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

M87 is arguably the best supermassive black hole (BH) to explore the jetand/or accretion physics due to its proximity and fruitful high-resolutionmulti-waveband observations. We model the multi-wavelength spectral energydistribution (SED) of M87 core that observed at a scale of 0.4 arcsec ($\sim10^5R_{\rm g}$, $R_{\rm g}$ is gravitational radius) as recently presented byPrieto et al. Similar to Sgr A*, we find that the millimeter bump as observedby Atacama Large Millimeter/submillimeter Array (ALMA) can be modeled by thesynchrotron emission of the thermal electrons in advection dominated accretionflow (ADAF), while the low-frequency radio emission and X-ray emission maydominantly come from the jet. The millimeter radiation from ADAF dominantlycome from the region within $10R_{\rm g}$, which is roughly consistent with therecent very long baseline interferometry observations at 230\,GHz. We furthercalculate the Faraday rotation measure (RM) from both ADAF and jet models, andfind that the RM predicted from the ADAF is roughly consistent with themeasured value while the RM predicted from the jet is much higher if jetvelocity close to the BH is low or moderate (e.g., $v_{\rmjet}\lesssim0.6\,c$). With the constraints from the SED modeling and RM, wefind that the accretion rate close to the BH horizon is $\sim(0.2-1)\times10^{-3}{M}_{\odot} \rm yr^{-1}\ll\dot{\it M}_{\rm B}\sim 0.2\it{M}_{\odot} \rm yr^{-1}$ ($\dot{M}_{\rm B}$ is Bondi accretion rate), where theelectron density profile, $n_{\rm e}\propto r^{\sim -1}$, in the accretion flowis consistent with that determined from X-ray observation inside the Bondiradius and recent numerical simulations.

An accretion-jet model for M87: interpreting the spectral energy distribution and Faraday rotation measure