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.).
Highlights
We present a model of the pressurepulse-driven jets and their evolutionary properties, which may mimic the variety of impulsive chromospheric jets originating at the top of the photosphere
The pressure perturbations mimic the impulsive origin of these jets due to the localized heating episodes that might occur at some time epoch in the solar chromosphere and that cause the direct pressure disturbance in the equilibrium atmosphere
We studied chromospheric cool jets in order to be able to take a certain amplitude of the pressure pulse at the chromospheric height below the transition region (TR) to generate these plasma ejecta
Summary
Observations reveal that various types of plasma jets are ubiquitous in the solar atmosphere at diverse spatio-temporal scales (e.g. Sterling, 2000; Katsukawa et al, 2007; Shibata et al, 2007; Nisticò et al, 2009; Wedemeyer-Böhm et al, 2012; Tian et al, 2014; Raouafi et al, 2016; Kayshap et al, 2018, and references cited therein). Sterling, 2000; Katsukawa et al, 2007; Shibata et al, 2007; Nisticò et al, 2009; Wedemeyer-Böhm et al, 2012; Tian et al, 2014; Raouafi et al, 2016; Kayshap et al, 2018, and references cited therein) These jets may play a significant role in transporting energy and mass in the localized upper atmosphere (i.e. corona) of the Sun. As far as the complex magnetic structuring of the solar chromosphere is concerned, it triggers various types of cool plasma jets (e.g. spicules, macrospicules, surges, magnetic swirls, network jets, evolution of plasma twists, and so on.), which attribute to the association of exotic wave and plasma processes Roy, 1973; Wilhelm, 2000; Morita et al, 2010, and references cited therein) The evolution of such a variety of chromospheric jets at diverse spatio-temporal scales provides a very detailed picture of the ongoing different plasma processes triggering these jets in an abundant measure in the localized solar atmosphere
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