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Кобанов, Н. И.; Makarchik, D. V.; Sklyar, A. A.

doi:10.1023/a:1027301101788

Cited by 14 publications

(9 citation statements)

References 6 publications

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“…Investigating the oscillations at the base of coronal holes helps to better understand the nature of the physical processes in them. The observational manifestations of wave processes in the lower layers of CHs have been actively studied by various methods with ground-based instruments for the last two decades (Stepanian 1995; Malanushenko et al 1997Malanushenko et al , 1999Kobanov 2001;Kobanov et al 2003 ) are devoted to the study of propagating waves in the upper layers of CHs. At the same time, it is obvious that particular attention should be given to the Alfv´en waves, which are distinguished by weak damping and, as a consequence, are capable of propagating to considerable distances (Nakariakov et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Periodic variations of the Ba II 4554 Å and Ca II 8542 Å line profiles in coronal holes

2016

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The oscillations of the half-width of the Ba II 4554Å and Ca II 8542Å spectral lines have been analyzed using observations at the base of solar coronal holes (CHs). The observed variations (∼50 mÅ for Ca II and ∼4 mÅ for Ba II) exceed considerably the thermal broadenings of these lines calculated from the measured intensity oscillations, suggesting their nonthermal nature. We point out a number of observational facts that hamper an unambiguous interpretation of the periodic Ba II and Ca II profile variations solely by the manifestation of torsional Alfv´en waves in the lower solar atmosphere.

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Section: Introductionmentioning

confidence: 99%

Periodic variations of the Ba II 4554 Å and Ca II 8542 Å line profiles in coronal holes

2016

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“…In the five-minute range, they found signs of propagating waves. Kobanov et al [2003] observed LOS velocity oscillations with frequencies of 1 mHz and lower along with three-and five-minute oscillations above coronal holes. Anfinogentov et al [2010], using the 171 Å coronal line, observed longitudinal and transverse oscillations predominantly with 15-30 min periods in loops located in a coronal hole.…”

Section: Oscillations On the Sunmentioning

confidence: 85%

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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“…Chromospheric oscillations have been detected in 1700, 1600, 1216, and 1550 Å wavelengths, with most frequent periods of 283 s in the network, which was also found to have a greater oscillatory power than the internetwork (McAteer et al 2004;McIntosh & Smillie 2004). They were also seen in coronal holes (Kobanov et al 2003;). Oscillations with periods between 100 and 500 s have also been discovered in dark mottles and dark grains, which were interpreted as the same structures, the only difference being their respective inclinations to the line of sight (Tziotziou et al 2003.…”

Section: Chromoseismologymentioning

confidence: 94%