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Nonthermal Electrons in Radiatively Inefficient Accretion Flow Models of Sagittarius A*

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Yuan, Feng, Quataert, Eliot, Narayan, Ramesh·2003·The Astrophysical Journal

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 .

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Metadata

Authors
Yuan, F., Quataert, E., & Narayan, R.
Venue
The Astrophysical Journal
Published
2003-11-20
Volume
598
Issue
1
Pages
301-312
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2006900906
Cited by
708
References
57
FWCI
16.62
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: Nonthermal Electrons in Radiatively Inefficient Accretion Flow Models of Sagittarius A*. https://app.cochat.ai/papers/10.1086/378716
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Yuan, F., Quataert, E., & Narayan, R. (2003). Nonthermal Electrons in Radiatively Inefficient Accretion Flow Models of Sagittarius A*. The Astrophysical Journal. https://doi.org/10.1086/378716

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