Numerical simulation of solar photospheric jet-like phenomena caused by magnetic reconnection

Abstract

Jet phenomena with a bright loop in their footpoint, called anemone jets, have been observed in the solar corona and chromosphere. These jets are formed as a consequence of magnetic reconnection, and from the scale universality of magnetohydrodynamics (MHD), it can be expected that anemone jets exist even in the solar photosphere. However, it is not necessarily apparent that jets can be generated as a result of magnetic reconnection in the photosphere, where the magnetic energy is not dominant. Furthermore, MHD waves generated from photospheric jets could contribute to chromospheric heating and spicule formation; however, this hypothesis has not yet been thoroughly investigated. In this study, we perform three-dimensional MHD simulation including gravity with the solar photospheric parameter to investigate anemone jets in the solar photosphere. In the simulation, jet-like structures were induced by magnetic reconnection in the solar photosphere. We determined that these jet-like structures were caused by slow shocks formed by the reconnection and were propagated approximately in the direction of the background magnetic field. We also suggested that MHD waves from the jet-like structures could influence local atmospheric heating and spicule formation.

Dissipative Instability of Magnetohydrodynamic Sausage Waves in a Compressional Cylindrical Plasma: Effect of Flow Shear and Viscosity Shear

“…Sunspot or pore can be of interest for DI. But the more smaller radial size, the stronger the DI, so in our view, the detection of DI may be more available for small scale jets (Kotani & Shibata 2020;Muglach 2021;Skirvin et al 2023) or small magnetic loops (Martínez González & Bellot Rubio 2009;Gömöry et al 2010).…”

Unified Relationship between Cold Plasma Ejections and Flare Energies Ranging from Solar Microflares to Giant Stellar Flares

“…Cold plasma ejections have also been found with campfires, which are smaller EUV brightenings recently discovered by the Solar Orbiter/Extreme Ultraviolet Imager (Berghmans et al 2021;Panesar et al 2021). Considering the scale-free self-similar characteristics of magnetohydrodynamics, we can expect similar phenomena at smaller scales (Kotani & Shibata 2020). Even in the case of stellar flares occurring on M-type stars, which are sometimes much stronger than solar flares, blue asymmetry has been found in spectral profiles of the chromospheric lines (Houdebine et al 1990;Vida et al 2016Vida et al , 2019Honda et al 2018;Moschou et al 2019;Maehara et al 2021).…”

Macrospicules and Their Connection to Magnetic Reconnection in the Lower Solar Atmosphere

“…This suggests that the triggering of macrospicules might involve shock waves. The origin of the shock waves has been attributed to two possible mechanisms: the leakage of p-mode waves from the photosphere (e.g., De Pontieu et al 2004;Hansteen et al 2006;Heggland et al 2007;Zhang et al 2017) or the energy release in reconnection (e.g., Takasao et al 2013;Yang et al 2014;Song et al 2017;Kotani & Shibata 2020). In our case, we tend to believe that magnetic reconnection plays a key role in driving the upward shock waves, as suggested by simulations (e.g., Kayshap et al 2013;Takasao et al 2013;Kotani & Shibata 2020).…”

“…The origin of the shock waves has been attributed to two possible mechanisms: the leakage of p-mode waves from the photosphere (e.g., De Pontieu et al 2004;Hansteen et al 2006;Heggland et al 2007;Zhang et al 2017) or the energy release in reconnection (e.g., Takasao et al 2013;Yang et al 2014;Song et al 2017;Kotani & Shibata 2020). In our case, we tend to believe that magnetic reconnection plays a key role in driving the upward shock waves, as suggested by simulations (e.g., Kayshap et al 2013;Takasao et al 2013;Kotani & Shibata 2020). This speculation can be supported by two pieces of observational evidence, including (1) the macrospicules are closely related to reconnection-induced base BPs, and (2) the period of the macrospicules (10 minutes) is much longer than that of the leakage of p-mode wave from the photosphere (3-5 minutes).…”