Energy Release in Stellar Flares

Pallavicini, R.

doi:10.1007/978-94-009-0667-9_16

Cited by 1 publication

(1 citation statement)

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“…Broad Balmer emission wings have been observed during flares produced by very different kinds of stars, showing blue or red asymmetries (Doyle et al 1988;Phillips et al 1988;Eason et al 1992;Houdebine et al 1993;Gunn et al 1994a;Abdul-Aziz et al 1995;Abranin et al 1998;Berdyugina et al 1998;Montes & Ramsey 1999;López-Santiago et al 2003) or no obvious line asymmetries (Hawley & Pettersen 1991). Broadened profiles and red asymmetries are important constraints on flare models (Pallavicini 1990). They can be attributed to plasma turbulence or mass motions in the flare region (see Fuhrmeister et al 2005, and references therein).…”

Section: Linementioning

confidence: 99%

Analysis and modeling of high temporal resolution spectroscopic observations of flares on AD Leonis

Crespo‐Chacón

Montes

García-Álvarez

et al. 2006

A&A

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We report the results of a high temporal resolution spectroscopic monitoring of the flare star AD Leo. During 4 nights, more than 600 spectra were taken in the optical range using the Isaac Newton Telescope (INT) and the Intermediate Dispersion Spectrograph (IDS). We observed a large number of short and weak flares occurring very frequently (flare activity > 0.71 h We estimated the physical parameters of the flaring plasma by using a procedure that assumes a simplified slab model of flares. All the obtained physical parameters are consistent with previously derived values for stellar flares, and the areas -less than 2.3% of the stellar surface -are comparable with the size inferred for other solar and stellar flares. We studied the relationships between the physical parameters and the area, duration, maximum flux and energy released during the detected flares.

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