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Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit. / Xie, Fei; Di Marco, Alessandro; La Monaca, Fabio; Liu, Kuan; Muleri, Fabio; Bucciantini, Niccolò; Romani, Roger W.; Costa, Enrico; Rankin, John; Soffitta, Paolo; Bachetti, Matteo; Di Lalla, Niccolò; Fabiani, Sergio; Ferrazzoli, Riccardo; Gunji, Shuichi; Latronico, Luca; Negro, Michela; Omodei, Nicola; Pilia, Maura; Trois, Alessio; Watanabe, Eri; Agudo, Iván; Antonelli, Lucio A.; Baldini, Luca; Baumgartner, Wayne H.; Bellazzini, Ronaldo; Bianchi, Stefano; Bongiorno, Stephen D.; Bonino, Raffaella; Brez, Alessandro; Capitanio, Fiamma; Castellano, Simone; Cavazzuti, Elisabetta; Ciprini, Stefano; De Rosa, Alessandra; Del Monte, Ettore; Di Gesu, Laura; Donnarumma, Immacolata; Doroshenko, Victor; Dovčiak, Michal; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Yuri; Garcia, Javier A.; Hayashida, Kiyoshi; Heyl, Jeremy; Iwakiri, Wataru; Jorstad, Svetlana G.; Karas, Vladimir; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Krawczynski, Henric; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marin, Frédéric; Marinucci, Andrea; Marscher, Alan P.; Marshall, Herman L.; Massaro, Francesco; Matt, Giorgio; Mitsuishi, Ikuyuki; Mizuno, Tsunefumi; Ng, C.-Y.; O’Dell, Stephen L.; Oppedisano, Chiara; Papitto, Alessandro; Pavlov, George G.; Peirson, Abel L.; Perri, Matteo; Pesce-Rollins, Melissa; Petrucci, Pierre-Olivier; Possenti, Andrea; Poutanen, Juri; Puccetti, Simonetta; Ramsey, Brian D.; Ratheesh, Ajay; Sgró, Carmelo; Slane, Patrick; Spandre, Gloria; Tamagawa, Toru; Tavecchio, Fabrizio; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicolas E.; Tombesi, Francesco; Tsygankov, Sergey S.; Turolla, Roberto; Vink, Jacco; Weisskopf, Martin C.; Wu, Kinwah; Zane, Silvia.
в:
Nature, Том 612, № 7941, 2022, стр. 658-660.
Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование
Harvard
Xie, F, Di Marco, A, La Monaca, F, Liu, K, Muleri, F, Bucciantini, N, Romani, RW, Costa, E, Rankin, J, Soffitta, P, Bachetti, M, Di Lalla, N, Fabiani, S, Ferrazzoli, R, Gunji, S, Latronico, L, Negro, M, Omodei, N, Pilia, M, Trois, A, Watanabe, E, Agudo, I, Antonelli, LA, Baldini, L, Baumgartner, WH, Bellazzini, R, Bianchi, S, Bongiorno, SD, Bonino, R, Brez, A, Capitanio, F, Castellano, S, Cavazzuti, E, Ciprini, S, De Rosa, A, Del Monte, E, Di Gesu, L, Donnarumma, I, Doroshenko, V, Dovčiak, M, Ehlert, SR, Enoto, T, Evangelista, Y, Garcia, JA, Hayashida, K, Heyl, J, Iwakiri, W
, Jorstad, SG, Karas, V, Kitaguchi, T, Kolodziejczak, JJ, Krawczynski, H, Liodakis, I, Maldera, S, Manfreda, A, Marin, F, Marinucci, A, Marscher, AP, Marshall, HL, Massaro, F, Matt, G, Mitsuishi, I, Mizuno, T, Ng, C-Y, O’Dell, SL, Oppedisano, C, Papitto, A, Pavlov, GG, Peirson, AL, Perri, M, Pesce-Rollins, M, Petrucci, P-O, Possenti, A, Poutanen, J, Puccetti, S, Ramsey, BD, Ratheesh, A, Sgró, C, Slane, P, Spandre, G, Tamagawa, T, Tavecchio, F, Taverna, R, Tawara, Y, Tennant, AF, Thomas, NE, Tombesi, F, Tsygankov, SS, Turolla, R, Vink, J, Weisskopf, MC, Wu, K & Zane, S 2022, '
Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit',
Nature, Том. 612, № 7941, стр. 658-660.
https://doi.org/10.1038/s41586-022-05476-5APA
Xie, F., Di Marco, A., La Monaca, F., Liu, K., Muleri, F., Bucciantini, N., Romani, R. W., Costa, E., Rankin, J., Soffitta, P., Bachetti, M., Di Lalla, N., Fabiani, S., Ferrazzoli, R., Gunji, S., Latronico, L., Negro, M., Omodei, N., Pilia, M., ... Zane, S. (2022).
Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit.
