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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

The extended X-ray emission observed at arcsec scales along the propagationtrajectory of the precessing relativistic jets of the Galactic microquasar SS433 features a broad emission line, with the position of the centroid beingsignificantly different for the approaching and receding jets ($ \approx7.3 $and $ \approx6.4 $ keV, respectively). These observed line positions are atodds with the predictions of the kinematic model for any of the plausiblebright spectral lines in this band, raising the question of theiridentification. Here we address this issue by taking into account time delaysof the emission coming from the receding regions of the jets relative to thatfrom the approaching ones, which cause a substantial phase shift and distortionof the predicted line positions for the extended ($ \sim 10^{17}$ cm) emissioncompared to the X-ray and optical lines observed from the central source(emitted at distances $ \sim 10^{11}$ cm and $ \sim 10^{15}$ cm, respectively).We demonstrate that the observed line positions are fully consistent with theFe XXVI Ly$\alpha$ ($E_0=6.96$ keV) line emerging from a region of size $\sim6\times10^{16}$ cm along the jet. This supports the idea that intensivereheating of the jets up to temperatures $ \gtrsim10 $ keV takes place at thesedistances, probably as a result of partial deceleration of the jets due tointeraction with the surrounding medium, which might cause collisions betweendiscrete dense blobs inside the jets.

Identification of X-ray lines in the spectrum of the arcsec-scale precessing jets of SS 433