English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

In this paper, we describe the kinematical and evolutionary properties of theimpulsive cool jets in the solar atmosphere using numerical simulation byGodunov-type PLUTO code at two different strength of the quiet-Sun magneticfield (B=56, 112 Gauss). These types of chromospheric jets are originated bythe pressure pulse, which mimics after effects of the localized heating in thelower solar atmosphere. These jets may be responsible for the transport of massand energy in the localized upper atmosphere (i.e., corona). The detection ofthe height-time profiles for the jets, originated by imposing the differentpressure pulses, exhibit the asymmetric near parabolic behaviour. This infersthat the upward motion of the jet occurs under the influence of pressureperturbation. However, its downward motion is not only governed by thegravitational free fall, but also due to the complex plasma motions near itsbase under the effect of counter propagating pulses. Maximum height andlife-time of the jets w.r.t. the strength of the pressure pulse show a linearincreasing trend. This suggests that if the extent of the heating and thuspressure perturbations will be longer then more longer chromospheric jets canbe triggered from the same location in the chromosphere. For the certainamplitude of pressure pulse, the strong magnetic field configuration (B=112Gauss) leads more longer jet compared to the weaker field (B=56 Gauss). Thissuggests that the strong magnetic field guides the pressure pulse driven jetsmore efficiency towards the higher corona. In conclusion, our model mimics theproperties and evolution of variety of the cool impulsive jets in thechromosphere (e.g., macrospicules, network jets, isolated repeated cool jets,confined \& small surges etc).

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