Počet záznamů: 1
Prominence eruption observed in He II 304 angstrom up to > 6 R-circle dot by EUI/FSI aboard Solar Orbiter
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SYSNO ASEP 0558623 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Prominence eruption observed in He II 304 angstrom up to > 6 R-circle dot by EUI/FSI aboard Solar Orbiter Tvůrce(i) Mierla, M. (BE)
Zhukov, A. (BE)
Berghmans, D. (BE)
Heinzel, Petr (ASU-R) RID, ORCIDCelkový počet autorů 27 Číslo článku L5 Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 662, June (2022)Poč.str. 11 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova coronal mass ejections ; imaging telescope ; flux cancellation Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP GA22-34841S GA ČR - Grantová agentura ČR GA19-16890S GA ČR - Grantová agentura ČR Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 000811793500001 EID SCOPUS 85132449343 DOI 10.1051/0004-6361/202244020 Anotace We report observations of a unique, large prominence eruption that was observed in the He II 304 angstrom passband of the Extreme Ultraviolet Imager/Full Sun Imager telescope aboard Solar Orbiter on 15-16 February 2022. Observations from several vantage points - Solar Orbiter, the Solar-Terrestrial Relations Observatory, the Solar and Helio-spheric Observatory, and Earth-orbiting satellites - were used to measure the kinematics of the erupting prominence and the associated coronal mass ejection. Three-dimensional reconstruction was used to calculate the deprojected positions and speeds of different parts of the prominence. Observations in several passbands allowed us to analyse the radiative properties of the erupting prominence. The leading parts of the erupting prominence and the leading edge of the corresponding coronal mass ejection propagate at speeds of around 1700 km s(-1) and 2200 km s(-1), respectively, while the trailing parts of the prominence are significantly slower (around 500 km s(-1)). Parts of the prominence are tracked up to heights of over 6 R-circle dot. The He II emission is probably produced via collisional excitation rather than scattering. Surprisingly, the brightness of a trailing feature increases with height. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2023 Elektronická adresa https://hdl.handle.net/11104/0332729
Počet záznamů: 1