong magnetic field. Here we present results of the observations of Cen X-3...

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Veröffentlicht in:	arXiv.org 2022-09
Hauptverfasser:	Tsygankov, Sergey S, Doroshenko, Victor, Poutanen, Juri, Heyl, Jeremy, Mushtukov, Alexander A, Caiazzo, Ilaria, Alessandro Di Marco, sblom, Sofia V, González-Caniulef, Denis, Klawin, Moritz, Fabio La Monaca, Malacaria, Christian, Marshall, Herman L, Muleri, Fabio, Ng, Mason, Suleimanov, Valery F, Sunyaev, Rashid A, Turolla, Roberto, Agudo, Iván, Antonelli, Lucio A, Bachetti, Matteo, Baldini, Luca, Baumgartner, Wayne H, Bellazzini, Ronaldo, Bianchi, Stefano, Bongiorno, Stephen D, Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolò, Capitanio, Fiamma, Castellano, Simone, Cavazzuti, Elisabetta, Ciprini, Stefano, Costa, Enrico, De Rosa, Alessandra, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Donnarumma, Immacolata, Dovčiak, Michal, Ehlert, Steven R, Enoto, Teruaki, Evangelista, Yuri, Fabiani, Sergio, Ferrazzoli, Riccardo, Garcia, Javier A, Gunji, Shuichi, Hayashida, Kiyoshi, Iwakiri, Wataru, Jorstad, Svetlana G, Karas, Vladimir, Kitaguchi, Takao, Kolodziejczak, Jeffery J, Krawczynski, Henric, Latronico, Luca, Liodakis, Ioannis, Maldera, Simone, Manfreda, Alberto, Marin, Frédéric, Marinucci, Andrea, Marscher, Alan P, Giorgio, Matt, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, C -Y Ng, O'Dell, Stephen L, Omodei, Nicola, Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G, Peirson, Abel L, Perri, Matteo, Pesce-Rollins, Melissa, Petrucci, Pierre-Olivier, Pilia, Maura, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D, Rankin, John, Ratheesh, Ajay, Romani, Roger W, Sgrò, Carmelo, Slane, Patrick, Soffitta, Paolo, Spandre, Gloria, Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F, Thomas, Nicolas E, Tombesi, Francesco, Trois, Alessio, Vink, Jacco, Weisskopf, Martin C, Wu, Kinwah, Xie, Fei, Zane, Silvia
Format:	Artikel
Sprache:	eng
Schlagworte:	Birefringence Deposition Luminosity Neutron stars Physics - High Energy Astrophysical Phenomena Polarimetry Polarization Pulsars Radiation X ray imagery
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creator	Tsygankov, Sergey S Doroshenko, Victor Poutanen, Juri Heyl, Jeremy Mushtukov, Alexander A Caiazzo, Ilaria Alessandro Di Marco sblom, Sofia V González-Caniulef, Denis Klawin, Moritz Fabio La Monaca Malacaria, Christian Marshall, Herman L Muleri, Fabio Ng, Mason Suleimanov, Valery F Sunyaev, Rashid A Turolla, Roberto Agudo, Iván Antonelli, Lucio A Bachetti, Matteo Baldini, Luca Baumgartner, Wayne H Bellazzini, Ronaldo Bianchi, Stefano Bongiorno, Stephen D Bonino, Raffaella Brez, Alessandro Bucciantini, Niccolò Capitanio, Fiamma Castellano, Simone Cavazzuti, Elisabetta Ciprini, Stefano Costa, Enrico De Rosa, Alessandra Ettore Del Monte Laura Di Gesu Niccolò Di Lalla Donnarumma, Immacolata Dovčiak, Michal Ehlert, Steven R Enoto, Teruaki Evangelista, Yuri Fabiani, Sergio Ferrazzoli, Riccardo Garcia, Javier A Gunji, Shuichi Hayashida, Kiyoshi Iwakiri, Wataru Jorstad, Svetlana G Karas, Vladimir Kitaguchi, Takao Kolodziejczak, Jeffery J Krawczynski, Henric Latronico, Luca Liodakis, Ioannis Maldera, Simone Manfreda, Alberto Marin, Frédéric Marinucci, Andrea Marscher, Alan P Giorgio, Matt Mitsuishi, Ikuyuki Mizuno, Tsunefumi C -Y Ng O'Dell, Stephen L Omodei, Nicola