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

Aims. Hot accretion flows are thought to be able to power the relativisticjets observed in Active Galactic Nuclei. They can present themselves as SANE(Standard And Normal Evolution) disks or MAD (Magnetically Arrested Disks), twostates implying profound differences in the physical properties of the disksthemselves and of the outflows they produce. Methods. In this paper we use amulti-frequency and multi-epoch data set to study the giant radio galaxy NGC315, with the goal to explore the properties of its accretion disk andsub-parsec jet. We analyze the source maps with a pixel-based analysis and weuse theoretical models to link the observational properties of the jet to thephysical state of the accretion disk. Results. We propose that the bulk flow inNGC 315 accelerates on sub-pc scales, concurrently with the parabolicexpansion. We show that this fast acceleration can be theoretically reconciledwith a magnetically driven acceleration. Along the acceleration and collimationzone, we observe an unexpected spectral behavior, with very steep spectralindex values $\alpha \sim -1.5$ ($S_\nu \propto \nu^\alpha$) between 22 GHz and43 GHz. Based on the properties of this region, we predict the black hole ofNGC 315 to be fast rotating and the magnetic flux threading the accretion diskto be in excellent agreement with that expected in the case of a MAD. Using anew formalism based on the core-shift effect, we model the magnetic fielddownstream a quasi-parabolic accelerating jet and we reconstruct it up to theevent horizon radius. In the MAD scenario, we compare it with the expectedmagnetic saturation strengths in the disk, finding a good agreement.

Exploring the disk-jet connection in NGC 315