Results 111 to 120 of about 324,715 (248)
Space Weather, 2018 On 6 September 2017, an X‐class flare of the magnitude 9.3 occurred around noon UT, being the strongest flare event in a decade. The flare itself was the highlight of a quite interesting phase of solar‐terrestrial interactions caused by the active region
J. Berdermann +8 more
semanticscholar +1 more source
, 2016 In this paper, we focus on the pre-flare coronal dimmings. We report our multiwavelength observations of the GOES X1.6 solar flare and the accompanying halo CME produced by the eruption of a sigmoidal magnetic flux rope (MFR) in NOAA active region (AR ...
Ji, H. S., Su, Y. N., Zhang, Q. M.
core +1 more source
Block-induced Complex Structures Building the Flare-productive Solar Active Region 12673 [PDF]
, 2017 Solar active region (AR) 12673 produced 4 X-class, 27 M-class, and numerous lower-class flares during its passage across the visible solar disk in 2017 September.
Shuhong Yang +3 more
semanticscholar +1 more source
Early Abnormal Temperature Structure of X-ray Looptop Source of Solar Flares [PDF]
, 2008 This Letter is to investigate the physics of a newly discovered phenomenon -- contracting flare loops in the early phase of solar flares. In classical flare models, which were constructed based on the phenomenon of expansion of flare loops, an energy releasing site is put above flare loops.
arxiv +1 more source
The Relationship Between EUV Nonthermal Line Broadening and High-energy Particle During Solar Flare [PDF]
, 2013 We have studied the relationship between the location of EUV nonthermal broadening and high-energy particles during the large flares by using EUV imaging spectrometer onboard {\it Hinode}, Nobeyama Radio Polarimeter, Nobeyama Radioheliograph, and Atmospheric Imaging Assembly onboard {\it Solar Dynamic Observatory}. We have analyzed the five large flare
arxiv +1 more source
Chromospheric Evaporation in an X1.0 Flare on 2014 March 29 Observed with IRIS and EIS
, 2015 Chromospheric evaporation refers to dynamic mass motions in flare loops as a result of rapid energy deposition in the chromosphere. These have been observed as blueshifts in X-ray and extreme-ultraviolet (EUV) spectral lines corresponding to upward ...
Cheng, J. X. +3 more
core +1 more source
Using the Maximum X-ray Flux Ratio and X-ray Background to Predict Solar Flare Class [PDF]
, 2015 We present the discovery of a relationship between the maximum ratio of the flare flux (namely, 0.5-4 Ang to the 1-8 Ang flux) and non-flare background (namely, the 1-8 Ang background flux), which clearly separates flares into classes by peak flux level.
arxiv +1 more source
GLOBAL SAUSAGE OSCILLATION OF SOLAR FLARE LOOPS DETECTED BY THE INTERFACE REGION IMAGING SPECTROGRAPH [PDF]
, 2016 An observation from the Interface Region Imaging Spectrograph reveals coherent oscillations in the loops of an M1.6 flare on 2015 March 12. Both the intensity and Doppler shift of Fe xxi 1354.08 Å show clear oscillations with a period of ∼25 s ...
H. Tian +6 more
semanticscholar +1 more source
A White Light Megaflare on the dM4.5e Star YZ CMi
, 2010 On UT 2009 January 16, we observed a white light megaflare on the dM4.5e star YZ CMi as part of a long-term spectroscopic flare-monitoring campaign to constrain the spectral shape of optical flare continuum emission.
Abbett +18 more
core +1 more source
, 2020 Solar flare activity is characterised by different classification systems, both in optical and X-ray ranges. The most generally accepted classifications of solar flares describe important parameters of flares such as the maximum of brightness of the ...
Bruevich, Elena
core