Abstract
Joule dissipation due to the dynamo action in the solar atmosphere is proposed as a possible mechanism for heating the photosphere and chromosphere. In nonactive regions, Joule heating is distributed in both photosphere and chromosphere. The power density (ergs cm−3 s−1) produced by the Joule dissipation in the nonactive photosphere‐chromosphere regions is calculated based on a model under the average quiet Sun condition (Vernazza et al., 1981). The calculated Joule dissipation under quiet conditions exhibits a double‐peak profile within the chromosphere; one is associated with the electron dissipation at lower altitude, while the other is due to the ion dissipation at higher altitude. The energy flux produced by the Joule dissipation can be calculated by integrating the Joule power density over the height of the dissipation region. The resulting energy flux produced by the Joule dissipation in nonactive photosphere‐chromosphere regions is ∼2.4 × 107 ergs cm−2 s−1 which is more than 40 times the energy flux carried away by the high‐speed solar wind streams originating in the coronal holes. In active regions the Joule heating is predicted to be confined to the photosphere and is more than 2 orders of magnitude greater than in nonactive regions.
Published Version
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