English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Over three thousand pulsars have been discovered, but none have beenconfirmed to be younger than a few hundred years. Observing a pulsar after asupernova explosion will help us understand the properties of newborn ones,including their capability to produce gamma-ray bursts and fast radio bursts.Here, the possible youngest pulsar wind nebula (PWN) at the center of the SN1986J remnant is studied. We demonstrate that the 5 GHz flux of 'PWN 1986J',increasing with time, is consistent with a stochastic acceleration model ofPWNe developed to explain the flat radio spectrum of the Crab Nebula. We obtainan acceleration time-scale of electrons/positrons and a decay time-scale of theturbulence responsible for the stochastic acceleration as about 10 and 70years, respectively. Our findings suggest that efficient stochasticacceleration and rising radio/submm light curves are characteristic signaturesof the youngest PWNe. Follow-up ${\it ALMA}$ observations of decades-oldsupernovae within a few tens of Mpc, including SN 1986J, are encouraged toreveal the origin of the flat radio spectrum of PWNe.

Testing a stochastic acceleration model of pulsar wind nebulae: Early evolution of a wind nebula associated with SN 1986J