Nonthermal electrons in radiatively inefficient accretion flow models of sagittarius A

Feng Yuan, Eliot Quataert, Ramesh Narayan

Research output: Contribution to journalArticlepeer-review

503 Scopus citations

Abstract

We investigate radiatively inefficient accretion flow models for Sgr A*, the supermassive black hole in our Galactic center, in light of new observational constraints. Confirmation of linear polarization in the submillimeter emission argues for accretion rates much less than the canonical Bondi rate. We consider models with low accretion rates and calculate the spectra produced by a hybrid electron population consisting of both thermal and nonthermal particles. The thermal electrons produce the submillimeter emission and can account for its linear polarization properties. As noted in previous work, the observed low-frequency radio spectrum can be explained if a small fraction (≡ 1.5%) of the electron thermal energy resides in a soft power-law tail. In the innermost region of the accretion flow, turbulence and/ or magnetic reconnection events may occasionally accelerate a fraction of the electrons into a harder power-law tail. We show that the synchrotron emission from these electrons, or the Compton upscattering of synchrotron photons by the same electrons, may account for the X-ray flares observed by Chandra.

Original languageEnglish (US)
Pages (from-to)301-312
Number of pages12
JournalAstrophysical Journal
Volume598
Issue number1 I
DOIs
StatePublished - Nov 20 2003
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Accretion,Accretion disks
  • Black hole physics
  • Galaxies: active
  • Galaxy: center
  • Radiation mechanisms: nonthermal
  • Radiation mechanisms: thermal

Fingerprint

Dive into the research topics of 'Nonthermal electrons in radiatively inefficient accretion flow models of sagittarius A'. Together they form a unique fingerprint.

Cite this