New solar extreme-ultraviolet irradiance observations during flares

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dc.contributorVirginia Techen
dc.contributor.authorWoods, T. N.en
dc.contributor.authorHock, R.en
dc.contributor.authorEparvier, F. G.en
dc.contributor.authorJones, A. R.en
dc.contributor.authorChamberlin, P. C.en
dc.contributor.authorKlimchuk, J. A.en
dc.contributor.authorDidkovsky, L.en
dc.contributor.authorJudge, D.en
dc.contributor.authorMariska, J.en
dc.contributor.authorWarren, H.en
dc.contributor.authorSchrijver, C. J.en
dc.contributor.authorWebb, D. F.en
dc.contributor.authorBailey, S.en
dc.contributor.authorTobiska, W. K.en
dc.contributor.departmentElectrical and Computer Engineeringen
dc.date.accessed2014-02-05en
dc.date.accessioned2014-02-25T13:57:06Zen
dc.date.available2014-02-25T13:57:06Zen
dc.date.issued2011-10-01en
dc.description.abstractNew solar extreme-ultraviolet (EUV) irradiance observations from the NASA Solar Dynamics Observatory (SDO) EUV Variability Experiment provide full coverage in the EUV range from 0.1 to 106 nm and continuously at a cadence of 10 s for spectra at 0.1 nm resolution and even faster, 0.25 s, for six EUV bands. These observations can be decomposed into four distinct characteristics during flares. First, the emissions that dominate during the flare's impulsive phase are the transition region emissions, such as the He II 30.4 nm. Second, the hot coronal emissions above 5 MK dominate during the gradual phase and are highly correlated with the GOES X-ray. A third flare characteristic in the EUV is coronal dimming, seen best in the cool corona, such as the Fe IX 17.1 nm. As the post-flare loops reconnect and cool, many of the EUV coronal emissions peak a few minutes after the GOES X-ray peak. One interesting variation of the post-eruptive loop reconnection is that warm coronal emissions (e. g., Fe XVI 33.5 nm) sometimes exhibit a second large peak separated from the primary flare event by many minutes to hours, with EUV emission originating not from the original flare site and its immediate vicinity, but rather from a volume of higher loops. We refer to this second peak as the EUV late phase. The characterization of many flares during the SDO mission is provided, including quantification of the spectral irradiance from the EUV late phase that cannot be inferred from GOES X-ray diagnostics.en
dc.description.sponsorshipNASAen
dc.format.mimetypeapplication/pdfen
dc.identifier.citationThomas N. Woods et al. 2011. "new solar extreme-ultraviolet irradiance observations during flares," ApJ 739 59 doi:10.1088/0004-637X/739/2/59en
dc.identifier.doihttps://doi.org/10.1088/0004-637x/739/2/59en
dc.identifier.issn0004-637Xen
dc.identifier.urihttp://hdl.handle.net/10919/25559en
dc.identifier.urlhttp://iopscience.iop.org/0004-637X/739/2/59/pdf/0004-637X_739_2_59.pdfen
dc.language.isoenen
dc.publisherIOP Publishingen
dc.rightsIn Copyrighten
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/en
dc.subjectSun--Coronaen
dc.subjectSun--Flaresen
dc.subjectSun: transition regionen
dc.subjectUV radiationen
dc.subjectCoronal mass ejectionsen
dc.subjectX-raysen
dc.subjectModelen
dc.subjectEUVen
dc.subjectDisturbancesen
dc.subjectEmissionsen
dc.subjectRhessien
dc.titleNew solar extreme-ultraviolet irradiance observations during flaresen
dc.title.serialAstrophysical Journalen
dc.typeArticle - Refereeden
dc.type.dcmitypeTexten

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