The Characteristics of Solar X-Class Flares and CMEs: A Paradigm for Stellar Superflares and Eruptions?

被引：74

作者：

Harra, Louise K. ^{[1
]}

Schrijver, Carolus J. ^{[2
]}

Janvier, Miho ^{[3
]}

Toriumi, Shin ^{[4
]}

Hudson, Hugh ^{[5
]}

Matthews, Sarah ^{[1
]}

Woods, Magnus M. ^{[1
]}

Hara, Hirohisa ^{[4
]}

Guedel, Manuel ^{[6
]}

Kowalski, Adam ^{[7
]}

Osten, Rachel ^{[8
]}

Kusano, Kanya ^{[9
]}

Lueftinger, Theresa ^{[6
]}

机构：

[1] UCL Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[2] Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St, Palo Alto, CA 94304 USA

[3] Univ Paris Saclay, Univ Paris Sud, Inst Astrophys Spatiale, UMR8617,CNRS, Batiment 121, F-91405 Orsay, France

[4] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[5] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow, Lanark, Scotland

[6] Univ Vienna, Dept Astrophys, Turkenschanzst 17, A-1180 Vienna, Austria

[7] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[8] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[9] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan

来源：

SOLAR PHYSICS | 2016年 / 291卷 / 06期

关键词：

Corona; Flares; dynamics; magnetic fields; CORONAL MASS EJECTIONS; MAGNETICALLY ACTIVE STARS; CHROMOSPHERIC EVAPORATION; IMAGING SPECTROMETER; RAY FLARE; DME STARS; ENERGY; RECONNECTION; DYNAMICS; MODEL;

D O I：

10.1007/s11207-016-0923-0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

This paper explores the characteristics of 42 solar X-class flares that were observed between February 2011 and November 2014, with data from the Solar Dynamics Observatory (SDO) and other sources. This flare list includes nine X-class flares that had no associated CMEs. In particular our aim was to determine whether a clear signature could be identified to differentiate powerful flares that have coronal mass ejections (CMEs) from those that do not. Part of the motivation for this study is the characterization of the solar paradigm for flare/CME occurrence as a possible guide to the stellar observations; hence we emphasize spectroscopic signatures. To do this we ask the following questions: Do all eruptive flares have long durations? Do CME-related flares stand out in terms of active-region size vs. flare duration? Do flare magnitudes correlate with sunspot areas, and, if so, are eruptive events distinguished? Is the occurrence of CMEs related to the fraction of the active-region area involved? Do X-class flares with no eruptions have weaker non-thermal signatures? Is the temperature dependence of evaporation different in eruptive and non-eruptive flares? Is EUV dimming only seen in eruptive flares? We find only one feature consistently associated with CME-related flares specifically: coronal dimming in lines characteristic of the quiet-Sun corona, i.e. 1 - 2 MK. We do not find a correlation between flare magnitude and sunspot areas. Although challenging, it will be of importance to model dimming for stellar cases and make suitable future plans for observations in the appropriate wavelength range in order to identify stellar CMEs consistently.

引用

页码：1761 / 1782

页数：22

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