Nature,
612(7941), 658-660.
https://doi.org/10.1038/s41586-022-05476-5Vancouver
Author
Xie, Fei ; Di Marco, Alessandro ; La Monaca, Fabio ; Liu, Kuan ; Muleri, Fabio ; Bucciantini, Niccolò ; Romani, Roger W. ; Costa, Enrico ; Rankin, John ; Soffitta, Paolo ; Bachetti, Matteo ; Di Lalla, Niccolò ; Fabiani, Sergio ; Ferrazzoli, Riccardo ; Gunji, Shuichi ; Latronico, Luca ; Negro, Michela ; Omodei, Nicola ; Pilia, Maura ; Trois, Alessio ; Watanabe, Eri ; Agudo, Iván ; Antonelli, Lucio A. ; Baldini, Luca ; Baumgartner, Wayne H. ; Bellazzini, Ronaldo ; Bianchi, Stefano ; Bongiorno, Stephen D. ; Bonino, Raffaella ; Brez, Alessandro ; Capitanio, Fiamma ; Castellano, Simone ; Cavazzuti, Elisabetta ; Ciprini, Stefano ; De Rosa, Alessandra ; Del Monte, Ettore ; Di Gesu, Laura ; Donnarumma, Immacolata ; Doroshenko, Victor ; Dovčiak, Michal ; Ehlert, Steven R. ; Enoto, Teruaki ; Evangelista, Yuri ; Garcia, Javier A. ; Hayashida, Kiyoshi ; Heyl, Jeremy ; Iwakiri, Wataru
; Jorstad, Svetlana G. ; Karas, Vladimir ; Kitaguchi, Takao ; Kolodziejczak, Jeffery J. ; Krawczynski, Henric ; Liodakis, Ioannis ; Maldera, Simone ; Manfreda, Alberto ; Marin, Frédéric ; Marinucci, Andrea ; Marscher, Alan P. ; Marshall, Herman L. ; Massaro, Francesco ; Matt, Giorgio ; Mitsuishi, Ikuyuki ; Mizuno, Tsunefumi ; Ng, C.-Y. ; O’Dell, Stephen L. ; Oppedisano, Chiara ; Papitto, Alessandro ; Pavlov, George G. ; Peirson, Abel L. ; Perri, Matteo ; Pesce-Rollins, Melissa ; Petrucci, Pierre-Olivier ; Possenti, Andrea ; Poutanen, Juri ; Puccetti, Simonetta ; Ramsey, Brian D. ; Ratheesh, Ajay ; Sgró, Carmelo ; Slane, Patrick ; Spandre, Gloria ; Tamagawa, Toru ; Tavecchio, Fabrizio ; Taverna, Roberto ; Tawara, Yuzuru ; Tennant, Allyn F. ; Thomas, Nicolas E. ; Tombesi, Francesco ; Tsygankov, Sergey S. ; Turolla, Roberto ; Vink, Jacco ; Weisskopf, Martin C. ; Wu, Kinwah ; Zane, Silvia. /
Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit. в:
Nature. 2022 ; Том 612, № 7941. стр. 658-660.
BibTeX
@article{a709891fc750430a8273fe8271544238,
title = "Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit",
abstract = "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 remnant2. Previous X-ray observations revealed two prominent arcs that are bisected by a jet and counter jet3,4. Radio maps have shown high linear polarization of 60% in the outer regions of the nebula5. 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.",
author = "Fei Xie and {Di Marco}, Alessandro and {La Monaca}, Fabio and Kuan Liu and Fabio Muleri and Niccol{\`o} Bucciantini and Romani, {Roger W.} and Enrico Costa and John Rankin and Paolo Soffitta and Matteo Bachetti and {Di Lalla}, Niccol{\`o} and Sergio Fabiani and Riccardo Ferrazzoli and Shuichi Gunji and Luca Latronico and Michela Negro and Nicola Omodei and Maura Pilia and Alessio Trois and Eri Watanabe and Iv{\'a}n Agudo and Antonelli, {Lucio A.} and Luca Baldini and Baumgartner, {Wayne H.} and Ronaldo Bellazzini and Stefano Bianchi and Bongiorno, {Stephen D.} and Raffaella Bonino and Alessandro Brez and Fiamma Capitanio and Simone Castellano and Elisabetta Cavazzuti and Stefano Ciprini and {De Rosa}, Alessandra and {Del Monte}, Ettore and {Di Gesu}, Laura and Immacolata Donnarumma and Victor Doroshenko and Michal Dov{\v c}iak and Ehlert, {Steven R.} and Teruaki Enoto and Yuri Evangelista and Garcia, {Javier A.} and Kiyoshi Hayashida and Jeremy Heyl and Wataru Iwakiri and Jorstad, {Svetlana G.} and Vladimir Karas and Takao Kitaguchi and Kolodziejczak, {Jeffery J.} and Henric Krawczynski and Ioannis Liodakis and Simone Maldera and Alberto Manfreda and Fr{\'e}d{\'e}ric Marin and Andrea Marinucci and Marscher, {Alan P.} and Marshall, {Herman L.} and Francesco Massaro and Giorgio Matt and Ikuyuki Mitsuishi and Tsunefumi Mizuno and C.-Y. Ng and O{\textquoteright}Dell, {Stephen L.} and Chiara Oppedisano and Alessandro Papitto and Pavlov, {George G.} and Peirson, {Abel L.} and Matteo Perri and Melissa Pesce-Rollins and Pierre-Olivier Petrucci and Andrea Possenti and Juri Poutanen and Simonetta Puccetti and Ramsey, {Brian D.} and Ajay Ratheesh and Carmelo Sgr{\'o} and Patrick Slane and Gloria Spandre and Toru Tamagawa and Fabrizio Tavecchio and Roberto Taverna and Yuzuru Tawara and Tennant, {Allyn F.} and Thomas, {Nicolas E.} and Francesco Tombesi and Tsygankov, {Sergey S.} and Roberto Turolla and Jacco Vink and Weisskopf, {Martin C.} and Kinwah Wu and Silvia Zane",
year = "2022",
doi = "10.1038/s41586-022-05476-5",
language = "русский",
volume = "612",
pages = "658--660",
journal = "Nature",
issn = "0028-0836",
publisher = "Nature Publishing Group",
number = "7941",
}
RIS
TY - JOUR
T1 - Vela pulsar wind nebula X-rays are polarized to near the synchrotron limit
AU - Xie, Fei
AU - Di Marco, Alessandro
AU - La Monaca, Fabio
AU - Liu, Kuan
AU - Muleri, Fabio
AU - Bucciantini, Niccolò
AU - Romani, Roger W.