Oppedisano, Chiara Papitto, Alessandro Pavlov, George G Peirson, Abel L Perri, Matteo Pesce-Rollins, Melissa Petrucci, Pierre-Olivier Pilia, Maura Possenti, Andrea Puccetti, Simonetta Ramsey, Brian D Rankin, John Ratheesh, Ajay Romani, Roger W Sgrò, Carmelo Slane, Patrick Soffitta, Paolo Spandre, Gloria Tamagawa, Toru Tavecchio, Fabrizio Taverna, Roberto Tawara, Yuzuru Tennant, Allyn F Thomas, Nicolas E Tombesi, Francesco Trois, Alessio Vink, Jacco Weisskopf, Martin C Wu, Kinwah Xie, Fei Zane, Silvia
description	Cen X-3 is the first X-ray pulsar discovered 50 years ago. Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in presence of the strong magnetic field. Here we present results of the observations of Cen X-3 performed with the Imaging X-ray Polarimetry Explorer. The source exhibited significant flux variability and was observed in two states different by a factor of ~20 in flux. In the low-luminosity state no significant polarization was found either in pulse phase-averaged (with the 3$\sigma$ upper limit of 12%) or phase-resolved data (the 3$\sigma$ upper limits are 20-30%). In the bright state the polarization degree of 5.8$\pm$0.3% and polarization angle of $49.6\deg\pm1.5\deg$ with significance of about 20$\sigma$ was measured from the spectro-polarimetric analysis of the phase-averaged data. The phase-resolved analysis showed a significant anti-correlation between the flux and the polarization degree as well as strong variations of the polarization angle. The fit with the rotating vector model indicates a position angle of the pulsar spin axis of about 49$\deg$ and a magnetic obliquity of 17$\deg$. The detected relatively low polarization can be explained if the upper layers of the neutron star surface are overheated by the accreted matter and the conversion of the polarization modes occurs within the transition region between the upper hot layer and a cooler underlying atmosphere. A fraction of polarization signal can also be produced by reflection of radiation from the neutron star surface and the accretion curtain.
doi_str_mv	10.48550/arxiv.2209.02447
format	Article
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Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in presence of the strong magnetic field. Here we present results of the observations of Cen X-3 performed with the Imaging X-ray Polarimetry Explorer. The source exhibited significant flux variability and was observed in two states different by a factor of ~20 in flux. In the low-luminosity state no significant polarization was found either in pulse phase-averaged (with the 3$\sigma$ upper limit of 12%) or phase-resolved data (the 3$\sigma$ upper limits are 20-30%). In the bright state the polarization degree of 5.8$\pm$0.3% and polarization angle of $49.6\deg\pm1.5\deg$ with significance of about 20$\sigma$ was measured from the spectro-polarimetric analysis of the phase-averaged data. The phase-resolved analysis showed a significant anti-correlation between the flux and the polarization degree as well as strong variations of the polarization angle. The fit with the rotating vector model indicates a position angle of the pulsar spin axis of about 49$\deg$ and a magnetic obliquity of 17$\deg$. The detected relatively low polarization can be explained if the upper layers of the neutron star surface are overheated by the accreted matter and the conversion of the polarization modes occurs within the transition region between the upper hot layer and a cooler underlying atmosphere. A fraction of polarization signal can also be produced by reflection of radiation from the neutron star surface and the accretion curtain.