Magnetars are neutron stars with ultrastrong magnetic fields, which can be observed in x-rays. Polarization measurements could provide information on their magnetic fields and surface properties. We observed polarized x-rays from the magnetar 4U 0142+61 using the Imaging X-ray Polarimetry Explorer and found a linear polarization degree of 13.5 ± 0.8% averaged over the 2– to 8–kilo–electron volt band. The polarization changes with energy: The degree is 15.0 ± 1.0% at 2 to 4 kilo–electron volts, drops below the instrumental sensitivity ~4 to 5 kilo–electron volts, and rises to 35.2 ± 7.1% at 5.5 to 8 kilo–electron volts. The polarization angle also changes by 90° at ~4 to 5 kilo–electron volts. These results are consistent with a model in which thermal radiation from the magnetar surface is reprocessed by scattering off charged particles in the magnetosphere.

Polarized x-rays from a magnetar

Negro M.;Bonino R.;Latronico L.;Maldera S.;
2022-01-01

Abstract

Magnetars are neutron stars with ultrastrong magnetic fields, which can be observed in x-rays. Polarization measurements could provide information on their magnetic fields and surface properties. We observed polarized x-rays from the magnetar 4U 0142+61 using the Imaging X-ray Polarimetry Explorer and found a linear polarization degree of 13.5 ± 0.8% averaged over the 2– to 8–kilo–electron volt band. The polarization changes with energy: The degree is 15.0 ± 1.0% at 2 to 4 kilo–electron volts, drops below the instrumental sensitivity ~4 to 5 kilo–electron volts, and rises to 35.2 ± 7.1% at 5.5 to 8 kilo–electron volts. The polarization angle also changes by 90° at ~4 to 5 kilo–electron volts. These results are consistent with a model in which thermal radiation from the magnetar surface is reprocessed by scattering off charged particles in the magnetosphere.
2022
378
6620
646
650
https://arxiv.org/abs/2205.08898
Taverna R.; Turolla R.; Muleri F.; Heyl J.; Zane S.; Baldini L.; Gonzalez-Caniulef D.; Bachetti M.; Rankin J.; Caiazzo I.; Di Lalla N.; Doroshenko V.; Errando M.; Gau E.; Kirmizibayrak D.; Krawczynski H.; Negro M.; Ng M.; Omodei N.; Possenti A.; Tamagawa T.; Uchiyama K.; Weisskopf M.C.; Agudo I.; Antonelli L.A.; Baumgartner W.H.; Bellazzini R.; Bianchi S.; Bongiorno S.D.; Bonino R.; Brez A.; Bucciantini N.; Capitanio F.; Castellano S.; Cavazzuti E.; Ciprini S.; Costa E.; De Rosa A.; Del Monte E.; Di Gesu L.; Di Marco A.; Donnarumma I.; Doviak M.; Ehlert S.R.; Enoto T.; Evangelista Y.; Fabiani S.; Ferrazzoli R.; Garcia J.A.; Gunji S.; Hayashida K.; Iwakiri W.; Jorstad S.G.; Karas V.; Kitaguchi T.; Kolodziejczak J.J.; La Monaca F.; Latronico L.; Liodakis I.; Maldera S.; Manfreda A.; Marin F.; Marinucci A.; Marscher A.P.; Marshall H.L.; Matt G.; Mitsuishi I.; Mizuno T.; Ng S.C.-Y.; O'Dell S.L.; Oppedisano C.; Papitto A.; Pavlov G.G.; Peirson A.L.; Perri M.; Pesce-Rollins M.; Pilia M.; Poutanen J.; Puccetti S.; Ramsey B.D.; Ratheesh A.; Romani R.W.; Sgro C.; Slane P.; Soffitta P.; Spandre G.; Tavecchio F.; Tawara Y.; Tennant A.F.; Thomas N.E.; Tombesi F.; Trois A.; Tsygankov S.S.; Vink J.; Wu K.; Xie F.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/1891183
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