Probing the Density Fine Structuring of the Solar Corona with Comet Lovejoy

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dc.contributor.authorNistic, Giuseppecs
dc.contributor.authorZimbardo, Gaetanocs
dc.contributor.authorPerri, Silviacs
dc.contributor.authorNakariakov, Valery M.cs
dc.contributor.authorDuckenfield, Timothy j.cs
dc.contributor.authorDruckmüller, Miloslavcs
dc.coverage.issue1cs
dc.coverage.volume938cs
dc.date.issued2022-10-01cs
dc.description.abstractThe passage of sungrazing comets in the solar corona can be a powerful tool to probe the local plasma properties. Here, we carry out a study of the striae pattern appearing in the tail of sungrazing Comet Lovejoy, as observed by the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) during the inbound and outbound phases of the comet's orbit. We consider the images in EUV in the 171 angstrom bandpass, where emission from oxygen ions O4+ and O5+ is found. The striae are described as due to a beam of ions injected along the local magnetic field, with the initial beam velocity decaying because of collisions. Also, ion collisional diffusion contributes to ion propagation. Both the collision time for velocity decay and the diffusion coefficient for spatial spreading depend on the ambient plasma density. A probabilistic description of the ion beam density along the magnetic field is developed, where the beam position is given by the velocity decay and the spreading of diffusing ions is described by a Gaussian probability distribution. Profiles of emission intensity along the magnetic field are computed and compared with the profiles along the striae observed by AIA, showing a good agreement for most considered striae. The inferred coronal densities are then compared with a hydrostatic model of the solar corona. The results confirm that the coronal density is strongly spatially structured.en
dc.formattextcs
dc.format.extent20-20cs
dc.format.mimetypeapplication/pdfcs
dc.identifier.citationASTROPHYSICAL JOURNAL. 2022, vol. 938, issue 1, p. 20-20.en
dc.identifier.doi10.3847/1538-4357/ac8e62cs
dc.identifier.issn0004-637Xcs
dc.identifier.orcid0000-0001-7312-2410cs
dc.identifier.other179798cs
dc.identifier.researcheridABA-8307-2020cs
dc.identifier.scopus55814447000cs
dc.identifier.urihttp://hdl.handle.net/11012/208672
dc.language.isoencs
dc.publisherIOP Publishingcs
dc.relation.ispartofASTROPHYSICAL JOURNALcs
dc.relation.urihttps://iopscience.iop.org/article/10.3847/1538-4357/ac8e62cs
dc.rightsCreative Commons Attribution 4.0 Internationalcs
dc.rights.accessopenAccesscs
dc.rights.sherpahttp://www.sherpa.ac.uk/romeo/issn/0004-637X/cs
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/cs
dc.subjectcometen
dc.subjectsolar coronaen
dc.subjectextreme ultravioleten
dc.titleProbing the Density Fine Structuring of the Solar Corona with Comet Lovejoyen
dc.type.driverarticleen
dc.type.statusPeer-revieweden
dc.type.versionpublishedVersionen
sync.item.dbidVAV-179798en
sync.item.dbtypeVAVen
sync.item.insts2024.03.01 18:46:16en
sync.item.modts2024.03.01 18:14:10en
thesis.grantorVysoké učení technické v Brně. Fakulta strojního inženýrství. Ústav matematikycs
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