AU - Costa, Enrico
AU - Rankin, John
AU - Soffitta, Paolo
AU - Bachetti, Matteo
AU - Di Lalla, Niccolò
AU - Fabiani, Sergio
AU - Ferrazzoli, Riccardo
AU - Gunji, Shuichi
AU - Latronico, Luca
AU - Negro, Michela
AU - Omodei, Nicola
AU - Pilia, Maura
AU - Trois, Alessio
AU - Watanabe, Eri
AU - Agudo, Iván
AU - Antonelli, Lucio A.
AU - Baldini, Luca
AU - Baumgartner, Wayne H.
AU - Bellazzini, Ronaldo
AU - Bianchi, Stefano
AU - Bongiorno, Stephen D.
AU - Bonino, Raffaella
AU - Brez, Alessandro
AU - Capitanio, Fiamma
AU - Castellano, Simone
AU - Cavazzuti, Elisabetta
AU - Ciprini, Stefano
AU - De Rosa, Alessandra
AU - Del Monte, Ettore
AU - Di Gesu, Laura
AU - Donnarumma, Immacolata
AU - Doroshenko, Victor
AU - Dovčiak, Michal
AU - Ehlert, Steven R.
AU - Enoto, Teruaki
AU - Evangelista, Yuri
AU - Garcia, Javier A.
AU - Hayashida, Kiyoshi
AU - Heyl, Jeremy
AU - Iwakiri, Wataru
AU - Jorstad, Svetlana G.
AU - Karas, Vladimir
AU - Kitaguchi, Takao
AU - Kolodziejczak, Jeffery J.
AU - Krawczynski, Henric
AU - Liodakis, Ioannis
AU - Maldera, Simone
AU - Manfreda, Alberto
AU - Marin, Frédéric
AU - Marinucci, Andrea
AU - Marscher, Alan P.
AU - Marshall, Herman L.
AU - Massaro, Francesco
AU - Matt, Giorgio
AU - Mitsuishi, Ikuyuki
AU - Mizuno, Tsunefumi
AU - Ng, C.-Y.
AU - O’Dell, Stephen L.
AU - Oppedisano, Chiara
AU - Papitto, Alessandro
AU - Pavlov, George G.
AU - Peirson, Abel L.
AU - Perri, Matteo
AU - Pesce-Rollins, Melissa
AU - Petrucci, Pierre-Olivier
AU - Possenti, Andrea
AU - Poutanen, Juri
AU - Puccetti, Simonetta
AU - Ramsey, Brian D.
AU - Ratheesh, Ajay
AU - Sgró, Carmelo
AU - Slane, Patrick
AU - Spandre, Gloria
AU - Tamagawa, Toru
AU - Tavecchio, Fabrizio
AU - Taverna, Roberto
AU - Tawara, Yuzuru
AU - Tennant, Allyn F.
AU - Thomas, Nicolas E.
AU - Tombesi, Francesco
AU - Tsygankov, Sergey S.
AU - Turolla, Roberto
AU - Vink, Jacco
AU - Weisskopf, Martin C.
AU - Wu, Kinwah
AU - Zane, Silvia
PY - 2022
Y1 - 2022
N2 - 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 remnant2. Previous X-ray observations revealed two prominent arcs that are bisected by a jet and counter jet3,4. Radio maps have shown high linear polarization of 60% in the outer regions of the nebula5. 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.
AB - 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 remnant2. Previous X-ray observations revealed two prominent arcs that are bisected by a jet and counter jet3,4. Radio maps have shown high linear polarization of 60% in the outer regions of the nebula5. 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.
U2 - 10.1038/s41586-022-05476-5
DO - 10.1038/s41586-022-05476-5
M3 - статья
VL - 612
SP - 658
EP - 660
JO - Nature
JF - Nature
SN - 0028-0836
IS - 7941
ER -
