TY - JOUR
T1 - GALEX observations of an energetic ultraviolet flare on the dM4e star GJ 3685A
AU - Robinson, Richard D.
AU - Wheatley, Jonathan M.
AU - Welsh, Barry Y.
AU - Forster, Karl
AU - Morrissey, Patrick
AU - Seibert, Mark
AU - Rich, R. Michael
AU - Salim, Samir
AU - Barlow, Tom A.
AU - Bianchi, Luciana
AU - Byun, Yong Ik
AU - Donas, Jose
AU - Friedman, Peter G.
AU - Heckman, Timothy M.
AU - Jelinsky, Patrick N.
AU - Lee, Young Wook
AU - Madore, Barry F.
AU - Malina, Roger F.
AU - Martin, D. Christopher
AU - Milliard, Bruno
AU - Neff, Susan G.
AU - Schiminovich, David
AU - Siegmund, Oswald H.W.
AU - Small, Todd
AU - Szalay, Alex S.
AU - Wyder, Ted K.
PY - 2005/11/1
Y1 - 2005/11/1
N2 - The Galaxy Evolution Explorer (GALEX) satellite has obtained high time resolution ultraviolet photometry during a large flare on the M4 dwarf star GJ 3685 A. Simultaneous Near-ultraviolet (NUV, 1750-2800 Å) and Far-ultraviolet (FUV, 1350-1750 Å) time-tagged photometry with time resolution better than 0.1 s shows that the overall brightness in the FUV band increased by a factor of 1000 in 200 s. Under the assumption that the NUV emission is mostly due to a stellar continuum, and that the FUV flux is shared equally between emission lines and continuum, there is evidence for two distinct flare components for this event. The first flare type is characterized by an exponential increase in flux with little or no increase in temperature. The other involves rapid increases in both temperature and flux. While the decay time for the first flare component may be several hours, the second flare event decayed over less than 1 minute, suggesting that there was little or no confinement of the heated plasma.
AB - The Galaxy Evolution Explorer (GALEX) satellite has obtained high time resolution ultraviolet photometry during a large flare on the M4 dwarf star GJ 3685 A. Simultaneous Near-ultraviolet (NUV, 1750-2800 Å) and Far-ultraviolet (FUV, 1350-1750 Å) time-tagged photometry with time resolution better than 0.1 s shows that the overall brightness in the FUV band increased by a factor of 1000 in 200 s. Under the assumption that the NUV emission is mostly due to a stellar continuum, and that the FUV flux is shared equally between emission lines and continuum, there is evidence for two distinct flare components for this event. The first flare type is characterized by an exponential increase in flux with little or no increase in temperature. The other involves rapid increases in both temperature and flux. While the decay time for the first flare component may be several hours, the second flare event decayed over less than 1 minute, suggesting that there was little or no confinement of the heated plasma.
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U2 - 10.1086/444608
DO - 10.1086/444608
M3 - Article
AN - SCOPUS:29144491457
VL - 633
SP - 447
EP - 451
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 I
ER -