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2209.02447</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Birefringence ; Deposition ; Luminosity ; Neutron stars ; Physics - High Energy Astrophysical Phenomena ; Polarimetry ; Polarization ; Pulsars ; Radiation ; X ray imagery</subject><ispartof>arXiv.org, 2022-09</ispartof><rights>2022. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2209.02447$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/2041-8213/aca486$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Tsygankov, Sergey S</creatorcontrib><creatorcontrib>Doroshenko, Victor</creatorcontrib><creatorcontrib>Poutanen, Juri</creatorcontrib><creatorcontrib>Heyl, Jeremy</creatorcontrib><creatorcontrib>Mushtukov, Alexander A</creatorcontrib><creatorcontrib>Caiazzo, Ilaria</creatorcontrib><creatorcontrib>Alessandro Di Marco</creatorcontrib><creatorcontrib>sblom, Sofia V</creatorcontrib><creatorcontrib>González-Caniulef, Denis</creatorcontrib><creatorcontrib>Klawin, Moritz</creatorcontrib><creatorcontrib>Fabio La Monaca</creatorcontrib><creatorcontrib>Malacaria, Christian</creatorcontrib><creatorcontrib>Marshall, Herman L</creatorcontrib><creatorcontrib>Muleri, Fabio</creatorcontrib><creatorcontrib>Ng, Mason</creatorcontrib><creatorcontrib>Suleimanov, Valery F</creatorcontrib><creatorcontrib>Sunyaev, Rashid A</creatorcontrib><creatorcontrib>Turolla, Roberto</creatorcontrib><creatorcontrib>Agudo, Iván</creatorcontrib><creatorcontrib>Antonelli, Lucio A</creatorcontrib><creatorcontrib>Bachetti, Matteo</creatorcontrib><creatorcontrib>Baldini, Luca</creatorcontrib><creatorcontrib>Baumgartner, Wayne H</creatorcontrib><creatorcontrib>Bellazzini, Ronaldo</creatorcontrib><creatorcontrib>Bianchi, 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Riccardo</creatorcontrib><creatorcontrib>Garcia, Javier A</creatorcontrib><creatorcontrib>Gunji, Shuichi</creatorcontrib><creatorcontrib>Hayashida, Kiyoshi</creatorcontrib><creatorcontrib>Iwakiri, Wataru</creatorcontrib><creatorcontrib>Jorstad, Svetlana G</creatorcontrib><creatorcontrib>Karas, Vladimir</creatorcontrib><creatorcontrib>Kitaguchi, Takao</creatorcontrib><creatorcontrib>Kolodziejczak, Jeffery J</creatorcontrib><creatorcontrib>Krawczynski, Henric</creatorcontrib><creatorcontrib>Latronico, Luca</creatorcontrib><creatorcontrib>Liodakis, Ioannis</creatorcontrib><creatorcontrib>Maldera, Simone</creatorcontrib><creatorcontrib>Manfreda, Alberto</creatorcontrib><creatorcontrib>Marin, Frédéric</creatorcontrib><creatorcontrib>Marinucci, Andrea</creatorcontrib><creatorcontrib>Marscher, Alan P</creatorcontrib><creatorcontrib>Giorgio, Matt</creatorcontrib><creatorcontrib>Mitsuishi, Ikuyuki</creatorcontrib><creatorcontrib>Mizuno, Tsunefumi</creatorcontrib><creatorcontrib>C -Y Ng</creatorcontrib><creatorcontrib>O'Dell, Stephen L</creatorcontrib><creatorcontrib>Omodei, Nicola</creatorcontrib><creatorcontrib>Oppedisano, Chiara</creatorcontrib><creatorcontrib>Papitto, Alessandro</creatorcontrib><creatorcontrib>Pavlov, George G</creatorcontrib><creatorcontrib>Peirson, Abel