Coronal Heating and Solar Wind Generation by Flux Cancellation Reconnection

Abstract

In this paper, we propose that flux cancellation on small granular scales (≲1000 km) ubiquitously drives reconnection at a multitude of sites in the low solar atmosphere, contributing to chromospheric/coronal heating and the generation of the solar wind. We analyze the energy conversion in these small-scale flux cancellation events using both analytical models and three-dimensional, resistive magnetohydrodynamic (MHD) simulations. The analytical models—in combination with the latest estimates of flux cancellation rates—allow us to estimate the energy release rates due to cancellation events, which are found to be on the order 106–107 erg cm−2 s−1, sufficient to heat the chromosphere and corona of the quiet Sun and active regions, and to power the solar wind. The MHD simulations confirm the conversion of energy in reconnecting current sheets, in a geometry representing a small-scale bipole being advected toward an intergranular lane. A ribbon-like jet of heated plasma that is accelerated upward could also escape the Sun as the solar wind in an open-field configuration. We conclude that through two phases of atmospheric energy release—precancellation and cancellation—the cancellation of photospheric magnetic flux fragments and the associated magnetic reconnection may provide a substantial energy and mass flux contribution to coronal heating and solar wind generation.

Characterization of Turbulent Fluctuations in the Sub-Alfvénic Solar Wind

“…Both models have since been refined and extended by, e.g., Oughton et al (2001), Dmitruk et al (2001Dmitruk et al ( , 2002, Suzuki & Inutsuka (2005), Cranmer et al (2007Cranmer et al ( , 2013, Cranmer & van Ballegooijen (2010), Wang et al (2009), Chandran & Hollweg (2009), Verdini et al (2010), Matsumoto & Shibata (2010), Chandran et al (2011), Usmanov et al (2011Usmanov et al ( , 2014, Lionello et al (2014), Woolsey & Cranmer (2014), Shoda et al (2018), Chandran & Perez (2019), and Chandran (2021) for Alfvén wave or slab turbulence heating and driving, and by Zank et al (2021), Adhikari et al (2020Adhikari et al ( , 2022, Telloni et al (2022aTelloni et al ( , 2022bTelloni et al ( , 2023 for 2D nonlinear structures. PSP observations (Bale et al 2023;Raouafi et al 2023), Solar Dynamics Observatory spacecraft observations (Uritsky et al 2023), and theory (Priest et al 2018;Zank et al 2018;Pontin et al 2024) have identified small-and multiscale magnetic reconnection low in the corona as a possible mechanism for solar coronal heating. Such small-and multiscale reconnection can be expected to generate slab (Matthaeus 1999), 2D (Zank et al 2018), or an admixture of MHD turbulence low in the corona.…”