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Suppression of Hydrogen Emission in an X-class White-light Solar Flare
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SYSNO ASEP 0479466 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Suppression of Hydrogen Emission in an X-class White-light Solar Flare Author(s) Procházka, O. (GB)
Milligan, R.O. (GB)
Allred, J.C. (US)
Kowalski, A.F. (US)
Kotrč, Pavel (ASU-R) RID, ORCID
Mathioudakis, M. (GB)Source Title Astrophysical Journal - ISSN 0004-637X
Roč. 837, č. 1 (2017), 46/1-46/9Number of pages 9 s. Publication form Print - P Language eng - English Country US - United States Keywords Sun ; atmosphere ; flares Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA16-18495S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000395918600011 EID SCOPUS 85015163014 DOI 10.3847/1538-4357/aa5da8 Annotation We present unique NUV observations of a well-observed X-class flare from NOAA 12087 obtained at the Ondrejov Observatory. The flare shows a strong white-light continuum but no detectable emission in the higher Balmer and Lyman lines. Reuven Ramaty High-Energy Solar Spectroscopic Imager and Fermi observations indicate an extremely hard X-ray spectrum and gamma-ray emission. We use the RADYN radiative hydrodynamic code to perform two types of simulations: one where an energy of 3 x 10(11) erg cm(-2) s(-1) is deposited by an electron beam with a spectral index of approximate to 3, and a second where the same energy is applied directly to the photosphere. The combination of observations and simulations allows us to conclude that the white-light emission and the suppression or complete lack of hydrogen emission lines is best explained by a model where the dominant energy deposition layer is located in the lower layers of the solar atmosphere, rather than the chromosphere. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2018
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