L</creatorcontrib><creatorcontrib>Perri, Matteo</creatorcontrib><creatorcontrib>Pesce-Rollins, Melissa</creatorcontrib><creatorcontrib>Petrucci, Pierre-Olivier</creatorcontrib><creatorcontrib>Pilia, Maura</creatorcontrib><creatorcontrib>Possenti, Andrea</creatorcontrib><creatorcontrib>Puccetti, Simonetta</creatorcontrib><creatorcontrib>Ramsey, Brian D</creatorcontrib><creatorcontrib>Rankin, John</creatorcontrib><creatorcontrib>Ratheesh, Ajay</creatorcontrib><creatorcontrib>Romani, Roger W</creatorcontrib><creatorcontrib>Sgrò, Carmelo</creatorcontrib><creatorcontrib>Slane, Patrick</creatorcontrib><creatorcontrib>Soffitta, Paolo</creatorcontrib><creatorcontrib>Spandre, Gloria</creatorcontrib><creatorcontrib>Tamagawa, Toru</creatorcontrib><creatorcontrib>Tavecchio, Fabrizio</creatorcontrib><creatorcontrib>Taverna, Roberto</creatorcontrib><creatorcontrib>Tawara, Yuzuru</creatorcontrib><creatorcontrib>Tennant, Allyn F</creatorcontrib><creatorcontrib>Thomas, Nicolas E</creatorcontrib><creatorcontrib>Tombesi, Francesco</creatorcontrib><creatorcontrib>Trois, Alessio</creatorcontrib><creatorcontrib>Vink, Jacco</creatorcontrib><creatorcontrib>Weisskopf, Martin C</creatorcontrib><creatorcontrib>Wu, Kinwah</creatorcontrib><creatorcontrib>Xie, Fei</creatorcontrib><creatorcontrib>Zane, Silvia</creatorcontrib><title>The X-ray polarimetry view of the accreting pulsar Cen X-3</title><title>arXiv.org</title><description>Cen X-3 is the first X-ray pulsar discovered 50 years ago. Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in presence of the strong magnetic field. Here we present results of the observations of Cen X-3 performed with the Imaging X-ray Polarimetry Explorer. The source exhibited significant flux variability and was observed in two states different by a factor of ~20 in flux. In the low-luminosity state no significant polarization was found either in pulse phase-averaged (with the 3$\sigma$ upper limit of 12%) or phase-resolved data (the 3$\sigma$ upper limits are 20-30%). In the bright state the polarization degree of 5.8$\pm$0.3% and polarization angle of $49.6\deg\pm1.5\deg$ with significance of about 20$\sigma$ was measured from the spectro-polarimetric analysis of the phase-averaged data. The phase-resolved analysis showed a significant anti-correlation between the flux and the polarization degree as well as strong variations of the polarization angle. The fit with the rotating vector model indicates a position angle of the pulsar spin axis of about 49$\deg$ and a magnetic obliquity of 17$\deg$. The detected relatively low polarization can be explained if the upper layers of the neutron star surface are overheated by the accreted matter and the conversion of the polarization modes occurs within the transition region between the upper hot layer and a cooler underlying atmosphere. A fraction of polarization signal can also be produced by reflection of radiation from the neutron star surface and the accretion curtain.