Extreme solar storms based on solar magnetic field

Abstract

Many questions have to be answered before understanding the relationship between the emerging magnetic flux through the solar surface and the extreme geoeffective events. Which threshold determines the onset of the eruption? What is the upper limit in energy for a flare? Is the size of sunspot the only criteria to get extreme solar events? Based on observations of previous solar cycles, and theory, the main ingredients for getting X ray class flares and large Interplanetary Corona Mass Ejections e.g. the built up of the electric current in the corona, are presented such as the existence of magnetic free energy, magnetic helicity, twist and stress in active regions. The upper limit of solar flare energy in space research era and the possible chances to get super-flares and extreme solar events can be predicted using MHD simulation of coronal mass ejections

21 pages,4 Figures, Varsiti Conference in Varna June 2016

References in corpus (6)

• Why Is the Great Solar Active Region 12192 Flare-Rich But CME-Poor?
• Strong coronal channelling and interplanetary evolution of a solar storm up to Earth and Mars
• Magnetic Properties of Solar Active Regions that Govern Large Solar Flares and Eruptions
• The Confined X-class Flares of Solar Active Region 2192
• Three-dimensional evolution of erupted flux ropes from the Sun (2-20 Rs) to 1 AU
• Modeling the recovery phase of extreme geomagnetic storms

Cited by in corpus (5)

• Extreme solar events
• Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
• Statistical Properties of Superflares on Solar-type Stars: Results Using All of the Kepler Primary Mission Data
• The New 2018 Version of the Meudon Spectroheliograph
• Reminiscences