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

An extended  XMM–Newton  observation of the Seyfert 1 galaxy NGC 4051 in 2009 revealed a complex absorption spectrum, with a wide range of outflow velocities and ionization states. The main velocity and ionization structure was interpreted in Paper I in terms of a decelerating, recombining flow resulting from the shocking of a still higher velocity wind colliding with the interstellar medium or slower moving ejecta. The high sensitivity of the  XMM–Newton  observation also revealed a number of broad emission lines, all showing evidence of self‐absorption near the line cores. The line profiles are found here to be consistent with emission from a limb‐brightened shell of post‐shock gas building up ahead of the contact discontinuity. While the broad emission lines remain quasi‐constant as the continuum flux changes by an order of magnitude, recombination continua of several H‐ and He‐like ions are found to vary in response to the continuum, providing an important key to scaling the ionized flow.

An extended XMM–Newton observation of the Seyfert galaxy NGC 4051 – II. Soft X‐ray emission from a limb‐brightened shell of post‐shock gas