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dc.date.accessioned2017-08-15T11:32:00Z
dc.date.available2017-08-15T11:32:00Z
dc.date.created2014-08-19T12:10:29Z
dc.date.issued2014
dc.identifier.citationTian, H DeLuca, E. Reeves, K. K. McKillop, S. De Pontieu, Bart Walter Martinez-Sykora, Juan Carlsson, Mats Hansteen, Viggo Kleint, L. Cheung, M Golub, L. Saar, S. Testa, Paola Weber, M. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T.D. Wuelser, J. P. Kankelborg, C. Jaeggli, S. McIntosh, S.W. . HIGH-RESOLUTION OBSERVATIONS OF THE SHOCK WAVE BEHAVIOR FOR SUNSPOT OSCILLATIONS WITH THE INTERFACE REGION IMAGING SPECTROGRAPH. The Astrophysical Journal. 2014, 786(2)
dc.identifier.urihttp://hdl.handle.net/10852/57014
dc.description.abstractWe present the first results of sunspot oscillations from observations by the Interface Region Imaging Spectrograph. The strongly nonlinear oscillation is identified in both the slit-jaw images and the spectra of several emission lines formed in the transition region and chromosphere. We first apply a single Gaussian fit to the profiles of the Mg II 2796.35 Å, C II 1335.71 Å, and Si IV 1393.76 Å lines in the sunspot. The intensity change is ~30%. The Doppler shift oscillation reveals a sawtooth pattern with an amplitude of ~10 km s–1 in Si IV. The Si IV oscillation lags those of C II and Mg II by ~6 and ~25 s, respectively. The line width suddenly increases as the Doppler shift changes from redshift to blueshift. However, we demonstrate that this increase is caused by the superposition of two emission components. We then perform detailed analysis of the line profiles at a few selected locations on the slit. The temporal evolution of the line core is dominated by the following behavior: a rapid excursion to the blue side, accompanied by an intensity increase, followed by a linear decrease of the velocity to the red side. The maximum intensity slightly lags the maximum blueshift in Si IV, whereas the intensity enhancement slightly precedes the maximum blueshift in Mg II. We find a positive correlation between the maximum velocity and deceleration, a result that is consistent with numerical simulations of upward propagating magnetoacoustic shock waves. Reproduced with permission from the Astrophysical Journal. © IOP Publishingen_US
dc.languageEN
dc.publisherUniversity of Chicago Press
dc.titleHIGH-RESOLUTION OBSERVATIONS OF THE SHOCK WAVE BEHAVIOR FOR SUNSPOT OSCILLATIONS WITH THE INTERFACE REGION IMAGING SPECTROGRAPHen_US
dc.typeJournal articleen_US
dc.creator.authorTian, H
dc.creator.authorDeLuca, E.
dc.creator.authorReeves, K. K.
dc.creator.authorMcKillop, S.
dc.creator.authorDe Pontieu, Bart Walter
dc.creator.authorMartinez-Sykora, Juan
dc.creator.authorCarlsson, Mats
dc.creator.authorHansteen, Viggo
dc.creator.authorKleint, L.
dc.creator.authorCheung, M
dc.creator.authorGolub, L.
dc.creator.authorSaar, S.
dc.creator.authorTesta, Paola
dc.creator.authorWeber, M.
dc.creator.authorLemen, J.
dc.creator.authorTitle, A.
dc.creator.authorBoerner, P.
dc.creator.authorHurlburt, N.
dc.creator.authorTarbell, T.D.
dc.creator.authorWuelser, J. P.
dc.creator.authorKankelborg, C.
dc.creator.authorJaeggli, S.
dc.creator.authorMcIntosh, S.W.
cristin.unitcode185,15,3,0
cristin.unitnameInstitutt for teoretisk astrofysikk
cristin.ispublishedtrue
cristin.fulltextoriginal
cristin.qualitycode2
dc.identifier.cristin1147786
dc.identifier.bibliographiccitationinfo:ofi/fmt:kev:mtx:ctx&ctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=The Astrophysical Journal&rft.volume=786&rft.spage=&rft.date=2014
dc.identifier.jtitleThe Astrophysical Journal
dc.identifier.volume786
dc.identifier.issue2
dc.identifier.pagecount9
dc.identifier.doihttp://dx.doi.org/10.1088/0004-637X/786/2/137
dc.identifier.urnURN:NBN:no-59752
dc.type.documentTidsskriftartikkelen_US
dc.type.peerreviewedPeer reviewed
dc.source.issn0004-637X
dc.identifier.fulltextFulltext https://www.duo.uio.no/bitstream/handle/10852/57014/1/Tian_2014_ApJ_786_137.pdf
dc.type.versionPublishedVersion
cristin.articleid137


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