Magnetic Energy Release and Transients in the Solar Flare of 2000 July 14

By Alexander G. Kosovichev, V. V. Zharkova. 2001

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View Paper: https://www.semanticscholar.org/paper/e4f7a34772aa70a22b347a216c1687be20433411

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In Astronomy and Astrophysics

Citations in the corpus

Rapid Change of δ Spot Structure Associated with Seven Major Flares (2005, background): “…been studying flarerelated changes in photospheric magnetic fields for nearly four decades (Severny 1964; Zvereva & Severny 1970; Moore et al. 1984; Kosovichev & Zharkova 1999, 2001; Wang & Tang 1993; Wang et al. 1994), which would provide crucial information as to how an active region stores and…”
Longitudinal Magnetic Field Changes Accompanying Solar Flares (2005, background): “…(1999) detected a permanent change in the longitudinal magnetic field of about 100 G on a timescale of 1–5 minutes and on a spatial scale of 5–20 Mm. Kosovichev & Zharkova (2001) later reported on changes in the magnetic field seen at seven locations in the active region that produced the X5.”
Orientation of the Magnetic Fields in Interplanetary Flux Ropes and Solar Filaments (2001, background): “Kosovichev & Zharkova (2001) also reported rapid oscillations in the magnetic Ðeld during the Ñare.”
Recent Advances in Understanding Particle Acceleration Processes in Solar Flares (2011, background): “Such magnetic field changes are irreversible: the magnetic field reaches a new steady state and does not return to its pre-flare value (Kosovichev & Zharkova 2001; Sudol & Harvey 2005; Zharkova et al. 2005).”
TIME-RESOLVED PROPERTIES AND GLOBAL TRENDS IN dMe FLARES FROM SIMULTANEOUS PHOTOMETRY AND SPECTRA (2013, background): “However, we know today that fluxes larger than this are possible even on the Sun (Neidig et al. 1993; Krucker et al. 2011).”
KEPLER FLARES. I. ACTIVE AND INACTIVE M DWARFS (2014, background): “…and that are therefore more prone to sequential heating of new flaring areas within the same active region, analogous to the appearance of transient optical/UV foot-points during flare evolution as seen in high spatial resolution solar observations (Kosovichev & Zharkova 2001; Wang et al. 2007).”