</description><subject>Birefringence</subject><subject>Deposition</subject><subject>Luminosity</subject><subject>Neutron stars</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Polarimetry</subject><subject>Polarization</subject><subject>Pulsars</subject><subject>Radiation</subject><subject>X ray 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E</creator><creator>Tombesi, Francesco</creator><creator>Trois, Alessio</creator><creator>Vink, Jacco</creator><creator>Weisskopf, Martin C</creator><creator>Wu, Kinwah</creator><creator>Xie, Fei</creator><creator>Zane, Silvia</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20220906</creationdate><title>The X-ray polarimetry view of the accreting pulsar Cen X-3</title><author>Tsygankov, Sergey S ; Doroshenko, Victor ; Poutanen, Juri ; Heyl, Jeremy ; Mushtukov, Alexander A ; Caiazzo, Ilaria ; Alessandro Di Marco ; sblom, Sofia V ; González-Caniulef, Denis ; Klawin, Moritz ; Fabio La Monaca ; Malacaria, Christian ; Marshall, Herman L ; Muleri, Fabio ; Ng, Mason ; Suleimanov, Valery F ; Sunyaev, Rashid A ; Turolla, Roberto ; Agudo, Iván ; Antonelli, Lucio A ; Bachetti, Matteo ; Baldini, Luca ; Baumgartner, Wayne H ; Bellazzini, Ronaldo ; Bianchi, Stefano ; Bongiorno, Stephen D ; Bonino, Raffaella ; Brez, Alessandro ; Bucciantini, Niccolò ; Capitanio, Fiamma ; Castellano, Simone ; Cavazzuti, Elisabetta ; Ciprini, Stefano ; Costa, Enrico ; De Rosa, Alessandra ; Ettore Del Monte ; Laura Di Gesu ; Niccolò Di Lalla ; Donnarumma, Immacolata ; Dovčiak, Michal ; Ehlert, Steven R ; Enoto, Teruaki ; Evangelista, Yuri ; Fabiani, Sergio ; Ferrazzoli, Riccardo ; Garcia, Javier A ; Gunji, Shuichi ; Hayashida, Kiyoshi ; Iwakiri, Wataru ; Jorstad, Svetlana G ; Karas, Vladimir ; Kitaguchi, Takao ; Kolodziejczak, Jeffery J ; Krawczynski, Henric ; Latronico, Luca ; Liodakis, Ioannis ; Maldera, Simone ; Manfreda, Alberto ; Marin, Frédéric ; Marinucci, Andrea ; Marscher, Alan P ; Giorgio, Matt ; Mitsuishi, Ikuyuki ; Mizuno, Tsunefumi ; C -Y Ng ; O'Dell, Stephen L ; Omodei, Nicola ; Oppedisano, Chiara ; Papitto, Alessandro ; Pavlov, George G ; Peirson, Abel L ; Perri, Matteo ; Pesce-Rollins, Melissa ; Petrucci, Pierre-Olivier ; Pilia, Maura ; Possenti, Andrea ; Puccetti, Simonetta ; Ramsey, Brian D ; Rankin, John ; Ratheesh, Ajay ; Romani, Roger W ; Sgrò, Carmelo ; Slane, Patrick ; Soffitta, Paolo ; Spandre, Gloria ; Tamagawa, Toru ; Tavecchio, Fabrizio ; Taverna, Roberto ; Tawara, Yuzuru ; Tennant, Allyn F ; Thomas, Nicolas E ; Tombesi, Francesco ; Trois, Alessio ; Vink, Jacco ; Weisskopf, Martin C ; Wu, Kinwah ; Xie, Fei ; Zane, 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Christian</au><au>Marshall, Herman L</au><au>Muleri, Fabio</au><au>Ng, Mason</au><au>Suleimanov, Valery F</au><au>Sunyaev, Rashid A</au><au>Turolla, Roberto</au><au>Agudo, Iván</au><au>Antonelli, Lucio A</au><au>Bachetti, Matteo</au><au>Baldini, Luca</au><au>Baumgartner, Wayne H</au><au>Bellazzini, Ronaldo</au><au>Bianchi, Stefano</au><au>Bongiorno, Stephen D</au><au>Bonino, Raffaella</au><au>Brez, Alessandro</au><au>Bucciantini, Niccolò</au><au>Capitanio, Fiamma</au><au>Castellano, Simone</au><au>Cavazzuti, Elisabetta</au><au>Ciprini, Stefano</au><au>Costa, Enrico</au><au>De Rosa, Alessandra</au><au>Ettore Del Monte</au><au>Laura Di Gesu</au><au>Niccolò Di Lalla</au><au>Donnarumma, Immacolata</au><au>Dovčiak, Michal</au><au>Ehlert, Steven R</au><au>Enoto, Teruaki</au><au>Evangelista, Yuri</au><au>Fabiani, Sergio</au><au>Ferrazzoli, Riccardo</au><au>Garcia, Javier A</au><au>Gunji, Shuichi</au><au>Hayashida, Kiyoshi</au><au>Iwakiri, Wataru</au><au>Jorstad, Svetlana G</au><au>Karas, Vladimir</au><au>Kitaguchi, Takao</au><au>Kolodziejczak, Jeffery