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dc.contributor.authorGošić, M.-
dc.contributor.authorde la Cruz Rodríguez, J.-
dc.contributor.authorDe Pontieu, B.-
dc.contributor.authorBellot Rubio, Luis R.-
dc.contributor.authorCarlsson, M.-
dc.contributor.authorEsteban Pozuelo, S.-
dc.contributor.authorOrtiz, A.-
dc.contributor.authorPolito, V.-
dc.date.accessioned2020-06-09T05:51:44Z-
dc.date.available2020-06-09T05:51:44Z-
dc.date.issued2018-
dc.identifierdoi: 10.3847/1538-4357/aab1f0-
dc.identifierissn: 1538-4357-
dc.identifier.citationAstrophysical Journal 857(1): 48 (2018)-
dc.identifier.urihttp://hdl.handle.net/10261/213803-
dc.description.abstractThe heating of the solar chromosphere remains one of the most important questions in solar physics. Our current understanding is that small-scale internetwork (IN) magnetic fields play an important role as a heating agent. Indeed, cancellations of IN magnetic elements in the photosphere can produce transient brightenings in the chromosphere and transition region. These bright structures might be the signature of energy release and plasma heating, probably driven by the magnetic reconnection of IN field lines. Although single events are not expected to release large amounts of energy, their global contribution to the chromosphere may be significant due to their ubiquitous presence in quiet Sun regions. In this paper, we study cancellations of IN elements and analyze their impact on the energetics and dynamics of the quiet Sun atmosphere. We use high-resolution, multiwavelength, coordinated observations obtained with the Interface Region Imaging Spectrograph and the Swedish 1 m Solar Telescope (SST) to identify cancellations of IN magnetic flux patches and follow their evolution. We find that, on average, these events live for ∼3 minutes in the photosphere and ∼12 minutes in the chromosphere and/or transition region. Employing multi-line inversions of the Mg ii h and k lines, we show that cancellations produce clear signatures of heating in the upper atmospheric layers. However, at the resolution and sensitivity accessible to the SST, their number density still seems to be one order of magnitude too low to explain the global chromospheric heating.© 2018. The American Astronomical Society. All rights reserved.-
dc.description.sponsorshipRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. M.G. was supported by NASA grant NNX16AC34G. J.dl.C.R. is supported by grants from the Swedish Research Council (2015-03994), the Swedish National Space Board (128/15), and the Swedish Civil Contingencies Agency (MSB). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (SUNMAG, grant agreement 759548). B.D.P. was supported by NASA grant NNX11AN98G and NASA contracts NNG09FA40C (IRIS). The work of L.B.R. and S.E.P. was supported by the Spanish Ministerio de Economia and Competitividad through grants ESP2013-47349-C6-1-R and ESP2016-77548-C5-1-R, including a percentage from European FEDER funds. Image reconstruction was performed at IAA-CSIC supercomputing facilities. The Swedish 1 m Solar Telescope is operated by the Institute for Solar Physics of Stockholm University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. M.C. was supported by the Research Council of Norway through its Centres of Excellence scheme, project number 262622, and through grants of computing time from the Programme for Supercomputing. This research has made use of NASA's Astrophysics Data System.-
dc.languageeng-
dc.publisherIOP Publishing-
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/759548-
dc.relationMINECO/ICTI2013-2016/ESP2013-47349-C6-1-R-
dc.relationMINECO/ICTI2013-2016/ESP2016-77548-C5-1-R-
dc.relation.isversionofPostprint-
dc.rightsopenAccess-
dc.subjectSun: atmosphere-
dc.subjectSun: chromosphere-
dc.subjectSun: magnetic fields-
dc.subjectSun: transition region-
dc.titleChromospheric Heating due to Cancellation of Quiet Sun Internetwork Fields-
dc.typeartículo-
dc.relation.publisherversionhttp://dx.doi.org/10.3847/1538-4357/aab1f0-
dc.date.updated2020-06-09T05:51:44Z-
dc.contributor.funderEuropean Southern Observatory-
dc.contributor.funderNorwegian Space Agency-
dc.contributor.funderNational Aeronautics and Space Administration (US)-
dc.contributor.funderSwedish Research Council-
dc.contributor.funderSwedish National Space Board-
dc.contributor.funderSwedish Civil Contingencies Agency-
dc.contributor.funderEuropean Research Council-
dc.contributor.funderMinisterio de Economía y Competitividad (España)-
dc.contributor.funderEuropean Commission-
dc.contributor.funderResearch Council of Norway-
dc.relation.csic-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100004604es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100001859es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003329es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
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