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Parametric survey of longitudinal prominence oscillation simulations View all abstracts by submitter

Qingmin Zhang   Submitted: 2013-04-16 02:58

{Longitudinal filament oscillations recently attracted more and more attention, while the restoring force and the damping mechanisms are still elusive.} {In this paper, we intend to investigate the underlying physics for coherent longitudinal oscillations of the entire filament body, including their triggering mechanism, dominant restoring force, and damping mechanisms.} {With the MPI-AMRVAC code, we carry out radiative hydrodynamic numerical simulations of the longitudinal prominence oscillations. Two types of perturbations, i.e., impulsive heating at one leg of the loop and an impulsive momentum deposition are introduced to the prominence, which then starts to oscillate. We study the resulting oscillations for a large parameter scan, including the chromospheric heating duration, initial velocity of the prominence, and field line geometry.} {It is found that both microflare-sized impulsive heating at one leg of the loop and a suddenly imposed velocity perturbation can propel the prominence to oscillate along the magnetic dip. An extensive parameter survey results in a scaling law, showing that the period of the oscillation, which weakly depends on the length and height of the prominence, and the amplitude of the perturbations, scales with sqrt{R/g_odot}, where R represents the curvature radius of the dip, and g_odot is the gravitational acceleration of the Sun. This is consistent with the linear theory of a pendulum, which implies that the field-aligned component of gravity is the main restoring force for the prominence longitudinal oscillations, as confirmed by the force analysis. However, the gas pressure gradient becomes non-negligible for short prominences. The oscillation damps with time in the presence of non-adiabatic processes. Compared to heat conduction, the radiative cooling is the dominant factor leading to the damping. A scaling law for the damping timescale is derived, i.e., ausim l1.63 D0.66w-1.21v0-0.30, showing strong dependence on the prominence length l, the geometry of the magnetic dip (characterized by the depth D and the width w), and the velocity perturbation amplitude v0. The larger the amplitude, the faster the oscillation damps. It is also found that mass drainage significantly reduces the damping timescale when the perturbation is too strong.}

Authors: Q. M. Zhang, P .F. Chen, C. Xia, R. Keppens, H. S. Ji
Projects: None

Publication Status: A&A in press
Last Modified: 2013-04-17 12:23
Go to main E-Print page  High-Cadence and High-Resolution Halpha Imaging Spectroscopy of a Circular Flare's Remote Ribbon with IBIS  Coronal loop physical parameters from the analysis of multiple observed transverse oscillations  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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