Properties of Solar Flares and Associated Sequential Chromospheric Brightenings

Astronomy and Astrophysics – Astrophysics

Scientific paper

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[7507] Solar Physics, Astrophysics, And Astronomy / Chromosphere, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7519] Solar Physics, Astrophysics, And Astronomy / Flares

Scientific paper

Solar sequential chromospheric brightenings (SCBs) are observed in conjunction with coronal mass ejection (CME) related flares. We present results from automated procedures to identify characteristics of large solar flares and flare associated SCBs. These procedures extract physical quantities: temporal variation of flare kernel and SCB relative intensities, relative energies of the bright kernels of the flare, apparent proper motion of the moving ribbons and the rate of SCB propagation. In two events, we observe multiple bursts of SCBs as a function of time and distance. We present evidence that SCBs are a different class of brightening than the flare ribbons and can be divided into two distinct types. The propagation speeds of SCBs are comparable to emerging CME speeds. We also observe an exponential decrease in the SCB intensity as a function of time and distance from the flare peak. The apparent motions of the flare ribbons are quantified and related to the locus of propagating brightening in coronal loops. We analyze H-α Doppler images and relate them to measured flare and SCB characteristics.

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