The dynamics of chromospheric spicules

Papushev, P. G.; Salakhutdinov, R. T.

doi:10.1007/bf00777840

Cited by 3 publications

(7 citation statements)

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“…Indeed, the oscillations of Doppler velocity in spicules with similar periods were reported by Zaqarashvili et al (2007). If the velocity of the kink wave is polarized in the plane of observation, then it results in the Doppler shift of the observed spectral line (Nikolsky and Sazanov (1967);Pasachoff et al (1968); Kulidzanishvili and Nikolsky (1978); Gadzhiev and Nikolsky (1982); Kulidzanishvili and Zhugzhda (1983); Hasan and Keil (1984); Papushev and Salakhutdinov (1994); ; Kukhianidze et al (2006); Zaqarashvili et al (2007)). However, if the velocity is polarized in the perpendicular plane then it results the visible displacement of spicule axis along the limb (Nikolsky and Sazanov (1967); Nikolsky and Platova (1971); Gadzhiev and Nikolsky (1982); Papushev and Salakhutdinov (1994)).…”

Section: Mhd Kink Wavesmentioning

confidence: 59%

“…3.9 Papushev and Salakhutdinov (1994) Observations were carried out with the 53 Lyot coronagraph of Sayan Observatory located near Irkutsk (Russia). The spectroscopic time series in different spectral lines varied from several minutes to hours with an excellent temporal resolution of 10-20 s. The spatial resolution of observations was better than 1 arcsec.…”

Section: Kulidzanishvili and Zhugzhdamentioning

confidence: 99%

“…Oscillations are more frequently observed in the Doppler velocity, which points towards transversal motions as the observations are performed at the solar limb. The longitudinal velocity component may also take a part in shaping the Doppler velocity oscillations as spicules are Weart (1970) random random Hα Nikolsky and Platova (1971) 50-70 s Hα Kulidzanishvili and Nikolsky (1978) 3-7 min 3-7 min Hα Gadzhiev and Nikolsky (1982) 3-6 min 3-6 min Hα Kulidzanishvili and Zhugzhda (1983) 5-min 5-min Hα Hasan and Keil (1984) 2-3 min > 300 km/s Hα Papushev and Salakhutdinov (1994) 80-120 s 80-120 80-120 > 300 km/s Hα 5-min 5-min EUV Kukhianidze et al (2006) 35-70 s ∼ 80 km/s Hα Zaqarashvili et al (2007) 30-110 s ∼ 110 km/s Hα De Pontieu et al (2007a) 100-500 s 50-200 km/s Ca II generally tilted away from the vertical. However, the transverse component seems to be the more important and determinant component in these oscillations as the visible displacement along the limb is also frequently reported.…”

Section: Summary Of Observed Oscillatory Phenomenamentioning

confidence: 99%

“…Hasan and Keil (1984) suggested the propagation of signals from lower to higher heights with an estimated velocity of more than 300 km s −1 . Papushev and Salakhutdinov (1994) studied the phase delays of fluctuations at different heights and also concluded that the propagation speeds should exceed 300 km s −1 . However, it must be noted that a standing oscillation pattern may also be responsible to explain these phenomena.…”

Section: Propagationmentioning

confidence: 99%

“…Temporal variations of Hα line profile parameters and the line-of-sight velocity of spicules at different heights, adapted fromPapushev and Salakhutdinov (1994). The solid line corresponds to the height of 5 Mm and the dashed line to 8 Mm above the solar limb, respectively.Temporal variations ofHα line profile parameters and line-of-sight velocity for one of spicules at two different heights are shown on Fig.8.…”

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confidence: 99%

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Oscillations and Waves in Solar Spicules

2009

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Since their discovery, spicules have attracted increased attention as energy/mass bridges between the dense and dynamic photosphere and the tenuous hot solar corona. Mechanical energy of photospheric random and coherent motions can be guided by magnetic field lines, spanning from the interior to the upper parts of the solar atmosphere, in the form of waves and oscillations. Since spicules are one of the most pronounced features of the chromosphere, the energy transport they participate in can be traced by the observations of their oscillatory motions. Oscillations in spicules have been observed for a long time. However the recent high-resolution and high-cadence space and ground based facilities with superb spatial, temporal and spectral capacities brought new aspects in the research of spicule dynamics. Here we review the progress made in imaging and spectroscopic observations of waves and oscillations in spicules. The observations are accompanied by a discussion on theoretical modelling and interpretations of these oscillations. Finally, we embark on the recent developments made on the presence and role of Alfvén and kink waves in spicules. We also address the extensive debate made on the Alfvén versus kink waves in the context of the explanation of the observed transverse oscillations of spicule axes.

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Section: Mhd Kink Wavesmentioning

confidence: 59%

Section: Kulidzanishvili and Zhugzhdamentioning

confidence: 99%

Section: Summary Of Observed Oscillatory Phenomenamentioning

confidence: 99%

Section: Propagationmentioning

confidence: 99%

mentioning

confidence: 99%

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Oscillations and Waves in Solar Spicules

2009

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Propagating wave in active region-loops, located over the solar disk observed by the Interface Region Imaging Spectrograph

Zhang

Hou

Zhang

2018

A&A

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Context.Aims. We aim to ascertain the physical parameters of a propagating wave over the solar disk detected by the Interface Region Imaging Spectrograph (IRIS). Methods. Using imaging data from the IRIS and the Solar Dynamic Observatory (SDO), we tracked bright spots to determine the parameters of a propagating transverse wave in active region (AR) loops triggered by activation of a filament. Deriving the Doppler velocity of Si IV line from spectral observations of IRIS, we have determined the rotating directions of active region loops which are relevant to the wave. Results. On 2015 December 19, a filament was located on the polarity inversion line of the NOAA AR 12470. The filament was activated and then caused a C1.1 two-ribbon flare. Between the flare ribbons, two rotation motions of a set of bright loops were observed to appear in turn with opposite directions. Following the end of the second rotation, a propagating wave and an associated transverse oscillation were detected in these bright loops. In 1400 Å channel, there was bright material flowing along the loops in a wave-like manner, with a period of ∼128 s and a mean amplitude of ∼880 km. For the transverse oscillation, we tracked a given loop and determine the transverse positions of the tracking loop in a limited longitudinal range. In both of 1400 Å and 171 Å channels, approximately four periods are distinguished during the transverse oscillation. The mean period of the oscillation is estimated as ∼143 s and the displacement amplitude as between ∼1370 km and ∼690 km. We interpret these oscillations as a propagating kink wave and obtain its speed of ∼1400 km s −1 . Conclusions. Our observations reveal that a flare associated with filament activation could trigger a kink propagating wave in active region loops over the solar disk.

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