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

We discuss the interpretation of transient, unpulsed radio emission detectedfrom the unique pulsar/Be-star binary system PSR B1259-63. Extensive monitoringof the 1994 and 1997 periastron passages has shown that the source flares overa 100-day interval around periastron, varying on time-scales as short as a dayand peaking at 60 mJy (~100 times the apastron flux density) at 1.4 GHz.Interpreting the emission as synchrotron radiation, we show that (i) theobserved variations in flux density are too large to be caused by the shockinteraction between the pulsar wind and an isotropic, radiatively driven,Be-star wind, and (ii) the radio emitting electrons do not originate from thepulsar wind. We argue instead that the radio electrons originate from thecircumstellar disk of the Be star and are accelerated at two epochs, one beforeand one after periastron, when the pulsar passes through the disk. A simplemodel incorporating two epochs of impulsive acceleration followed bysynchrotron cooling reproduces the essential features of the radio light curveand spectrum and is consistent with the system geometry inferred from pulsedradio data.Comment: To be published in Astrophysical Journal Letters 7 pages, 1  postscript figur

Origin of the Transient, Unpulsed Radio Emission from the PSR B1259−63 Binary System