J</au><au>Krawczynski, Henric</au><au>Latronico, Luca</au><au>Liodakis, Ioannis</au><au>Maldera, Simone</au><au>Manfreda, Alberto</au><au>Marin, Frédéric</au><au>Marinucci, Andrea</au><au>Marscher, Alan P</au><au>Giorgio, Matt</au><au>Mitsuishi, Ikuyuki</au><au>Mizuno, Tsunefumi</au><au>C -Y Ng</au><au>O'Dell, Stephen L</au><au>Omodei, Nicola</au><au>Oppedisano, Chiara</au><au>Papitto, Alessandro</au><au>Pavlov, George G</au><au>Peirson, Abel L</au><au>Perri, Matteo</au><au>Pesce-Rollins, Melissa</au><au>Petrucci, Pierre-Olivier</au><au>Pilia, Maura</au><au>Possenti, Andrea</au><au>Puccetti, Simonetta</au><au>Ramsey, Brian D</au><au>Rankin, John</au><au>Ratheesh, Ajay</au><au>Romani, Roger W</au><au>Sgrò, Carmelo</au><au>Slane, Patrick</au><au>Soffitta, Paolo</au><au>Spandre, Gloria</au><au>Tamagawa, Toru</au><au>Tavecchio, Fabrizio</au><au>Taverna, Roberto</au><au>Tawara, Yuzuru</au><au>Tennant, Allyn F</au><au>Thomas, Nicolas E</au><au>Tombesi, Francesco</au><au>Trois, Alessio</au><au>Vink, Jacco</au><au>Weisskopf, Martin C</au><au>Wu, Kinwah</au><au>Xie, Fei</au><au>Zane, Silvia</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The X-ray polarimetry view of the accreting pulsar Cen X-3</atitle><jtitle>arXiv.org</jtitle><date>2022-09-06</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Cen X-3 is the first X-ray pulsar discovered 50 years ago. Radiation from such objects is expected to be highly polarized due to birefringence of plasma and vacuum associated with propagation of photons in presence of the strong magnetic field. Here we present results of the observations of Cen X-3 performed with the Imaging X-ray Polarimetry Explorer. The source exhibited significant flux variability and was observed in two states different by a factor of ~20 in flux. In the low-luminosity state no significant polarization was found either in pulse phase-averaged (with the 3$\sigma$ upper limit of 12%) or phase-resolved data (the 3$\sigma$ upper limits are 20-30%). In the bright state the polarization degree of 5.8$\pm$0.3% and polarization angle of $49.6\deg\pm1.5\deg$ with significance of about 20$\sigma$ was measured from the spectro-polarimetric analysis of the phase-averaged data. The phase-resolved analysis showed a significant anti-correlation between the flux and the polarization degree as well as strong variations of the polarization angle. The fit with the rotating vector model indicates a position angle of the pulsar spin axis of about 49$\deg$ and a magnetic obliquity of 17$\deg$. The detected relatively low polarization can be explained if the upper layers of the neutron star surface are overheated by the accreted matter and the conversion of the polarization modes occurs within the transition region between the upper hot layer and a cooler underlying atmosphere. A fraction of polarization signal can also be produced by reflection of radiation from the neutron star surface and the accretion curtain.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2209.02447</doi><oa>free_for_read</oa></addata></record>
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subjects	Birefringence Deposition Luminosity Neutron stars Physics - High Energy Astrophysical Phenomena Polarimetry Polarization Pulsars Radiation X ray imagery
title	The X-ray polarimetry view of the accreting pulsar Cen X-3
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