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LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00004602naa a2200553 4500
001oai:DiVA.org:su-228269
003SwePub
008240411s2024 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-2282692 URI
0247 a https://doi.org/10.1051/0004-6361/2023478952 DOI
040 a (SwePub)su
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Pietrow, A. G. M.4 aut
2451 0a A comparative study of two X2.2 and X9.3 solar flares observed with HARPS-N :b Reconciling Sun-as-a-star spectroscopy and high-spatial resolution solar observations in the context of the solar-stellar connection
264 1c 2024
338 a print2 rdacarrier
520 a Context. Stellar flares cannot be spatially resolved, which complicates ascertaining the physical processes behind particular spectral signatures. Due to their proximity to Earth, solar flares can serve as a stepping stone for understanding their stellar counterparts, especially when using a Sun-as-a-star instrument and in combination with spatially resolved observations.Aims. We aim to understand the disk-integrated spectral behaviors of a confined X2.2 flare and its eruptive X9.3 successor, which had energies of 2.2 × 1031 erg and 9.3 × 1031 erg, respectively, as measured by Sun-as-a-star observations with the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N).Methods. The behavior of multiple photospheric (Na D1 & D2, Mg I at 5173 Å, Fe I at 6173 Å, and Mn I at 4031 Å) and chromospheric (Ca II H & K, Hα, Hβ, and He ID3) spectral lines were investigated by means of activity indices and contrast profiles. A number of different photospheric lines were also investigated by means of equivalent widths, and radial velocity measures, which were then related to physical processes directly observed in high-resolution observations made with the Swedish 1-m Solar Telescope (SST) and the Atmospheric Imaging Assembly (AIA) on board of the Solar Dynamics Observatory (SDO).Results. Our findings suggest a relationship between the evolving shapes of contrast profile time and the flare locations, which assists in constraining flare locations in disk-integrated observations. In addition, an upward bias was found in flare statistics based on activity indices derived from the Ca II H & K lines. In this case, much smaller flares cause a similar increase in the activity index as that produced by larger flares. Hα-based activity indices do not show this bias and are therefore less susceptible to activity jitter. Sodium line profiles show a strongly asymmetric response during flare activity, which is best captured with a newly defined asymmetrical sodium activity index. A strong flare response was detected in Mn I line profiles, which is unexpected and calls for further exploration. Intensity increases in Hα, Hβ, and certain spectral windows of AIA before the flare onset suggest their potential use as short-term flare predictors.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653 a Sun: flares
653 a methods: observational
653 a stars: flare
653 a techniques: spectroscopic
653 a sunspots
653 a line: formation
7001 a Cretignier, M.4 aut
7001 a Druett, M. K.4 aut
7001 a Alvarado-Gómez, J. D.4 aut
7001 a Hofmeister, S. J.4 aut
7001 a Verma, M.4 aut
7001 a Kamlah, R.4 aut
7001 a Baratella, M.4 aut
7001 a Amazo-Gómez, E. M.4 aut
7001 a Kontogiannis, I.4 aut
7001 a Dineva, E.4 aut
7001 a Warmuth, A.4 aut
7001 a Denker, C.4 aut
7001 a Poppenhaeger, K.4 aut
7001 a Andriienko, Oleksii,d 1972-u Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)olad6860
7001 a Dumusque, X.4 aut
7001 a Löfdahl, Mats G.,d 1961-u Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)lofda
7102 a Stockholms universitetb Institutionen för astronomi4 org
7730 t Astronomy and Astrophysicsg 682q 682x 0004-6361x 1432-0746
8564 u https://doi.org/10.1051/0004-6361/202347895y Fulltext
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-228269
8564 8u https://doi.org/10.1051/0004-6361/202347895

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