Periodic processes and plasma motions in solar coronal holes

Кобанов, Н. И.; Sklyar, A. A.

doi:10.1134/s1063772907090077

Cited by 9 publications

(3 citation statements)

References 18 publications

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“…These magnetic fields can act as waveguides for MHD waves. From observations of 15 coronal holes, Kobanov and Sklyar [2007] have found pronounced oscillations in three-and five-minute ranges. In the five-minute range, they found signs of propagating waves.…”

Section: Oscillations On the Sunmentioning

confidence: 98%

Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

Chelpanov¹,

Челпанов²,

Кобанов³

et al. 2018

Solar-Terrestrial Physics

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The aim of this paper is to structure and extend the knowledge of solar chromospheric sources of oscillations in the solar wind and their relationships with pulsations registered in the magnetosphere. We compare the oscillation spectra that we observe using instruments of the Institute of Solar-Terrestrial Physics in different chromospheric structures with those observed in the solar wind and magnetosphere. We explore the possibility that the observed periodic variations of the chromospheric line widths can be interpreted as torsional Alfvén wave manifestationthis mode can propagate long distances without dissipating in the interplanetary space; it can penetrate into Earth's magnetosphere directly or due to processes occurring at the plasmapause. We emphasize the similarities in the oscillation characteristics observed in different media, the similarities in the parameters of the media themselves and the processes developing in them. We believe that similar approaches can be applied to studying these media.

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Section: Oscillations On the Sunmentioning

confidence: 98%

Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

Chelpanov¹,

Челпанов²,

Кобанов³

et al. 2018

Solar-Terrestrial Physics

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show abstract

“…The sources of the solar wind are located at the heights of the chromosphere and transition zone (Marsch, 2018), and yet most research on coronal holes is concerned only with their manifestations and characteristics in the upper atmosphere (e.g. Banerjee et al, , 2020Banerjee, Pérez-Suárez, and Doyle, 2009;Banerjee, 2010;Banerjee, Gupta, and Teriaca, 2011;Krishna Prasad, Banerjee, and Van Doorsselaere, 2014), while works studying the lower atmosphere under coronal holes have not been as numerous in the last decade (Kobanov, Makarchik, and Sklyar, 2003;De Pontieu et al, 2007;Teplitskaya, Turova, and Ozhogina, 2007;Kobanov and Sklyar, 2007;Teplitskaya, Turova, and Ozhogina, 2010;Tian et al, 2014b;Zubkova et al, 2014;Grigoryeva, Turova, and Ozhogina, 2016). With this article, we try to contribute to this field by analyzing the oscillations we observe in the lower atmosphere under two coronal holes.…”

Section: Introductionmentioning

confidence: 99%

Propagating Oscillations in the Lower Atmosphere Under Coronal Holes

et al. 2021

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The subject of this study is oscillations in the lower atmosphere in coronal-hole regions, where the conditions are favorable for propagation between the atmospheric layers. Based on spectroscopic observations in photospheric and chromospheric lines, we analyzed the features of the oscillations that show signs of propagation between the layers of the solar atmosphere. Using the cross-spectrum wavelet algorithm, we found that both chromospheric and photospheric signals under coronal holes share a range of significant oscillations with periods around five minutes, while the signals outside coronal holes show no mutual oscillations in the photosphere and chromosphere. The phase shift between the layers indicates a predominantly upward propagation with partial presence of standing waves. We have also tested the assumption that the torsional Alfvén waves propagating in the corona originate in the lower atmosphere. However, the observed line-width oscillations, although similar in period to the Alfvén waves observed earlier in the corona of open-field regions, seem to be associated with other magnetohydrodynamic (MHD) modes. If we assume that the oscillations that we observed are related to Alfvén waves, then perhaps this is only through the mechanisms of the slow-MHD-wave transformation.

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“…Sources of the solar wind are located at the heights of the chromosphere and the transition zone (Marsch 2018), and yet most of the research on coronal holes concerns only their manifestations and characteristics in the upper atmosphere (e.g. Banerjee et al 2009bBanerjee et al , 2020Banerjee et al , 2009aBanerjee 2010;Banerjee et al 2011;Krishna Prasad et al 2014), while the works studying the lower atmosphere under coronal holes have not been as numerous in the recent decade (Kobanov et al 2003;De Pontieu et al 2007;Teplitskaya et al 2007;Kobanov & Sklyar 2007;Teplitskaya et al 2010;Tian et al 2014a;Zubkova et al 2014;Grigoryeva et al 2016). With this article, we try to contribute to this area by analyzing the oscillations that we observe in the lower atmosphere under two coronal holes.…”

Section: Introductionmentioning

confidence: 99%

Propagating Oscillations in the Lower Atmosphere under Coronal Holes

Chelpanov,

Kobanov,

Chelpanov

et al. 2021

Preprint

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The subject of this study is oscillations in the lower atmosphere in coronal-hole regions, where the conditions are favorable for propagation between the atmospheric layers. Based on spectroscopic observations in photospheric and chromospheric lines, we analysed the features of the oscillations that show signs of propagation between layers of the solar atmosphere. Using the cross-spectrum wavelet algorithm, we found that both chromospheric and photospheric signals under coronal holes share a range of significant oscillations of periods around five minutes, while the signals outside of coronal holes show no mutual oscillations in the photosphere and chromosphere. The phase shift between the layers indicates a predominantly upward propagation with partial presence of standing waves. We also tested the assumption that torsional Alfvén waves propagating in the corona originate in the lower atmosphere. However, the observed line-width oscillations, although similar in period to the Alfvén waves observed earlier in the corona of open-field regions, seem to be associated with other MHD modes. If we assume that the oscillations that we observed are related to Alfvén waves, then perhaps this is only through the mechanisms of the slow MHD wave transformation.

show abstract

Periodic processes and plasma motions in solar coronal holes

Cited by 9 publications

References 18 publications

Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

Comparing the main oscillation characteristics in the solar chromosphere and magnetosphere based on studies made in ISTP SB RAS

Propagating Oscillations in the Lower Atmosphere Under Coronal Holes

Propagating Oscillations in the Lower Atmosphere under Coronal Holes

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