Numerical Simulations of Solar Spicule Jets at a Magnetic Null-Point

Smirnova, V. V.; Konkol, P.; Соловьев, А. А.; Murawski, K.

doi:10.1007/s11207-016-0976-0

Cited by 8 publications

(8 citation statements)

References 19 publications

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“…According to Smirnova et al (2016), for 𝑘 = 1/ℎ, 𝐵 0 = 𝐵 𝑦 (0, 0) has the physical meaning of the magnetic field strength at the point (𝑥 = 0, 𝑦 = 0). Along 𝑦−axes (for 𝑥 = 0 Mm) we have…”

Section: Magnetic Field Configurationmentioning

confidence: 99%

“…Among the numerical simulations related to the null points, there are studies of cool and dense blobs (Murawski et al 2011a) as well as MHD wave propagation and shocks (see, e.g., Kuźma et al 2015;Sabri et al 2020;Pennicott & Cally 2021). Besides, Smirnova et al (2016) performed 2D numerical simulations of jet-like structures by launching a pressure pulse from the null point of a potential magnetic arcade in the framework of the single-fluid MHD and found jets that mimic some properties of type I and type II spicules.…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we extend the model of Smirnova et al (2016) and focus our analysis on a small-scale and inverted-Y shape jet (not limited to spicules) using the two-fluid equations that include ions+electrons and neutrals. In particular, we simulate the formation of an impulsively generated jet by pressure pulses initially launched from a magnetic null point of a potential arcade.…”

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

González-Avilés,

Murawski,

Zaqarashvili

2022

Preprint

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We study the formation and evolution of jets in the solar atmosphere using numerical simulations of partially ionized plasma. The two-fluid magnetohydrodynamic equations with ion+electron and neutral hydrogen components are used in two-dimensional (2D) Cartesian geometry. Numerical simulations show that a localized nonlinear Gaussian pulse of ion and neutral pressures initially launched from the magnetic null point of a potential arcade located below the transition region quickly develops into a shock due to the decrease of density with height. The shock propagates upwards into the solar corona and lifts the cold and dense chromospheric plasma behind in the form of a collimated jet with an inverted-Y shape. The inverted-Y shape of jets is connected with the topology of a magnetic null point. The pulse also excites a nonlinear wake in the chromosphere, which leads to quasi-periodic secondary shocks. The secondary shocks lift the chromospheric plasma upwards and create quasi-periodic jets in the lower corona. Ion and neutral fluids show generally similar behavior, but their relative velocity is higher near the upper part of jets, which leads to enhanced temperature or heating due to ion-neutral collisions. Simulations of jets with inverted-Y shape and their heating may explain the properties of some jets observed in the solar atmosphere.

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Section: Magnetic Field Configurationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

González-Avilés,

Murawski,

Zaqarashvili

2022

Preprint

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“…Also, Martínez-Sykora et al (2009) used three-dimensional MHD numerical simulations to show that type I spicules can be driven by various mechanisms that include p-modes and convecting buffeting of flux concentrations. Another process to excite spicules is found in Smirnova et al (2016), where authors carried out numerical simulations of a localized pressure pulse at the null point of a magnetic arcade. They found the formation of jets with some characteristics of type I and II spicules.…”

Section: Introductionmentioning

confidence: 99%

Numerical simulations of macrospicule jets under energy imbalance conditions in the solar atmosphere

González-Avilés,

Murawski,

Srivastava

et al. 2021

Preprint

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Using numerical simulations, we study the effects of thermal conduction and radiative cooling on the formation and evolution of solar jets with some macrospicules features. We initially assume that the solar atmosphere is rarely in equilibrium through energy imbalance. Therefore, we test whether the background flows resulting from an imbalance between thermal conduction and radiative cooling influence the jets' behavior. In this particular scenario we trigger the formation of the jets by launching a vertical velocity pulse localized at the upper chromosphere for the following test cases: i) adiabatic case; ii) thermal conduction case; iii) radiative cooling case; iv) thermal conduction + radiative cooling case. According to the test results, the addition of the thermal conduction results in smaller and hotter jets than in the adiabatic case. On the other hand the radiative cooling dissipates the jet after reaching the maximum height (≈ 5.5 Mm), making it shorter and colder than in the adiabatic and thermal conduction cases. Besides, the flow generated by the radiative cooling is more substantial than the caused by the thermal conduction. Despite the energy imbalance of the solar atmosphere background, the simulated jet shows morphological features of macrospicules. Furthermore, the velocity pulse steepens into a shock that propagates upward into a solar corona that maintains its initial temperature. The shocks generate the jets with a quasi-periodical behavior that follows a parabolic path on time-distance plots consistent with macrospicule jets' observed dynamics.

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“…The conversion of the fast mode to a slow mode is found to form an apparently stationary wave front, similar to what has been detected in observations. Smirnova et al (2016) perform two-dimensional (2D) numerical simulations of an impulsive pressure perturbation interacting with the null point of a potential magnetic arcade. The formation of double-structured jets comprised of a cold and dense lower region and a hotter and less dense upper region resembles properties of type I and type II spicules, respectively, that have been observed in the solar atmosphere.…”

mentioning

confidence: 99%

Preface to Topical Issue: Waves in the Solar Corona: From Microphysics to Macrophysics

et al. 2016

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Numerical Simulations of Solar Spicule Jets at a Magnetic Null-Point

Cited by 8 publications

References 19 publications

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

Numerical simulations of a two-fluid jet at a magnetic null point in a solar arcade

Numerical simulations of macrospicule jets under energy imbalance conditions in the solar atmosphere

Preface to Topical Issue: Waves in the Solar Corona: From Microphysics to Macrophysics

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