Quasi-periodic variations in Doppler velocities of Hα spicules

Khutshishvili, E.; Kulidzanishvili, V. I.; Kvernadze, Teimuraz; Zaqarashvili, T. V.; Kakhiani, V. O.; Khutsishvili, D.; Sikharulidze, M.

doi:10.1007/s10509-014-2100-y

Cited by 10 publications

(7 citation statements)

References 44 publications

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“…Such periodic/quasi-periodic rise and fall of the cool jets are physically well demonstrated in the present numerical simulations. In particular, the detected period of rise and fall of mass in the present case match well with the observed period reported by Khutsishvili et al (2014). There are also several other physical scenarios reported, which claim the formation of the spicule-like jets due to direct onset of the Lorentz force (e.g., Nishizuka et al 2008;Martínez-Sykora et al 2017b;Iijima & Yokoyama 2017;Oxley et al 2020, and references cited therein).…”

Section: Discussionsupporting

confidence: 90%

“…However, the present simulation demonstrates that under the given physical scenario, the quasi-periodic mass motions at typical ≃ 4.0 min time-scale can be generated in situ coupling the chromosphere-TRinner corona. These quasi-periodic mass motions (typical rise and fall of the cool jets) are seen in the observations also (e.g., Khutsishvili et al 2014;Samanta et al 2015). Such periodic/quasi-periodic rise and fall of the cool jets are physically well demonstrated in the present numerical simulations.…”

Section: Discussionsupporting

confidence: 83%

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Quasi-periodic spicule-like cool jets driven by Alfvén pulses

Balveer¹,

Srivastava²,

Sharma³

et al. 2022

Preprint

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We perform a 2.5 dimensional magnetohydrodynamic (MHD) simulation to understand a comprehensive view of the formation of spicule-like cool jets due to initial transverse velocity pulses akin to Alfvén pulses in the solar chromosphere. We invoke multiple velocity (V z ) pulses between 1.5 and 2.0 Mm in the solar atmosphere, which create the initial transverse velocity perturbations. These pulses transfer energy non-linearly to the field aligned perturbations due to the ponderomotive force. This physical process further creates the magnetoacoustic shocks followed by quasi-periodic plasma motions in the solar atmosphere. The field aligned magnetoacoustic shocks move upward which subsequently cause quasi-periodic rise and fall of the chromospheric plasma into the overlying corona as a thin and cool spicule-like jets. The magnitude of the initial applied transverse velocity pulses are taken in the range of 50-90 km s −1 . These pulses are found to be strong enough to generate the spicule-like jets. We analyze the evolution, kinematics and energetics of these spicule-like jets. We find that the transported mass flux and kinetic energy density are substantial in the localized solar-corona. These mass motions generate in situ quasi-periodic oscillations on the scale of ≃ 4.0 min above the transition region.

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Section: Discussionsupporting

confidence: 90%

Section: Discussionsupporting

confidence: 83%

Quasi-periodic spicule-like cool jets driven by Alfvén pulses

Balveer¹,

Srivastava²,

Sharma³

et al. 2022

Preprint

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“…This velocity will depend on the location of the observer (or Line-of-Sight) relative to the flux tube's bulk transverse motion (see Figure 11) and the radiative properties of the plasma along the line of sight. Doppler shift oscillations have recently been observed in Hα solar spicules (Zaqarashvili et al, 2007a;De Pontieu et al, 2012;Khutsishvili et al, 2014Khutsishvili et al, , 2017. The authors determined the properties of spicules and calculated the oscillations present in these structures.…”

Section: Wave Phenomena In Solar Jetsmentioning

confidence: 95%

Small-scale solar jet formation and their associated waves and instabilities

Skirvin¹,

Verth²,

González-Avilés³

et al. 2022

Preprint

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Studies on small-scale jets' formation, propagation, evolution, and role, such as type I and II spicules, mottles, and fibrils in the lower solar atmosphere's energetic balance, have progressed tremendously thanks to the combination of detailed observations and sophisticated mathematical modelling. This review provides a survey of the current understanding of jets, their formation in the solar lower atmosphere, and their evolution from observational, numerical, and theoretical perspectives. First, we review some results to describe the jet properties, acquired numerically, analytically and through high-spatial and temporal resolution observations. Further on, we discuss the role of hydrodynamic and magnetohydrodynamic instabilities, namely Rayleigh-Taylor and Kelvin-Helmholtz instabilities, in jet evolution and their role in the energy transport through the solar atmosphere in fully and partially ionised plasmas. Finally, we discuss several mechanisms of magnetohydrodynamic wave generation, propagation, and energy transport in the context of small-scale solar jets in detail. This review identifies several gaps in the understanding of small-scale solar jets and some misalignments between the observational studies and knowledge acquired through theoretical studies and numerical modelling. It is to be expected that these gaps will be closed with the advent of high-resolution observational instruments, such as Daniel K. Inouye Solar Telescope, Solar Orbiter, Parker Solar Probe, and Solar CubeSats for Linked Imaging Spectropolarimetry, combined with further theoretical and computational developments.

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“…Ïîçaeå, 3-7 -ìèíóòíûå (ïèê íà 5 ìèí) êîëåáàíèÿ ñïèêóë îòìå÷åíû â [24][25][26][27][28][29]. Êîëåáàíèÿ áûëè èçó÷åíû De Pontieu, Erdélyi & James [30], Khutsishvili et al [31,32] è äðóãèìè. Êîëåáàíèÿ ñïèêóë ñ ìåíüøèìè ïåðèîäàìè óïîìèíàþòñÿ â ðàáîòå Nikolsky & Platova [33].…”

mentioning

confidence: 99%

“…Kukhianidze et al, [35] è Zaqarashvili et al, [36] ïîëó÷èëè äëÿ  H -ñïèêóë êîëåáàíèÿ äîïëåðîâñêèõ ñêîðîñòåé â äèàïàçîíå 30-100 ñ (ñì. òàêaeå, [31,37,38]).…”

unclassified

Изменение Доплеровских Скоростей И Полуширин Линии D3 Спикул

Khutsishvili¹,

Khutsishvili²,

Kakhiani³

et al. 2022

Astrophysics

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В представленной работе анализируются спектральные наблюдения спикул в линии гелия D3, полученные в Абастуманской астрофизической обсерватории (Грузия) с помощью 53-см внезатменного коронографа. Сделан вывод, что изменения доплеровских (лучевых) скоростей и полуширины линии D3 находятся в противофазе. Максимумы периодов колебаний доплеровских скоростей совпадают с минимумами колебаний полуширины D3. This paper analyses spectral observations of spicules in the helium D3 line obtained in the Abastumani astrophysical observatory (Georgia) with a 53 cm eclipse-free coronagraph. It is concluded that the changes in the Doppler radial velocities and half-widths of the D3 line are antiphase. The maxima of the Doppler velocity oscillation periods coincide with those of the minima of the D3 half-width oscillations.

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Quasi-periodic variations in Doppler velocities of Hα spicules

Cited by 10 publications

References 44 publications

Quasi-periodic spicule-like cool jets driven by Alfvén pulses

Quasi-periodic spicule-like cool jets driven by Alfvén pulses

Small-scale solar jet formation and their associated waves and instabilities

Изменение Доплеровских Скоростей И Полуширин Линии D3 Спикул

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