Abstract
Abstract Using numerical simulations, we study the effects of magnetic resistivity and thermal conductivity in the dynamics and properties of solar jets with characteristics of Type II spicules and cool coronal jets. The dynamic evolution of the jets is governed by the resistive MHD equations with thermal conduction along the magnetic field lines on a 2.5D slice. The magnetic field configuration consists of two symmetric neighboring loops with opposite polarity, used to support reconnection and followed by the plasma jet formation. In total, 10 simulations were carried out with different values of resistivity and thermal conductivity that produce jets with different morphological and thermal properties we quantify. We find that an increase in magnetic resistivity does not produce significant effects on the morphology, velocity, and temperature of the jets. However, thermal conductivity affects both temperature and morphology of the jets. In particular, thermal conductivity causes jets to reach greater heights and increases the temperature of the jet-apex. Also, heat flux maps indicate the jet-apex and corona interchange energy more efficiently than the body of the jet. These results could potentially open a new avenue for plasma diagnostics in the Sun’s atmosphere.
Highlights
Solar spicules are small-scale, jet-like plasma features observed ubiquitously in the solar chromosphere (Beckers 1972; Sterling 2000; De Pontieu et al 2004, 2011)
We study the effects of magnetic resistivity and thermal conductivity on the jet formation process with characteristics of Type II spicules
At the top of jetapex the gradient of temperature is nearly radial as seen in Figure 2(a) and magnetic field lines have a radial component; another case is that heat flux is nearly zero aside the jet for z between 2 and 7 Mm because the gradient of T is nearly horizontal whereas the magnetic field lines are nearly vertical, and the effect of thermal conductivity is minimal
Summary
Solar spicules are small-scale, jet-like plasma features observed ubiquitously in the solar chromosphere (Beckers 1972; Sterling 2000; De Pontieu et al 2004, 2011). A number of theoretical models that related to formation and dynamics of spicules, including shocks wave plasma driving (Sterling 2000; De Pontieu et al 2004), Alfvén waves (Cranmer & Woolsey 2015; Iijima & Yokoyama 2017), amplified magnetic tension (Martínez-Sykora et al 2017b), or magnetic reconnection (Ding et al 2011; Sheylag et al 2018). At the end of their life they usually exhibit rapid fading in chromospheric lines (De Pontieu et al 2007a, 2017a)
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