A testable stochastic acceleration model for flares in sagittarius A*

Siming Liu, Vahé Petrosian, Fulvio Melia, Christopher L. Fryer

Research output: Contribution to journalArticle

29 Scopus citations

Abstract

The near-IR and X-ray flares in Sagittarius A* are believed to be produced by relativistic electrons via synchrotron and synchrotron self-Comptonization, respectively. These electrons are likely energized by turbulent plasma waves through second-order Fermi acceleration that, in combination with the radiative cooling processes, produces a relativistic Maxwellian distribution in the steady state. This model has four principal parameters, namely the magnetic field B, the electron density n and temperature γcmec2, and the size of the flare region R. In the context of stochastic acceleration, the quantities Rn1/2B and γcRn should remain nearly constant in time. Therefore, simultaneous spectroscopic observations in the NIR and X-ray bands can readily test the model, which, if proven to be valid, may be used to determine the evolution of the plasma properties during an eruptive event with spectroscopic observations in either band or simultaneous flux density measurements in both bands. The formulae can be applied to other isolated or confined systems, where electrons are accelerated to relativistic energies by plasma wave turbulence and produce most of the emission via synchrotron processes.

Original languageEnglish (US)
Pages (from-to)1020-1025
Number of pages6
JournalAstrophysical Journal
Volume648
Issue number2 I
DOIs
Publication statusPublished - Sep 10 2006

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Keywords

  • Acceleration of particles
  • Black hole physics
  • Galaxy: center
  • Plasmas
  • Radiation mechanisms: thermal
  • Turbulence

ASJC Scopus subject areas

  • Space and Planetary Science

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