White-Light Continuum in Stellar Flares
arXiv:1511.05085 · doi:10.1017/S1743921316000028
Abstract
In this talk, we discuss the formation of the near-ultraviolet and optical continuum emission in M dwarf flares through the formation of a dense, heated chromospheric condensation. Results are used from a recent radiative-hydrodynamic model of the response of an M dwarf atmosphere to a high energy flux of nonthermal electrons. These models are used to infer the charge density and optical depth in continuum emitting flare layers from spectra covering the Balmer jump and optical wavelength regimes. Future modeling and observational directions are discussed.
9 pages, 2 figures. Invited review talk submitted to the proceedings of the IAU Symposium 320 "Solar and Stellar Flares and Their Effects on Planets" (eds. A. G. Kosovichev, S. L. Hawley, P. Heinzel) held on 10-14 August, 2015, in Honolulu, USA
References in corpus (7)
- Impulsive phase flare energy transport by large-scale Alfven waves and the electron acceleration problem
- A Unified Computational Model for Solar and Stellar Flares
- Statistical properties of superflares on solar-type stars based on 1-min cadence data
- A White Light Megaflare on the dM4.5e Star YZ CMi
- Temporal evolution of multiple evaporating ribbon sources in a solar flare
- Radiative Hydrodynamic Models of Optical and Ultraviolet Emission from M Dwarf Flares
- The Radiated Energy Budget of Chromospheric Plasma in a Major Solar Flare Deduced From Multi-Wavelength Observations