grenade
发表于 2025-3-25 06:34:07
Thermal Evolution of Flare Plasmaspectral range. The general trend that the thermal plasma observed in soft X-rays is heated by the non-thermal electrons that emit as the hard X-ray bursts is confirmed by the observation of an electron temperature increase at the time interval of hard X-ray spikes and a quantitative comparison betw
HUMID
发表于 2025-3-25 10:36:39
Conductive Flux in the Chromosphere Derived from Line Linear Polarization Observationdirected towards disk center..This polarization could be due to collisional excitation of hydrogen and SI by energetic electrons beamed in the vertical direction. Direct excitation by a highly energetic beam of electrons of order 10–100 keV.is doubtful. The heat flux in the region connecting the tra
召集
发表于 2025-3-25 13:50:25
Upper Limits on the Total Radiant Energy of Solar Flaresn board the Solar Maximum Mission. Typical limits amount to 6 x 10. erg/s for a 32-second integration time, with 5σ statistical significance for an impulsive emission; for a gradual component, about 4 x 10. ergs total radiant energy. The limits lie about an order of magnitude higher than the total r
URN
发表于 2025-3-25 17:03:17
Energetic Electrons as an Energy Transport Mechanism in Solar Flaresen “thermal” and “nonthermal” origins of these electrons. We discuss diagnostics in hard X-rays, especially those relating to the recent observations of the SMM and HINOTORI satellites. We also briefly address the response of the atmosphere to energy input in the form of high energy electrons, in pa
FLEET
发表于 2025-3-25 23:39:07
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stress-response
发表于 2025-3-26 02:03:49
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擦掉
发表于 2025-3-26 06:33:10
Recent Advances in the Understanding of Solar FlaresProceedings of the U
nitroglycerin
发表于 2025-3-26 09:40:34
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collagenase
发表于 2025-3-26 16:14:43
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pulmonary
发表于 2025-3-26 18:21:59
Conductive Flux in the Chromosphere Derived from Line Linear Polarization Observationof the conductive heat flux in the high chromosphere. This conductive flux is of the order of magnitude of the total radiation loss in the chromosphere and below, which is also of the order of magnitude of the conductive flux in the transition zone.