Periodic oscillations found in coronal velocity fields

Tsubaki, Tokio

doi:10.1007/bf00240450

Cited by 23 publications

(5 citation statements)

References 3 publications

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“…We note that Tsubaki (1977), Ichimoto & Singh (2000), and Tomczyk et al (2007) reported a presence of waves in the corona with a period of 4 ∼ 5 minutes found in the Doppler signal of the coronal emission lines. Since these waves are not detected in the intensity of coronal emission lines, they are interpreted as Alfvénic waves.…”

Section: Short-period Wavessupporting

confidence: 47%

Observation of Persistent Propagating Waves in a Solar Prominence

Ichimoto,

Hashimoto,

Huang

et al. 2024

ApJ

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Spectropolarimetric observation of a quiescent prominence was performed in He i 1083 nm. With the slit of the spectrograph fixed on the prominence, we obtained a time series of Stokes profiles for a duration of 108 minutes with a cadence of 8 s. Also using imaging spectroscopic data in Hα and extreme-ultraviolet images at 193 Å, we obtained the following results: (1) The prominence harbors persistent waves propagating across its body. (2) The waves are conspicuous in the line-of-sight (LOS) velocity with an amplitude of about 2 km s−1 but not detectable in the intensity of emission lines or magnetic field. (3) Noticeable periods are about 4 minutes (220 and 260 s) and 15 minutes (910 s), and they propagate with phase speeds of 140 ∼ 200 and ∼24 km s−1 preferentially in horizontal and vertical directions, respectively. (4) Magnetic field strength was estimated to be about 2.5 G with its LOS component of 0 ± 1 G on average. We interpret the 4 minute oscillation as Alfvénic waves propagating in the corona containing the prominence threads, and it is not a resonant wave trapped in the prominence body but excited by an external source. On the other hand, a 15 minute oscillation is interpreted as Alfvénic waves propagating upward in the prominence body. The prominence was evolving in its height during our observation, and there is a hint that the 15 minute period gradually gets longer during the observation. These waves are thought to be taking place in layers with different field directions and strength superposed in the LOS.

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Section: Short-period Wavessupporting

confidence: 47%

Observation of Persistent Propagating Waves in a Solar Prominence

Ichimoto,

Hashimoto,

Huang

et al. 2024

ApJ

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“…Early observations already pointed to the existence of quasi-periodic perturbations in solar coronal structures (see e.g., Billings, 1959;Rosenberg, 1970;Vernazza et al, 1975;Tsubaki, 1977;Trottet et al, 1979;Antonucci et al, 1984;Aschwanden, 1987;Deubner & Fleck, 1989). The detection of these oscillations was based on the measurement of the temporal and spatial variation of spectroscopic properties (intensity, width, and Doppler velocity) of coronal emission lines.…”

Section: Observed Wave Activitymentioning

confidence: 99%

“…Early observations already pointed to the existence of quasi-periodic perturbations in solar coronal structures (e.g. [66][67][68][69][70][71][72][73]). The detection of these oscillations was based on the measurement of the temporal and spatial variation of spectroscopic properties (intensity, width and Doppler velocity) of coronal emission lines.…”

Section: Observed Wave Activitymentioning

confidence: 99%

Wave heating of the solar atmosphere

Arregui

2015

Phil. Trans. R. Soc. A.

162

142

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One contribution of 13 to a Theo Murphy meeting issue 'New approaches in coronal heating' . Magnetic waves are a relevant component in the dynamics of the solar atmosphere. Their significance has increased because of their potential as a remote diagnostic tool and their presumed contribution to plasma heating processes. We discuss our current understanding of coronal heating by magnetic waves, based on recent observational evidence and theoretical advances. The discussion starts with a selection of observational discoveries that have brought magnetic waves to the forefront of the coronal heating discussion. Then, our theoretical understanding of the nature and properties of the observed waves and the physical processes that have been proposed to explain observations are described. Particular attention is given to the sequence of processes that link observed wave characteristics with concealed energy transport, dissipation and heat conversion. We conclude with a commentary on how the combination of theory and observations should help us to understand and quantify magnetic wave heating of the solar atmosphere.

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“…Since the first detection of coronal oscillations by the Billings (1959) and their subsequent confirmation by Tsubaki (1977), there have been a number of observational pieces of evidence presented for verifying the widespread existence of oscillations in the solar atmosphere. Using spectroscopic observation with a 40 cm coronagraph, Koutchmy, Zhugzhda, and Locans (1983) found velocity oscillations with periods of 300, 80, and 43 s but no intensity oscillation in the green line (5303 Å).…”

Section: Introductionmentioning

confidence: 99%

Detection of High-Frequency Oscillations and Damping from Multi-slit Spectroscopic Observations of the Corona

et al. 2015

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During the total solar eclipse of 11 July 2010, multi-slit spectroscopic observations of the solar corona were performed from Easter Island, Chile. To search for "high-frequency waves", observations were taken at a high cadence in the green line at 5303Å due to [Fe xiv] and the red line at 6374Å due to [Fe x].The data are analyzed to study the periodic variations in the intensity, Doppler velocity and line width using wavelet analysis. The data with high spectral and temporal resolution enabled us to study the rapid dynamical changes within coronal structures. We find that at certain locations each parameter shows significant oscillation with periods ranging from 6 -25 s. For the first time, we could detect damping of "high-frequency oscillations" with periods of the order of 10 s. If the observed damped oscillations are due to magnetohydrodynamic (MHD) waves then they can contribute significantly in the heating of the corona. From a statistical study we try to characterize the nature of the observed oscillations while looking at the distribution of power in different line parameters.

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Periodic oscillations found in coronal velocity fields

Cited by 23 publications

References 3 publications

Observation of Persistent Propagating Waves in a Solar Prominence

Observation of Persistent Propagating Waves in a Solar Prominence

Wave heating of the solar atmosphere

Detection of High-Frequency Oscillations and Damping from Multi-slit Spectroscopic Observations of the Corona

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