Journal Article

Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit

Bachetti, Matteo, Poutanen, Juri, Marshall, Herman L., O’Dell, Stephen L., Tsygankov, Sergey S., Kitaguchi, Takao, Possenti, Andrea, Bucciantini, Niccolò, Papitto, Alessandro, Enoto, Teruaki, Oppedisano, Chiara, Zane, Silvia, Latronico, Luca, Soffitta, Paolo, Fabiani, Sergio, Ramsey, Brian D., Wu, Kinwah, Cavazzuti, Elisabetta, Heyl, Jeremy, Weisskopf, Martin C., Di Gesu, Laura, Bianchi, Stefano, Iwakiri, Wataru, Ratheesh, Ajay, Bongiorno, Stephen D., Petrucci, Pierre-Olivier, Donnarumma, Immacolata, Mitsuishi, Ikuyuki, Brez, Alessandro, Watanabe, Eri, Xie, Fei, La Monaca, Fabio, Rankin, John, Baumgartner, Wayne H., Trois, Alessio, Bellazzini, Ronaldo, Ng, C.-Y., Liodakis, Ioannis, Muleri, Fabio, Bonino, Raffaella, Slane, Patrick, Tawara, Yuzuru, Tavecchio, Fabrizio, Negro, Michela, Marscher, Alan P., Agudo, Iván, Liu, Kuan, Matt, Giorgio, Maldera, Simone, Tombesi, Francesco, Dovčiak, Michal, Tennant, Allyn F., Peirson, Abel L., Ferrazzoli, Riccardo, Omodei, Nicola, Antonelli, Lucio A., Karas, Vladimir, Massaro, Francesco, Castellano, Simone, Tamagawa, Toru, Ehlert, Steven R., Capitanio, Fiamma, Kolodziejcz

2022

Overview

Pulsar wind nebulae are formed when outflows of relativistic electrons and positrons hit the surrounding supernova remnant or interstellar medium at a shock front. The Vela pulsar wind nebula is powered by a young pulsar (B0833-45, aged 11,000 years) 1 and located inside an extended structure called Vela X, which is itself inside the supernova remnant 2 . Previous X-ray observations revealed two prominent arcs that are bisected by a jet and counter jet 3 , 4 . Radio maps have shown high linear polarization of 60% in the outer regions of the nebula 5 . Here we report an X-ray observation of the inner part of the nebula, where polarization can exceed 60% at the leading edge—approaching the theoretical limit of what can be produced by synchrotron emission. We infer that, in contrast with the case of the supernova remnant, the electrons in the pulsar wind nebula are accelerated with little or no turbulence in a highly uniform magnetic field. Polarization can exceed 60% at the leading edge of the inner part of the Vela pulsar wind nebula; in contrast with the case of the supernova remnant, the electrons in the pulsar wind nebula are accelerated with little or no turbulence in a highly uniform magnetic field.

• Publisher: Nature Publishing Group UK,Nature Publishing Group
• Subject: 140/146 / 639/33/34/864 / 639/33/34/866 / Electrons / Energy / Humanities and Social Sciences / Interstellar matter / Interstellar medium / Linear polarization / Magnetic fields / multidisciplinary / Nebulae / Polarization / Positrons / Pulsar winds / Pulsars / Radiation / Science / Science (multidisciplinary) / Sciences of the Universe / Sensors / Stellar winds / Supernova / Supernova remnants / Supernovae / Symmetry / Synchrotrons / X-ray astronomy / X-rays