Solar Flares and Solar Magnetic Reconnection Get New Spotlight in Two Blazing Studies

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Solar Flares and Solar Magnetic Reconnection Get New Spotlight in Two Blazing Studies
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Image of a solar flare obtained by NASA’s Solar Dynamics Observatory on Oct. 2, 2014, with a burst of solar material erupting being observed just to the right of the solar flare. discuss findings regarding solar flare properties and a new classification index and the Sun’s magnetic field, specifically what’s called solar magnetic reconnection.

For the study, the researchers sought to expand upon and improve the GOES classification index by measuring what’s known as impulsiveness, which Tamburri refers to as a “suddenness” of energy release. During a 4-year period between 2010 and 2014, the researchers obtained impulsiveness measurements using Solar Dynamics Observatory/Extreme Ultraviolet Experiment for 1,368 solar flares, categorizing their impulsiveness as low, mid, and high.

“At this point, we don’t fully understand the fast, intense initial phase of a flare,” Tamburri tells. “Ultimately, an accurate, complete picture of the flaring process must tie together the flare process in all regimes – the magnetic field in the low-density corona, the high-energy processes in the dense chromosphere, and even what lies below, in the photosphere.

For the study, the researchers analyzed high-resolution imaging data from a set of M-class and X-class solar flares and statistical analyses on 73 solar flares ranging from C-class to X-class using a known flare ribbon computer database to ascertain QPP properties. Better understanding the mechanisms responsible for QPPs will provide greater insight into solar flare energy and activity within the Sun’s atmosphere and the relationship they have with solar magnetic reconnection.

“The results of this study suggest that the plasma contained within the region where magnetic reconnection occurs during solar flare are involved in highly complex dynamics,” Corchado-Albelo tells. “Understanding the origin of these dynamics can help us diagnose properties of the solar magnetic fields involved in flare reconnection. Properties that could help us possibly constrain the flaring magnetic field geometry, as well as potentially the strength of the field in the reconnection region.

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