Abstract
The possibility that large-scale coronal loops of solar-type stars and M dwarfs make a significant contribution to the white-light continuum emission is considered. It is shown that that the existence of high-density (>1012 cm–3) coronal loops contradicts the standard model of solar and stellar flares. As a result, the optical flare emission cannot be determined by free–free or free–bound processes within loops. The contribution from the lower atmosphere, which is heated beneath the loops due to the irradiation of soft X-ray emission, should be also negligible. The possible alternative scenarios are discussed.
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