The white-light flare of 1982 June 15 - A midchromospheric kernel

Mauas, P. J. D.

doi:10.1086/173136

Cited by 8 publications

(4 citation statements)

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“…This fact was already known for the Sun (Vernazza et al 1981), and was later found in Paper I for other G stars, for which negative cooling rates in the temperature minimum region were also obtained. Within the plane-parallel, homogeneous approximation we are investigating, this implies either mechanical energy extraction or, more likely, that the calculations have neglected important sources of radiative cooling (see Mauas 1993).…”

Section: Non-radiative Heating In K Starsmentioning

confidence: 99%

Chromospheric changes in K stars with activity

Vieytes

Mauas

Díaz

2009

Monthly Notices of the Royal Astronomical Society

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Section: Non-radiative Heating In K Starsmentioning

confidence: 99%

Chromospheric changes in K stars with activity

Vieytes

Mauas

Díaz

2009

Monthly Notices of the Royal Astronomical Society

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“…Machado et al (1980) developed models for a bright flare and a faint one that reproduce lines and continua of H I, Si I, C I, Ca II, and Mg II, and show a substantial temperature enhancement from the photosphere up to the transition region. Semi-empirical models of a white-light flare also show that flare-related perturbations can affect the formation heights of the wings and continuum, as well as the continuum emission originating in the photosphere (Mauas 1990(Mauas , 1993Mauas et al 1990). Gan & Fang (1987) and Gan et al (1993) used Hα line profiles to construct semi-empirical models for two flares that showed evidence for chromospheric condensations, which can reproduce the well-observed asymmetries in Hα line profiles in flares.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic Inversions of the Ca ii 8542 Å Line in a C-class Solar Flare

Kuridze

Henriques

Mathioudakis

et al. 2017

ApJ

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We study the C8.4-class solar flare SOL2016-05-14T11:34 UT using high-resolution spectral imaging in the Ca II 8542 Å line obtained with the CRISP imaging spectropolarimeter on the Swedish 1 m Solar Telescope. Spectroscopic inversions of the Ca II 8542 Å line using the non-LTE code NICOLE are used to investigate the evolution of the temperature and velocity structure in the flaring chromosphere. A comparison of the temperature stratification in flaring and non-flaring areas reveals strong footpoint heating during the flare peak in the lower atmosphere. The temperature of the flaring footpoints between log 2.5 and 3.5 500 t » --, where τ 500 is the continuum optical depth at 500 nm, is 5 6.5 kK -close to the flare peak, reducing gradually to 5 kK . The temperature in the middle and upper chromosphere, between log 3.5 500 t » -and −5.5, is estimated to be ∼6.5-20 kK, decreasing to preflare temperatures, ∼5-10 kK, after approximately 15 minutes. However, the temperature stratification of the non-flaring areas is unchanged. The inverted velocity fields show that the flaring chromosphere is dominated by weak downflowing condensations at the formation height of Ca II 8542 Å.

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“…For example the temperature-height structure around the temperature minimum region can be studied using the Ca II K lines (Machado et al 1978), and the temperature and density structure respectively from Mg I at 4571Å and 5173Å (Metcalf et al 1990a,b). The mid and upper chromosphere are sampled by other lines such as the Mg I b multiplet (Mauas 1993), CIV 1549Å and of course the hydrogen Balmer series. Both the structure of the heated flare atmosphere (e.g.…”

Section: Fletchermentioning

confidence: 99%