Počet záznamů: 1
High-density Off-limb Flare Loops Observed by SDO
- 1.
SYSNO ASEP 0497539 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název High-density Off-limb Flare Loops Observed by SDO Tvůrce(i) Jejčič, Sonja (ASU-R)
Kleint, L. (CH)
Heinzel, Petr (ASU-R) RID, ORCIDČíslo článku 134 Zdroj.dok. Astrophysical Journal - ISSN 0004-637X
Roč. 867, č. 2 (2018)Poč.str. 10 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. US - Spojené státy americké Klíč. slova Sun ; flares ; radio radiation Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP GA16-18495S GA ČR - Grantová agentura ČR GA16-16861S GA ČR - Grantová agentura ČR Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 000450221700001 EID SCOPUS 85056699532 DOI 10.3847/1538-4357/aae650 Anotace On 2017 September 10, a prominent loop system appeared during the gradual phase of an X8.2 flare (SOL2017-09-10), visible in all passbands of SDO/AIA and in the white-light continuum of SDO/HMI. We investigate its electron density by taking into account all radiation processes in the flare loops, i.e., the Thomson continuum, hydrogen Paschen and Brackett recombination continua, as well as free–free continuum emission. We derive a quadratic function of the electron density for a given temperature and effective loop thickness. By absolutely calibrating SDO/HMI intensities, we convert the measured intensities into electron density at each pixel in the loops. For a grid of plausible temperatures between cool (6000 K) and hot (106 K) structures, the electron density is computed for representative effective thicknesses between 200 and 20,000 km. We obtain a relatively high maximum electron density, about 1013 cm‑3. At such high electron densities, the Thomson continuum is negligible and therefore one would not expect a significant polarization degree in dense loops. We conclude that the Paschen and Brackett recombination continua are dominant in cool flare loops, while the free–free continuum emission is dominant for warmer and hot loops. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2019 Elektronická adresa http://hdl.handle.net/11104/0290095
Počet záznamů: 1