{"paper":{"title":"X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"A. A. Lutovinov, A. A. Mushtukov, A. Brez, A. De Rosa, A. Di Marco, A. E. Shtykovsky, A. F. Tennant, A. L. Peirson, A. Manfreda, A. N. Semena, A. Papitto, A. P. Marscher, A. Possenti, A. Ratheesh, A. Salganik, A. Trois, B. D. Ramsey, C. Malacaria, C. Oppedisano, C. Sgr\\`o, C.-T. Chen, C.-Y. Ng, D. A. Swartz, D. Gonz\\'alez-Caniulef, E. Cavazzuti, E. Costa, E. Del Monte, F. Capitanio, F. Kislat, F. La Monaca, F. Marin, F. Massaro, F. Muleri, F. Tavecchio, F. Tombesi, F. Xie, G. G. Pavlov, G. Matt, G. Spandre, H. Krawczynski, H. L. Marshall, I. Agudo, I. A. Mereminsky, I. Donnarumma, I. Liodakis, I. Mitsuishi, J. A. Garcia, J. Heyl, J. J. Kolodziejczak, J. Poutanen, J. Rankin, J. Vink, K. Hayashida, K. Wu, L. A. Antonelli, L. Baldini, L. Di Gesu, L. Latronico, M. Bachetti, M. C. Weisskopf, M. Dov\\v{c}iak, M. Negro, M. Perri, M. Pesce-Rollins, M. Pilia, N. Bucciantini, N. Di Lalla, N. E. Thomas, N. Omodei, O. J. Roberts, P. Kaaret, P.-O. Petrucci, P. Slane, P. Soffitta, R.A. Sunyaev, R. Bellazzini, R. Bonino, R. Ferrazzoli, R. Taverna, R. Turolla, R. W. Romani, S. Bianchi, S. Castellano, S. Ciprini, S. D. Bongiorno, S. Fabiani, S. G. Jorstad, S. Gunji, S. L. O'Dell, S. Maldera, S. Puccetti, S. R. Ehlert, S. S.Tsygankov, S. V. Forsblom, S. Zane, T. Enoto, T. Kitaguchi, T. Mizuno, T. Tamagawa, V. Doroshenko, V. F. Suleimanov, V. Karas, W. H. Baumgartner, W. Iwakiri, Y. Evangelista, Y. Tawara","submitted_at":"2023-03-30T12:26:10Z","abstract_excerpt":"X Persei is a persistent low-luminosity X-ray pulsar of period of $\\sim$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 $"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2303.17325","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2303.17325/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}