Статья

Radio emission from a pulsar’s magnetic pole revealed by general relativity

G. DesvignesLaboratoire d’Études Spatiales et d’Instrumentation en Astrophysique, Observatoire de Paris, Université Paris-Sciences-et-Lettres, Centre National de la Recherche Scientifique, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, FranceMichael KramerJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UKKejia LeeKavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People’s Republic of ChinaJ. van LeeuwenASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, NetherlandsI. H. StairsDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaA. JessnerMax-Planck-Institut für Radioastronomie, Auf dem Hügel, 69 D-53121 Bonn, GermanyIsmaël CognardLaboratoire de Physique et Chimie de l’Environnement et de l’Espace, Centre National de la Recherche Scientifique–Université d’Orléans, F-45071 Orléans, FranceLaura KasianDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaA. G. LyneJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UKB. W. StappersJodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK

2019en

ABI

Аннотация

Binary pulsars are affected by general relativity (GR), causing the spin axis of each pulsar to precess. We present polarimetric radio observations of the pulsar PSR J1906+0746 that demonstrate the validity of the geometrical model of pulsar polarization. We reconstruct the (sky-projected) polarization emission map over the pulsar's magnetic pole and predict the disappearance of the detectable emission by 2028. Two tests of GR are performed using this system, including the spin precession for strongly self-gravitating bodies. We constrain the relativistic treatment of the pulsar polarization model and measure the pulsar beaming fraction, with implications for the population of neutron stars and the expected rate of neutron star mergers.

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Идентификаторы

DOI: 10.1126/science.aav7272

Цитирования и источники

Цитирований: 2Использованных источников: 0

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