Solar irradiance variability during the October 2003 solar storm period

By T. Woods, F. Eparvier, J. Fontenla, J. Harder, Greg Kopp, W. McClintock, G. Rottman, B. Smiley, M. Snow. 2004

178 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/068af064a00124d649f470a7110b0d81cfebae6e

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In Astronomy and Astrophysics

Citations in the corpus

Stellar Lyα Emission Lines in the Hubble Space Telescope Archive: Intrinsic Line Fluxes and Absorption from the Heliosphere and Astrospheres (2005, background): “A figure in Woods et al. (2004) implies that quiescent solar Mg II k fluxes are about 1.6 times larger than Lyα.”
The Sun as a star: observations of white-light flares (2011, methodology): “and particle eects. 4.2. The case of the X17 ﬂare on 28 October 2003 The X17 ﬂare thAT occurred on October 28, 2003 is a very large ﬂare and the only one that has been unambiguously detected in TSI (Woods et al. 2004). Fig.6 shows irradiance light curves for this ﬂare and conﬁrms this ﬁnding by show”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, background): “In addition to solar effects, flare-related irradiance enhancements (Woods et al. 2004), solar energetic particles (SEPs, Masson et al. 2009) and coronal mass ejections (CMEs, Vourlidas et al. 2010) constitute major drivers for space weather, and are responsible for various environmental hazards at…”
Solar radiative output and its variability: evidence and mechanisms (2004, methodology): “Hopefully, the novel approaches now being utilized by instruments on the SORCE mission (Rottman et al., 1998; Lawrence et al., 2000; Harder et al., 2000; Woods et al., 2004) will produce spectral irradiance time series with signi cantly higher long-term repeatability than has been achieved thus far.”
Flare Irradiance Spectral Model (FISM): Flare component algorithms and results (2008, background): “…can cause the solar irradiance to increase 1000 times in the X rays (0.1--10 nm), by factors of 2--10 in the extreme ultraviolet (EUV; 10-- 120 nm), and by 1.1--10 times in the far ultraviolet (FUV; 122--200 nm) wavelengths, as well as about a 20% effect for Lyman-a (121.6 nm) [Woods et al., 2004].”
Space Weather: The Solar Perspective (2006, methodology): “After some proper reconstruction using calibrated proxy data the real magnitude of this flare was determined X40 which means a peak flux of 4 mW/m2 at Earth (Woods et al., 2004; Brodrick et al., 2005).”
An Observational Overview of Solar Flares (2011, methodology): “2) from the Total Irradiance Monitor on theSORCEspacecraft (Woods et al. 2004).”
Solar EUV Experiment (SEE): Mission overview and first results (2005, background): “As additional flare information, Woods et al. [2004b] give total and spectral solar irradiance results from SORCE and TIMED for the 28 October 2003 flare.”
The Total Irradiance Monitor (TIM): Science Results (2005, methodology): “…shorter than 100 nm, based on solar EUV measurements from other SORCE instruments and from a similar instrument on NASA’s TIMED mission, only account for roughly 20% of this energy, meaning the majority of the flare’s energy was emitted at wavelengths longer than 200 nm (Woods et al., 2004).”
The October 28, 2003 extreme EUV solar flare and resultant extreme ionospheric effects: Comparison to other Halloween events and the Bastille Day event (2005, background): “[9] VUV flare irradiances have been reported for times near the peaks of the Oct 28 and Nov 4 flares [Woods et al., 2004].”
A brief review of “solar flare effects” on the ionosphere (2009, background): “Flare X-ray fluxes can vary by 3 or even 4 orders of magnitude, EUV fluxes by much less [Tsurutani et al., 2005; Woods et al., 2004, 2006a, 2006b ] and visible light only by a factor of 2 [see Carrington, 1860; Tsurutani et al., 2003a].”