Response of optical hydrogen lines to beam heating: I. Electron beams

Details Response of optical hydrogen lines to beam heating: I. Electron beams Response of optical hydrogen lines to beam heating: I. Electron beams

2009-04-14

arxiv.org/abs/0904.2084v1

Astron.Astrophys.499:923-934,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

13 pages, 11 figures, accepted to Astronomy and Astrophysics

Scientific paper

We investigate the role of non-thermal electrons in the formation regions of Halpha, Hbeta, and Hgamma lines in order to unfold their influence on the formation of these lines. We concentrate on pulse-beam heating varying on a subsecond timescale. Furthermore, we theoretically explore possibility that a new diagnostic tool exists indicating the presence of non-thermal electrons in the flaring chromosphere based on observations of optical hydrogen lines. To model the evolution of the flaring atmosphere and the time-dependent hydrogen excitation and ionisation, we used a 1-D radiative hydrodynamic code combined with a test-particle code that simulates the propagation, scattering, and thermalisation of a power-law electron beam in order to obtain the flare heating and the non-thermal collisional rates due to the interaction of the beam with the hydrogen atoms. All calculated models have shown a time-correlated response of the modelled Balmer line intensities on a subsecond timescale, with a subsecond timelag behind the beam flux. Depending on the beam parameters, both line centres and wings can show pronounced intensity variations. The non-thermal collisional rates generally result in an increased emission from a secondary region formed in the chromosphere.

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