Longitudinal Magnetic Field Changes Accompanying Solar Flares

By J. Sudol, J. Harvey. 2005

240 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/de992ef4596d6674d665206eb47e73de4ed6df06

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Citations in the corpus

Alfvén Waves in the Solar Atmosphere (2012, background): “The potential of large-amplitude prominence oscillations for deriving the vertical magnetic field was first explored by Hyder (1966), who obtained field strengths of tens of Gauss.”
RESPONSE OF THE PHOTOSPHERIC MAGNETIC FIELD TO THE X2.2 FLARE ON 2011 FEBRUARY 15 (2011, background): “On the other hand, flare-related variations in the line-of-sight (LOS) component of pho- tospheric magnetic field have been clearly recognized (e.g., Wang et al. 2002; Spirock et al. 2002; Yurchyshyn et al. 2004; Sudol & Harvey 2005; Wang 2006; Wang & Liu 2010; Petrie & Sudol 2010).”
An Observational Overview of Solar Flares (2011, background): “When a solar flare happens, the observed photospheric field changes in a stepwise manner (Wang 1992; Sudol & Harvey 2005).”
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).”
WHY IS THE GREAT SOLAR ACTIVE REGION 12192 FLARE-RICH BUT CME-POOR? (2015, background): “The actual change near the FPIL is permanent and likely occurs on a timescale of minutes (Sudol & Harvey 2005).”
Global Properties of Solar Flares (2011, methodology): “The photospheric fields themselves also show striking flare effects when viewed via Zeeman splitting, rather than as an image feature such as umbra or facula (Wang 1992; Kosovichev and Zharkova 2001; Sudol and Harvey 2005) (see Figure 23).”
Global Forces in Eruptive Solar Flares: The Lorentz Force Acting on the Solar Atmosphere and the Solar Interior (2010, background): “Assuming a time scale of ten minutes for the photospheric magnetic fields to change (from the temporal evolution results of Sudol and Harvey, 2005 and Petrie and Sudol, 2010) then results in an upper limit on the mass of any CME coming from this flaring active region of 4.9× 1016 g.”
Impulsive Phase Flare Energy Transport by Large-Scale Alfvén Waves and the Electron Acceleration Problem (2007, methodology): “Sudol & Harvey (2005), using simultaneous SOHOMDI andGONGmagnetogram data, observe permanent line-of-sight photospheric magnetic changes (0.01–0.02T) to be ‘‘ubiquitous features’’ of X-class flares at least.”
Driving major solar flares and eruptions: A review (2008, background): “Sudol and Harvey (2005), for example, find: a) that the time scale for changes in the l.o.s. field is less than ∼ 10min., some even less than one minutes, but in all cases abrupt; b) in many cases these changes are close to the noise but in some cases very significant; c) the changes persist for at…”
EVOLUTION OF MAGNETIC FIELD AND ENERGY IN A MAJOR ERUPTIVE ACTIVE REGION BASED ON SDO/HMI OBSERVATION (2011, background): “During this process, fast, irreversible changes of the photospheric field have been observed as the possible imprint of the coronal activity, including transverse field and magnetic shear increase (e.g. Wang et al. 1994; Wang 2006) and longitudinal field decrease (Sudol & Harvey 2005).”