On modelling the kinematics and evolutionary properties of pressure-pulse-driven impulsive solar jets

Abstract

Abstract. In this paper, we describe the kinematical and evolutionary properties of the impulsive cool jets in the solar atmosphere using numerical simulation by Godunov-type PLUTO code at two different quiet-Sun magnetic field strengths (B=56 gauss and B=112 gauss). These types of chromospheric jets originate due to a pressure pulse, which mimics the after-effects of the localized heating in the lower solar atmosphere. These jets may be responsible for the transport of mass and energy in the localized upper atmosphere (i.e. corona). The detection of the height–time profiles for the jets, which were developed by imposing different pressure pulses, exhibit asymmetric near-parabolic behaviour. This infers that the upward motion of the jet occurs under the influence of pressure perturbation. However, its downward motion is not only governed by the gravitational free fall, but also by the complex plasma motions near its base under the effect of counter-propagating pulses. The maximum height and lifetime of the jets with respect to the strength of the pressure pulse show a linear increasing trend. This suggests that if the extent of the heating and, thus, the pressure perturbations are longer, then more longer chromospheric jets can be triggered from the same location in the chromosphere. For a certain amplitude of pressure pulse, the strong magnetic field configuration (B=112 gauss) leads to more longer jets compared with the weaker field (B=56 gauss). This suggests that the strong magnetic field guides the pressure-pulse-driven jets more efficiency towards the higher corona. In conclusion, our model mimics the properties and evolution of the variety of the cool impulsive jets in the chromosphere (e.g. macrospicules, network jets, isolated repeated cool jets, confined and small surges, and so on.).

Magnetohydrodynamic Simulations of Spicular Jet Propagation Applied to Lower Solar Atmosphere Model

“…By taking an average value for each velocity data point and then fitting an optimal curve using least squares, we estimated values of C = 10 −2.21 and n = 1.72, as shown in the lower (left) panel in Figure 4. The estimates from the power-law approximation suggest a nonlinear relation between apex height and pulse strength, in contrast to those reported by, e.g., Singh et al (2019). It must, however, be noted that Singh et al (2019) used an instant pressure pulse close to the TR as a driver in their simulation, which might not be directly comparable with our investigation.…”

CME Productive and Non-productive Recurring Jets Near an Active Region AR11176

“…These cool surges are associated with the flare, filament formation and its eruption and coronal mass ejection (CME) in the Sun (e.g., Chen, Jiang and Ma, 2009;Hong et al, 2011, and references cited there). Solar surges have been modeled by the flux emergence and magnetic reconnection process (Yokoyama and Shibata, 1995), impulsive pressure pulse and explosive events (e.g., Steinolfson, Schmahl and Wu, 1979;Shibata et al, 1982;Singh, Sharma and Srivastava, 2019, and references cited there). Apart from hot/cool coronal jets and cool Hα surges, there exist a different class of giant rotating plasma structures which result in coronal swirling motion and tornadoes (e.g., Wedemeyer-Böhm et al, 2012;Su et al, 2014;Wedemeyer and Steiner, 2014, and references cited there).…”

Velocity Response of the Observed Explosive Events in the Lower Solar Atmosphere: I. Formation of the Flowing Cool Loop System

“…In our numerical modelling, we set the Courant-Friedrichs-Lewy number equals to 0.25. We use Roe solver for the flux computation, which is linearized Riemann solver based on the characteristic decomposition of the Roe matrix (cf., Mignone et al 2007, Woloszkiewicz et al 2014, Singh et al 2019).…”

“…In the solar atmosphere maintained at the hydrostatic equilibrium, the realistic temperature profile T(y) is shown in Fig. 5 (right-panel), which is taken from the measurement of Avrett, & Loeser (2008), and also reported in Konkol et al (2010) and Singh et al (2019). The PLUTO code is a Godunov-type, non-linear, finite-volume magnetohydrodynamic (MHD) code which takes into account both ideal and non-ideal sets of governing equations (cf., Mignone et al 2007, Mignone et al 2012, Woloszkiewicz et al 2014.…”

“…In order to model the chromospheric cool plasma flows in the curved magnetic loop system we take into account a gravitationally-stratified and magnetized 2-D solar atmosphere that is described by the set of ideal MHD equations as (Mignone et al 2007;Mignone et al 2012, Woloszkiewicz et al 2014Singh et al 2019) , where v depicts the velocity field, B is the magnetic field satisfying the divergence-free condition at each and every point of the solar atmosphere, µ defines the magnetic permeability, p is the thermal pressure, and 2µ) is magnetic pressure. The specific heat ratio γ is chosen as 5/3.…”