2016/09/29 by J. J. González-Avilés, F. S. Guzmán, V. Fedun
Physics and Astronomy · #Astrophysics #Atmosphere (unit) #Chromosphere #Computational physics #Corona (planetary geology) #Coronal loop #Coronal mass ejection #Ionosphere and magnetosphere dynamics #Jet (fluid) #Magnetic field #Magnetic reconnection #Magnetohydrodynamics #Mechanics #Meteorology #Nanoflares #Physics #Plasma #Solar and Space Plasma Dynamics #Solar wind #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.3847/1538-4357/836/1/24
published as ApJ 836, 24 (2017) · Submitted to ApJ
arxiv created 2016/09/29 · openalex publication_date 2017/02/06 · arxiv updated 2017/05/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Using numerical simulations, we show that jets with features of type II spicules and cool coronal jets corresponding to temperatures of 10 4 K can be formed as a result of magnetic reconnection in a scenario with magnetic resistivity. For this, we model the low chromosphere–corona region using the C7 equilibrium solar atmosphere model, assuming that resistive MHD rules the dynamics of the plasma. The magnetic field configurations we analyze correspond to two neighboring loops with opposite polarity. The formation of a high-speed and sharp structure depends on the separation of the loops' feet. We analyze the cases where the magnetic field strength of the two loops is equal and different. In the first case, with a symmetric configuration the jets rise vertically, whereas in an asymmetric configuration the structure shows an inclination. With a number of simulations carried out under a 2.5D approach, we explore various properties of the excited jets, namely, inclination, lifetime, and velocity. The parameter space involves a magnetic field strength between 20 and 40 G, and the resistivity is assumed to be uniform with a constant value of the order .