Propagating Oscillations in the Lower Atmosphere Under Coronal Holes

Chelpanov, Andrei; Кобанов, Н. И.; Челпанов, Максим; Kiselev, Aleksandr

doi:10.1007/s11207-021-01909-y

Cited by 5 publications

(1 citation statement)

References 58 publications

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“…The observed oscillations can be associated with the lower atmospheric oscillations or they could be in-situ oscillations. Many authors have investigated the propagation of waves from the photosphere to the TR, as well as the relationship between upper and lower region oscillations (e.g., Zeighami et al 2020;Kayshap et al 2020;Chelpanov et al 2021). They interpreted these waves as upward propagating slow magneteoacoustic waves as they propagate along magnetic field lines and their phase speed between two heights is almost equal to the local sound speed.…”

Section: Discussionmentioning

confidence: 99%

Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using Si IV spectral line

Sangal¹,

Srivastava²,

Kayshap³

et al. 2022

Preprint

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In the present paper, we use Si IV 1393.755 Å spectral line observed by the Interface Region Imaging Spectrograph (IRIS) in the quiet-Sun to determine physical nature of the solar transition region (TR) oscillations. We analyze the properties of these oscillations using wavelet tools (e.g., power, cross-power, coherence, and phase difference) along with the stringent noise model (i.e., power-law + constant). We estimate the period of the intensity and Doppler velocity oscillations at each chosen location in the quiet-Sun (QS) and quantify the distribution of the statistically significant power and associated periods in one bright and two dark regions. In the bright TR region, the mean periods in intensity and velocity are 7 min, and 8 min respectively. In the dark region, the mean periods in intensity and velocity are 7 min, and 5.4 min respectively. We also estimate the phase difference between the intensity and Doppler velocity oscillations at each location. The statistical distribution of phase difference is estimated, which peaks at -119°± 13°, 33°± 10°, 102°± 10°in the bright region, while at -153°± 13°, 6°± 20°, 151°± 10°in the dark region. The statistical distribution reveals that the oscillations are caused by propagating slow magnetoacoustic waves encountered with the TR. Some of these locations may also be associated with the standing slow waves. Even, in the given time domain, several locations exhibit presence of both propagating and standing oscillations at different frequencies.

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Section: Discussionmentioning

confidence: 99%

Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using Si IV spectral line

Sangal¹,

Srivastava²,

Kayshap³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

Magnetohydrodynamic (MHD) Waves and Oscillations in the Sun’s Corona and MHD Coronal Seismology: Editorial

Kolotkov

Leibacher

2023

Sol Phys

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Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using the Si iv spectral line

Sangal

Srivastava

Kayshap

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In this paper, we use the Si iv 1393.755 Å spectral line observed by the Interface Region Imaging Spectrograph (IRIS) in the quiet-Sun (QS) to determine the physical nature of the solar transition region (TR) oscillations. We analyse the properties of these oscillations using wavelet tools (e.g. power, cross-power, coherence, and phase difference) along with the stringent noise model (i.e. power law + constant). We estimate the period of the intensity and Doppler velocity oscillations at each chosen location in the QS and quantify the distribution of the statistically significant power and associated periods in one bright region and two dark regions. In the bright TR region, the mean periods in intensity and velocity are 7 min and 8 min, respectively. In the dark regions, the mean periods in intensity and velocity are 7 min and 5.4 min, respectively. We also estimate the phase difference between the intensity and Doppler velocity oscillations at each location. The statistical distribution of the phase difference is estimated, which peaks at −119° ± 13°, 33° ± 10°, 102° ± 10° in the bright region and at −153° ± 13°, 6° ± 20°, 151° ± 10° in the dark regions. The statistical distribution reveals that the oscillations are caused by propagating slow magneto-acoustic waves encountered with the TR. Some of these locations may also be associated with standing slow waves. Moreover, in the given time domain, several locations exhibit the presence of both propagating and standing oscillations at different frequencies.

show abstract

Propagating Oscillations in the Lower Atmosphere Under Coronal Holes

Cited by 5 publications

References 58 publications

Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using Si IV spectral line

Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using Si IV spectral line

Magnetohydrodynamic (MHD) Waves and Oscillations in the Sun’s Corona and MHD Coronal Seismology: Editorial

Spectroscopic study of solar transition region oscillations in the quiet-Sun observed by IRIS using the Si iv spectral line

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