On the Asymmetric Longitudinal Oscillations of a Pikelner’s Model Prominence

Kraśkiewicz, J.; Murawski, K.; Соловьев, А. А.; Srivastava, A. K.

doi:10.1007/s11207-016-0850-0

Cited by 6 publications

(8 citation statements)

References 28 publications

(42 reference statements)

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“…Stable vertical fast and longitudinal slow MHD oscillations were found. Luna et al (2012) and Kraśkiewicz et al (2016) also considered prominences of a normal configuration, residing in a dip formed by curved magnetic field lines. The effects of the magnetic field geometry on longitudinal oscillations in prominences were addressed.…”

Section: Introductionmentioning

confidence: 99%

Finite amplitude transverse oscillations of a magnetic rope

Kolotkov

Nisticò

Rowlands

et al. 2018

Journal of Atmospheric and Solar-Terrestrial Physics

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The effects of finite amplitudes on the transverse oscillations of a quiescent prominence represented by a magnetic rope are investigated in terms of the model proposed by Kolotkov et al. (2016). We consider a weakly nonlinear case governed by a quadratic nonlinearity, and also analyse the fully nonlinear equations of motion. We treat the prominence as a massive line current located above the photosphere and interacting with the magnetised dipped environment via the Lorentz force. In this concept the magnetic dip is produced by two external current sources located at the photosphere. Finite amplitude horizontal and vertical oscillations are found to be strongly coupled between each other. The coupling is more efficient for larger amplitudes and smaller attack angles between the direction of the driver and the horizontal axis. Spatial structure of oscillations is represented by Lissajous-like curves with the limit cycle of a hourglass shape, appearing in the resonant case, when the frequency of the vertical mode is twice the horizontal mode frequency. A metastable equilibrium of the prominence is revealed, which is stable for small amplitude displacements, and becomes horizontally unstable, when the amplitude exceeds a threshold value. The maximum oscillation amplitudes are also analytically derived and analysed. Typical oscillation periods are determined by the oscillation amplitude, prominence current, its mass and position above the photosphere, and the parameters of the magnetic dip. The main new effects of the finite amplitude are the coupling of the horizontally and vertically polarised transverse oscillations (i.e. the lack of a simple, elliptically polarised regime) and the presence of metastable equilibria of prominences.

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Section: Introductionmentioning

confidence: 99%

Finite amplitude transverse oscillations of a magnetic rope

Kolotkov

Nisticò

Rowlands

et al. 2018

Journal of Atmospheric and Solar-Terrestrial Physics

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“…Therefore, from Eqs. (12) and (13), we find the following expressions for and p (Solov'ev 2010; Kraśkiewicz et al 2015;Kuźma et al 2015):…”

Section: Magnetic Atmospherementioning

confidence: 84%

“…These models are based on the analytical models of Solov'ev (2010). The Kraśkiewicz et al (2015) and Kuźma et al (2015) reports can also be referred for detailed mathematical formulation of the analytical and numerical models. Using these models, we performed the 2D numerical simulations of the vertical kink oscillations of this loop excited by the forced periodic driver that acts at the top of the photosphere, centrally below the apex of the loop.…”

Section: Discussionmentioning

confidence: 99%

New analytical and numerical models of a solar coronal loop

Murawski

Соловьев

Kraśkiewicz

et al. 2015

A&A

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Aims. We construct a new analytical model of a solar coronal loop that is embedded in a gravitationally stratified and magnetically confined atmosphere. On the basis of this analytical model, we devise a numerical model of solar coronal loops. We adopt this model to perform the numerical simulations of its vertical kink oscillations excited by an external driver. Methods. Our model of the solar atmosphere is constructed by adopting a realistic temperature distribution and specifying the curved magnetic field lines that constitute a coronal loop. This loop is described by 2D, ideal magnetohydrodynamic equations that are numerically solved by the FLASH code. Results. The vertical kink oscillations are excited by a periodic driver in the vertical component of velocity, which is acting at the top of the photosphere. For this forced driver with its amplitude 3 km s −1 , the excited oscillations exhibit about 1.2 km s −1 amplitude in their velocity and the loop apex oscillates with an amplitude in displacement of about 100 km. Conclusions. The newly devised analytical model of the coronal loops is utilized for the numerical simulations of the vertical kink oscillations, which match well with the recent observations of decayless kink oscillations excited in solar loops. The model will have further implications on the study of waves and plasma dynamics in coronal loops, revealing physics of energy and mass transport mechanisms in the localized solar atmosphere.

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“…Leading into this framework, we generalized the analytical model of Kraśkiewicz et al (2015) by implementing a magnetic field component along the invariant direction B z . The model we devised can be adopted to derive equilibrium conditions for any 2.5D magnetic structure in the solar atmosphere.…”

Section: Discussionmentioning

confidence: 99%

“…From Eqs. (21) and (27), it follows that the equilibrium mass density, , and a gas pressure, p, simplify to the following expressions (see also Solov'ev 2010; Kraśkiewicz et al 2015):…”

Section: The Magnetic Null Linementioning

confidence: 99%

Numerical simulations of sheared magnetic lines at the solar null line

Kuźma

Murawski

Соловьев

2015

A&A

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Aims. We perform numerical simulations of sheared magnetic lines at the magnetic null line configuration of two magnetic arcades that are settled in a gravitationally stratified and magnetically confined solar corona. Methods. We developed a general analytical model of a 2.5D solar atmospheric structure. As a particular application of this model, we adopted it for the curved magnetic field lines with an inverted Y shape that compose the null line above two magnetic arcades, which are embedded in the solar atmosphere that is specified by the realistic temperature distribution. The physical system is described by 2.5D magnetohydrodynamic equations that are numerically solved by the FLASH code. Results. The magnetic field line shearing, implemented about 200 km below the transition region, results in Alfvén and magnetoacoustic waves that are able to penetrate solar coronal regions above the magnetic null line. As a result of the coupling of these waves, partial reflection from the transition region and scattering from inhomogeneous regions the Alfvén waves experience fast attenuation on time scales comparable to their wave periods, and the physical system relaxes in time. The attenuation time grows with the large amplitude and characteristic growing time of the shearing. Conclusions. By having chosen a different magnetic flux function, the analytical model we devised can be adopted to derive equilibrium conditions for a diversity of 2.5D magnetic structures in the solar atmosphere.

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On the Asymmetric Longitudinal Oscillations of a Pikelner’s Model Prominence

Cited by 6 publications

References 28 publications

Finite amplitude transverse oscillations of a magnetic rope

Finite amplitude transverse oscillations of a magnetic rope

New analytical and numerical models of a solar coronal loop

Numerical simulations of sheared magnetic lines at the solar null line

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