Observation of kink waves in solar spicules

Kukhianidze, V.; Zaqarashvili, T. V.; Khutsishvili, E. V.

doi:10.1051/0004-6361:200600018

Cited by 87 publications

(72 citation statements)

References 18 publications

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“…A cadence of ∼7.7 s limits the maximum phase speed that may be detected to ∼130 km s −1 . The mean period, amplitude, and phase speed of the observed oscillations are similar to results found for limb spicules (Kukhianidze et al 2006;Zaqarashvili et al 2007;Kim et al 2008;He et al 2009b;Okamoto & de Pontieu 2011).…”

Section: Analysis and Discussionsupporting

confidence: 85%

Transverse Oscillations in Chromospheric Mottles

Kuridze

Morton

Erdélyi

et al. 2012

ApJ

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A number of recent investigations have revealed that transverse waves are ubiquitous in the solar chromosphere. The vast majority of these have been reported in limb spicules and active region fibrils. We investigate long-lived, quiet-Sun, on-disk features such as chromospheric mottles (jet-like features located at the boundaries of supergranular cells) and their transverse motions. The observations were obtained with the Rapid Oscillations in the Solar Atmosphere instrument at the Dunn Solar Telescope. The data set is comprised of simultaneous imaging in the Hα core, Ca ii K, and G band of an on-disk quiet-Sun region. Time-distance techniques are used to study the characteristics of the transverse oscillations. We detect over 40 transverse oscillations in both bright and dark mottles, with periods ranging from 70 to 280 s, with the most frequent occurrence at ∼165 s. The velocity amplitudes and transverse displacements exhibit characteristics similar to limb spicules. Neighboring mottles oscillating in-phase are also observed. The transverse oscillations of individual mottles are interpreted in terms of magnetohydrodynamic kink waves. Their estimated periods and damping times are consistent with phase mixing and resonant mode conversion.

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Section: Analysis and Discussionsupporting

confidence: 85%

Transverse Oscillations in Chromospheric Mottles

Kuridze

Morton

Erdélyi

et al. 2012

ApJ

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“…The bulk (shear) Alfvén waves only exist in a homogeneous medium (Nakariakov & Verwichte 2005;Goossens et al 2013), that is likely not the case in the solar atmosphere. The SCFs are possibly a manifestation of plasma jets along horizontal flux tubes, thus, according to the MHD wave theory, the kink mode is the most appropriate interpretation of their swaying motions (Kukhianidze et al 2006;Erdélyi & Fedun 2007;Zaqarashvili et al 2007). Note, however, that the fact that brightenings along the fibrils start more often inside the bulk of the fibrils than at one of their edges speaks against the interpretation of the fibrils as plasma jets.…”

Section: The Structures Listed Inmentioning

confidence: 99%

Transverse Oscillations in Slender Ca ii H Fibrils Observed with Sunrise/SuFI

Jafarzadeh

Solanki

Gafeira

et al. 2017

ApJS

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We present observations of transverse oscillations in slender Ca IIH fibrils (SCFs) in the lower solar chromosphere. We use a 1 hr long time series of high-(spatial and temporal-) resolutionseeing-free observations in a 1.1 Å wide passband covering the line core of Ca IIH 3969 Å from the second flight of the SUNRISE balloon-borne solar observatory. The entire field of view, spanning the polarity inversion line of an active region close to the solar disk center, is covered with bright, thin, and very dynamic fine structures. Our analysis reveals the prevalence of transverse waves in SCFs with median amplitudes and periods on the order of 2.4±0.8 km s −1 and 83±29 s, respectively (with standard deviations given as uncertainties). We find that the transverse waves often propagate along (parts of) the SCFs with median phase speeds of 9±14 km s −1. While the propagation is only in one direction along the axis in some of the SCFs, propagating waves in both directions, as well as standing waves are also observed. The transverse oscillations are likely Alfvénic and are thought to be representative of magnetohydrodynamic kink waves. The wave propagation suggests that the rapidhigh-frequency transverse waves,often produced in the lower photosphere, can penetrate into the chromospherewith an estimated energy flux of ≈15 kW m −2. Characteristics of these waves differ from those reported for other fibrillar structures, which, however, were observed mainly in the upper solar chromosphere.

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“…Giovanelli (1975), e.g., describes waves along Hα mottles and fibrils with speeds of 70 km s −1 and interprets them as Alfvén waves in magnetic flux tubes with approximately 10 Gauss field strength. Kukhianidze et al (2006), from time sequences in Hα off the limb, found kink waves in spicules with periods of 35−70 s. Hansteen et al (2006) and Rouppe van der Voort et al (2007) observed spicules and fibrils in the quiet Sun and in active regions with high spatial and temporal resolution observations. They succeeded via numerical simulations in explaining the dynamics of these chromospheric small-scale structures by magnetoacoustic shocks, excited mainly by the solar 5-min oscillations (see also the simulations by Sterling & Hollweg 1989; and the review by Carlsson & Hansteen 2005).…”

Section: Introductionmentioning

confidence: 99%

Fast events and waves in an active region of the Sun observed in H$\mathsf{\alpha}$ with high spatial resolution

Nuño

González

Rodríguez

et al. 2008

A&A

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Context. We study the chromosphere of an active region of the Sun in the Hα line. Aims. The development of new instrumentation and new methods of data analysis allows to scrutinize the dynamics of the solar chromosphere with high spatial, spectral, and temporal resolution. The observations we present shed light on some magneto-dynamic processes occurring above an active region in the chromosphere. Methods. We took a time series of 55 min in Hα from AR 10875 at ϑ ≈ 36• . We used the "Göttingen" Fabry-Perot spectrometer at the Vacuum Tower Telescope, Observatorio del Teide/Tenerife, to obtain two-dimensional spectrograms in Hα. Adaptive optics and image reconstruction yielded a spatial resolution better than 0. 5 throughout the time sequence. From the wealth of structures, we selected areas of interest to study further, in detail, some ongoing processes. Results. A small straight surge developed aside of a pore with upward phase speed of 100 km s −1 and line-of-sight (LOS) velocity of 15 km s −1 . The surge retreated rapidly with LOS velocity of 45 km s −1 at its mouth. It underwent a rebound and fell back again. Two sympathetic mini-flares were observed that lasted only approximately 40 s, but showed strong Hα emission. We found magnetoacoustic waves in long fibrils as mainly short wave trains, short packets or pulses, i.e., solitary waves consisting of small (1 −2 ) blobs. They start at either end of the fibrils and travel with phase speeds of 12−14 km s −1 , i.e., close to the tube speed and approximately the sound velocity for sufficiently large magnetic field strengths. Some waves speed up to reach velocities of the order of 30 km s −1 . This is much lower than the expected Alfvén velocity of ≥200 km s −1 for reasonable magnetic field strengths and mass densities. We suggest that slow waves are not purely longitudinal, but possess gas velocities perpendicular to the direction of propagation of few km s −1 . Also, fast waves travel along sinuous lines suggesting entangled magnetic fields. They spread out along the direction of propagation in the course of their evolution and often vanish. We discuss the implications.

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Observation of kink waves in solar spicules

Cited by 87 publications

References 18 publications

Transverse Oscillations in Chromospheric Mottles

Transverse Oscillations in Chromospheric Mottles

Transverse Oscillations in Slender Ca ii H Fibrils Observed with Sunrise/SuFI

Fast events and waves in an active region of the Sun observed in H$\mathsf{\alpha}$ with high spatial resolution

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