Periodic Motion along a Solar Filament Initiated by a Subflare

Jing, Ju; Lee, Jeongwoo; Spirock, T. J.; Xu, Yan; Wang, Haimin; Choe, G. S.

doi:10.1086/373886

Cited by 128 publications

(160 citation statements)

References 11 publications

Supporting

Mentioning

149

Contrasting

Order By: Relevance

“…In recent years, large amplitude oscillations have been observed not only using H α (Jing et al 2003), but also other wavelengths such as EUV (Isobe & Tripathi 2006), microwave (Isobe et al 2007) and He 10830 Å (Gilbert et al 2008), enabling the plane-of-sky (POS) velocity to be determined. It is therefore possible to combine the LOS and POS information in order to find the total velocity amplitude, as shown by Isobe & Tripathi (2006).…”

Section: Introductionmentioning

confidence: 99%

“…Jing et al 2003), or as a transverse displacement of the prominence axis in either the horizontal (e.g. Isobe & Tripathi 2006) or vertical (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…the time taken for the amplitude of an oscillation to be reduced by a factor of e. Damping times of between two and four cycles have been measured for longitudinal oscillations (Jing et al 2003(Jing et al , 2006Vršnak et al 2007), while for transverse oscillations the damping time has not been quantified, although Gilbert et al (2008) reports a duration of around six cycles for a vertical oscillation. Damping times of two to three cycles are typical for both kink mode loop oscillations (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Gilbert et al 2008), large-scale coronal waves (Okamoto et al 2004), or by nearby sub-flares (e.g. Jing et al 2003) and jets (Isobe & Tripathi 2006). Moreton waves have speeds of around 1000 km s −1 and were first seen by Moreton (1960) using chromospheric filtergrams.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

Hershaw

Foullon

Nakariakov

et al. 2011

A&A

View full text Add to dashboard Cite

Aims. We investigate two successive trains of large amplitude transverse oscillations in an arched EUV prominence, observed with SoHO/EIT on the north-east solar limb on 30 July 2005. The oscillatory trains are triggered by two large scale coronal waves, associated with an X-class and a C-class flare occurring in the same remote active region. Methods. The oscillations are tracked within rectangular slits parallel to the solar limb at different heights, which are taken to move with the apparent height profile of the prominence to account for solar rotation. Time series for the two prominence arch legs are extracted using Gaussian fitting on the 195 Å absorption features, and fitted to a damped cosine curve to determine the oscillatory parameters.Results. Differing energies of the two triggering flares and associated waves are found to agree with the velocity amplitudes, of 50.6 ± 3.2 and 15.9 ± 8.0 km s −1 at the apex, for the first and second oscillatory trains respectively, as estimated in the transverse direction. The period of oscillation is similar for both trains, with an average of 99 ± 11 min, indicating a characteristic frequency as predicted by magnetohydrodynamics. Increasing velocity amplitude with height during the first oscillatory train, and in-phase starting motions of the two legs regardless of height, for each train, demonstrate that the prominence exhibits a global kink mode to a first approximation. However, discrepancies between the oscillatory characteristics of the two legs and an apparent dependence of period upon height, suggest that the prominence actually oscillates as a collection of separate but interacting threads. Damping times of around two to three cycles are observed. Combining our results with those of previously analysed loop oscillations, we find an approximately linear dependence of damping time upon period for kink oscillations, supporting resonant absorption as the damping mechanism despite limitations in testing this theory.

show abstract

Section: Introductionmentioning

confidence: 99%

“…Jing et al 2003), or as a transverse displacement of the prominence axis in either the horizontal (e.g. Isobe & Tripathi 2006) or vertical (e.g.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

Hershaw

Foullon

Nakariakov

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…From observations, such a wave was identified as Moreton or EIT waves (e.g. Ramsey & Smith 1966;Eto et al 2002;Okamoto et al 2004), and these activities were either microflares (Jing et al 2003), emerging flux (Isobe & Tripathi 2006;Isobe et al 2007;Xu et al 2008), or surges . Observational studies of quiescent prominences have revealed a great diversity in characteristic periods ranging from less than 1 min up to 90 min (Bashkirtsev & Mashinich 1984;Tsubaki & Takeuchi 1986;Tsubaki et al 1987aTsubaki et al ,b, 1988Molowny-Horas et al 1999;Terradas et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Small-scale oscillations in a quiescent prominence observed by HINODE/SOT

Ning¹,

Cao²,

Okamoto³

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Investigations of the behavior of small-scale threads can provide an alternative approach to studying prominence dynamics and understanding its origin and nature. Aims. The behavior of threads are analyzed in a quiescent prominence, including drifting and both the horizontally and vertically oscillating motions. These indicate waves in the solar prominence. Methods. We used the Hα images at a setting wavelength of +0.076 Å. A quiescent prominence was observed by HINODE/SOT on 2008 January 15 for about 3 h in total. Results. Consistent with previous findings, prominences show numerous thread-like structures. Some threads clearly exhibit both vertically and horizontally oscillatory motions, while others are only drifting. Complicated cases show both drifting and oscillatory motions simultaneously. In the upper part of the prominence, the threads are oscillating independently of each other. We find that three threads oscillate with the same phase for at least two periods. The oscillations seem to be strongly damped since they disappear after a few periods. The maximum number of observed periods is 8 in our observations. In the lower part of the prominence, however, the different threads have a mixed character with the individual oscillatory motions unstable for one entire period. Most oscillatory motions will disappear after a half period or less, while the new oscillatory motions are excited nearby. A 5-min period is predominant, and the oscillating amplitudes show an average value of ±3.5 km s −1 . We find some upflows in the spicule layer, and they appear to transport the mass from photosphere (or spicules themselves) to the prominence. These upflows have an average velocity amplitude of 0.8 km s −1 . Conclusions. The threads exhibit three distinct behaviors. The first is only drifting, the second is typically oscillating, and the third shows both characteristics. There are no substantial differences between the periods of horizontally and vertically oscillating threads in this prominence.

show abstract

Orbital synchronization of homogeneous mechanical systems with one degree of underactuation

Herrera

Rodríguez-Liñán

Meza‐Sánchez

et al. 2022

Intl J Robust & Nonlinear

View full text Add to dashboard Cite

A methodology for asymptotic orbital synchronization of a set of homogeneous mechanical systems with one degree of underactuation is proposed. A reference model generating a reference orbit is first constructed under the virtual holonomic constraints approach. Then, the  ∞ synthesis is designed to, first, estimate the state vector of the homogeneous systems, provided that only position measurements are available, and second, to drive the state of the systems to that of the reference model. Due to the  ∞ synthesis properties, the homogeneous systems converge asymptotically to the reference orbit when there are no disturbances affecting the systems nor the measurements. When disturbances are present, robustness is guaranteed provided that the  2 gain of the closed-loop systems remains lower than an attenuation level 𝛾. Numerical results for a set of underactuated cart-pendulums corroborate the proposed methodology.

show abstract

Periodic Motion along a Solar Filament Initiated by a Subflare

Cited by 128 publications

References 11 publications

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

Small-scale oscillations in a quiescent prominence observed by HINODE/SOT

Orbital synchronization of homogeneous mechanical systems with one degree of underactuation

Contact Info

Product

Resources

About