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

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00604621" target="_blank" >RIV/67985815:_____/22:00604621 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1038/s41586-022-05476-5" target="_blank" >https://doi.org/10.1038/s41586-022-05476-5</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1038/s41586-022-05476-5" target="_blank" >10.1038/s41586-022-05476-5</a>

Jazyk výsledku

angličtina

Název v původním jazyce

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

Popis výsledku v původním jazyce

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 11,000years)(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.

Název v anglickém jazyce

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

Popis výsledku anglicky

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 11,000years)(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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Nature

ISSN

0028-0836

e-ISSN

1476-4687

Svazek periodika

612

Číslo periodika v rámci svazku

7941

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

3

Strana od-do

658-660

Kód UT WoS článku

000934065100014

EID výsledku v databázi Scopus

2-s2.0-85144598053