Multiwavelength Observations of Flares on AD Leonis

By S. Hawley, J. Allred, C. Johns–Krull, G. Fisher, W. Abbett, I. Alekseev, S. Avgoloupis, S. Deustua, A. Gunn, J. Seiradakis and 2 more. 2003

172 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3dd76bb633c0b52b78426664a711ef5843f0c32b

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Citations in the corpus

TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM SIMULTANEOUS PHOTOMETRY AND SPECTRA (2013, methodology): “Values of X for the white-light emission are often calculated in the literature (van den Oord et al. 1996; Hawley et al. 2003; Kowalski et al. 2010; Osten et al. 2010; Walkowicz et al. 2011; Davenport et al. 2012).”
WHITE-LIGHT FLARES ON COOL STARS IN THE KEPLER QUARTER 1 DATA (2010, background): “Although stellar flares are fundamentally multiwavelength phenomena and have been observed across the electromagnetic spectrum (e.g. Hawley et al. 2003; Osten et al. 2005; Hawley et al. 2007) photometric flare campaigns in the optical tend to focus on observations in the blue due to the higher…”
ABIOTIC OZONE AND OXYGEN IN ATMOSPHERES SIMILAR TO PREBIOTIC EARTH (2014, background): “…efforts will be greatly aided by knowledge of the stellar energy distribution incident upon the planet, and this strongly motivates future UV observations of different star types, in particular F-type stars and M dwarfs (e. g. Hawley et al. 2003; Walkowicz et al. 2008; France et al. 2012).”
Stellar Lyα Emission Lines in the Hubble Space Telescope Archive: Intrinsic Line Fluxes and Absorption from the Heliosphere and Astrospheres (2005, background): “The high S/N is a result of the unusually long 52 ksec exposure time of the coadded HST spectrum, which was taken as part of an extensive flare monitoring campaign (Hawley et al. 2003).”
THE ULTRAVIOLET RADIATION ENVIRONMENT AROUND M DWARF EXOPLANET HOST STARS (2012, methodology): “Time-domain studies at optical wavelengths are also of interest for characterizing the flare-frequency of the largest flares that are panchromatic events (e.g., Hawley et al. 2003).”
A UNIFIED COMPUTATIONAL MODEL FOR SOLAR AND STELLAR FLARES (2015, background): “These joel.c.allred@nasa.gov stars spin faster and generate much larger magnetic fields (Hawley et al. 2014, and references therein) resulting in flares some 103 times more energetic than typical solar flares (e.g., Hawley & Pettersen 1991; Hawley et al. 2003; Kowalski et al. 2010).”
THE MUSCLES TREASURY SURVEY. I. MOTIVATION AND OVERVIEW (2016, background): “The relative UV emission line strengths also vary during flares (e.g., Hawley et al. 2003; Osten et al. 2005; Loyd & France 2014).”
KEPLER FLARES. II. THE TEMPORAL MORPHOLOGY OF WHITE-LIGHT FLARES ON GJ 1243 (2014, background): “The source of the white light continuum emission in flares, and its relationship to the high energy and emission line behavior during these events, is an active area of research (Butler et al. 1988; Hawley & Pettersen 1991; Hawley et al. 2003; Kowalski et al. 2013). ar X iv :1 41 1.”