Observational study of chromospheric heating by acoustic waves

dc.bibliographicCitation.firstPageA52eng
dc.bibliographicCitation.journalTitleAstronomy and Astrophysicseng
dc.bibliographicCitation.volume642eng
dc.contributor.authorAbbasvand, V.
dc.contributor.authorSobotka, M.
dc.contributor.authorŠvanda, M.
dc.contributor.authorHeinzel, P.
dc.contributor.authorGarcía-Rivas, M.
dc.contributor.authorDenker, C.
dc.contributor.authorBalthasar, H.
dc.contributor.authorVerma, M.
dc.contributor.authorKontogiannis, I.
dc.contributor.authorKoza, J.
dc.contributor.authorKorda, D.
dc.contributor.authorKuckein, C.
dc.date.accessioned2021-07-20T07:49:01Z
dc.date.available2021-07-20T07:49:01Z
dc.date.issued2020
dc.description.abstractAims. Our aim is to investigate the role of acoustic and magneto-acoustic waves in heating the solar chromosphere. Observations in strong chromospheric lines are analyzed by comparing the deposited acoustic-energy flux with the total integrated radiative losses. Methods. Quiet-Sun and weak-plage regions were observed in the Ca ii 854.2 nm and H lines with the Fast Imaging Solar Spectrograph (FISS) at the 1.6-m Goode Solar Telescope on 2019 October 3 and in the H and H lines with the echelle spectrograph attached to the Vacuum Tower Telescope on 2018 December 11 and 2019 June 6. The deposited acoustic energy flux at frequencies up to 20 mHz was derived from Doppler velocities observed in line centers and wings. Radiative losses were computed by means of a set of scaled non-local thermodynamic equilibrium 1D hydrostatic semi-empirical models obtained by fitting synthetic to observed line profiles. Results. In the middle chromosphere (h = 1000–1400 km), the radiative losses can be fully balanced by the deposited acoustic energy flux in a quiet-Sun region. In the upper chromosphere (h > 1400 km), the deposited acoustic flux is small compared to the radiative losses in quiet as well as in plage regions. The crucial parameter determining the amount of deposited acoustic flux is the gas density at a given height. Conclusions. The acoustic energy flux is e ciently deposited in the middle chromosphere, where the density of gas is su ciently high. About 90% of the available acoustic energy flux in the quiet-Sun region is deposited in these layers, and thus it is a major contributor to the radiative losses of the middle chromosphere. In the upper chromosphere, the deposited acoustic flux is too low, so that other heating mechanisms have to act to balance the radiative cooling.eng
dc.description.versionpublishedVersioneng
dc.identifier.urihttps://oa.tib.eu/renate/handle/123456789/6282
dc.identifier.urihttps://doi.org/10.34657/5329
dc.language.isoengeng
dc.publisherLes Ulis : EDP Scienceseng
dc.relation.doihttps://doi.org/10.1051/0004-6361/202038559
dc.relation.essn1432-0746
dc.relation.issn0004-6361
dc.rights.licenseCC BY 4.0 Unportedeng
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/eng
dc.subject.ddc520eng
dc.subject.otherSun: chromosphereeng
dc.subject.otherSun: oscillationseng
dc.subject.otherradiative transfereng
dc.titleObservational study of chromospheric heating by acoustic waveseng
dc.typeArticleeng
dc.typeTexteng
tib.accessRightsopenAccesseng
wgl.contributorAIPeng
wgl.subjectPhysikeng
wgl.typeZeitschriftenartikeleng
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