用IXPE极化法测定X射线脉冲星的几何形状

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用IXPE极化法测定X射线脉冲星的几何形状

Determination of X-ray pulsar geometry with IXPE polarimetry

论文作者

Doroshenko, Victor, Poutanen, Juri, Tsygankov, Sergey S., Suleimanov, Valery F., Bachetti, Matteo, Caiazzo, Ilaria, Costa, Enrico, Di Marco, Alessandro, Heyl, Jeremy, La Monaca, Fabio, Muleri, Fabio, Mushtukov, Alexander A., Pavlov, George G., Ramsey, Brian D., Rankin, John, Santangelo, Andrea, Soffitta, Paolo, Staubert, Rüdiger, Weisskopf, Martin C., Zane, Silvia, Agudo, Iván, Antonelli, Lucio A., 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, De Rosa, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccolò, Donnarumma, Immacolata, Dovciak, 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., Marshall, Herman L., Matt, Giorgio, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Ng, C. -Y., O'Dell, Stephen L., Omodei, Nicola, Oppedisano, Chiara, Papitto, Alessandro, Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Pilia, Maura, Possenti, Andrea, Puccetti, Simonetta, Ratheesh, Ajay, Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Spandre, Gloria, Sunyaev, Rashid A., Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicolas E., Tombesi, Francesco, Trois, Alessio, Turolla, Roberto, Vink, Jacco, Wu, Kinwah, Xie, Fei

论文摘要

使用成像X射线极化探索器对X射线脉冲星的观察，我们报告了从积聚中子恒星中对极化信号的高度显着（$>17σ$）的检测。发现观察到的$ \ sim $ 10 \％的线性极化程度远低于该物体的理论期望，并且在PULSAR的整个自旋周期中保持较低。极化度和角度都表现出脉冲相的可变性，这使我们能够测量脉冲星旋转位置角57（2）deg和磁性斜率12（4）dEG，这是详细建模X射线脉冲星的详细建模的重要步骤。将我们的结果与光学偏光数据相结合，我们发现中子恒星的自旋轴和二进制轨道的角动量至少被至少$ \ sim $ 20摄氏度错误对准，这是支持模型的强有力的论点，该模型解释了与中子恒星的presevessions presevession the natermon star的稳定性。

Using observations of X-ray pulsar Her X-1 by the Imaging X-ray Polarimetry Explorer, we report on a highly significant ($>17σ$) detection of the polarization signal from an accreting neutron star. The observed degree of the linear polarization of $\sim$10\% is found to be far below theoretical expectations for this object, and stays low throughout the spin cycle of the pulsar. Both the polarization degree and the angle exhibit variability with pulse phase, which allowed us to measure the pulsar spin position angle 57(2) deg and the magnetic obliquity 12(4) deg, which is an essential step towards detailed modelling of the intrinsic emission of X-ray pulsars. Combining our results with the optical polarimetric data, we find that the spin axis of the neutron star and the angular momentum of the binary orbit are misaligned by at least $\sim$20 deg, which is a strong argument in support of the models explaining stability of the observed super-orbital variability with the precession of the neutron star.

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