Continuous spectral observations of spicules

Khutsishvili, E. V.

doi:10.1007/bf00161355

Cited by 11 publications

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“…The big (53 cm) coronagraph and universal spectrograph of Abastumani Astrophysical Observatory has been used to obtain chromospheric Hα line spectra at different heights (8 heights) above the photosphere (Khutsishvili 1986). Instrumental spectral resolution is 0.04 Å and dispersion 1 Å/mm in Hα.…”

Section: Observationmentioning

confidence: 99%

“…The duration of each height series was 7 s, with the total duration of the observation being 44 min. More details about the observation can be found in Khutsishvili (1986).…”

Section: Observationmentioning

confidence: 99%

“…It is well known that transverse kink waves can be generated in photospheric magnetic tubes by buffeting of granular motions (Roberts 1979;Hollweg 1981;Spruit 1981;Hasan & Kalkofen 1999). Kink waves cause the displacement of the tube axis, therefore their propagation can be traced either by direct observation of the tube displacement along the limb as in Nikolsky & Platova (1971) velocities in spicules has been detected almost 20 years ago by Khutsishvili (1986). Unfortunately, neither observers nor theorists paid attention to the phenomenon which can be simply explained in terms of kink waves.…”

Section: Introductionmentioning

confidence: 99%

“…Unfortunately, neither observers nor theorists paid attention to the phenomenon which can be simply explained in terms of kink waves. In this letter, we reanalyze the height series of Hα spectra obtained by Khutsishvili (1986) and then model the observation as propagating kink waves.…”

Section: Introductionmentioning

confidence: 99%

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Observation of kink waves in solar spicules

Kukhianidze

Zaqarashvili

Khutsishvili

2006

A&A

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Height series of Hα spectra in solar limb spicules obtained with the 53 cm coronagraph of the Abastumani Astrophysical Observatory are analyzed. Each height series covered 8 different heights beginning at 3800 km above the photosphere. The spatial difference between neighboring heights was 1 , consequently ∼3800−8700 km distance above the photosphere has been covered. The total time duration of each height series was 7 s. We found that nearly 20% of measured height series show a periodic spatial distribution of Doppler velocities. We suggest that this spatial periodicity in Doppler velocity is caused by propagating kink waves in spicules. The wave length is found to be ∼3500 km. However the wave length tends to be ∼1000 km at the photosphere due to the height variation of the kink speed. This probably indicates to a granular origin for the waves. The period of waves is estimated to be in the range of 35−70 s. These waves may carry photospheric energy into the corona, therefore can be of importance in coronal heating.

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Section: Observationmentioning

confidence: 99%

“…The duration of each height series was 7 s, with the total duration of the observation being 44 min. More details about the observation can be found in Khutsishvili (1986).…”

Section: Observationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Observation of kink waves in solar spicules

Kukhianidze

Zaqarashvili

Khutsishvili

2006

A&A

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“…Observations were carried out as height series beginning at 3800 km height from the photosphere and upwards (Khutsishvili 1986). The distance between neighboring heights was 1 arc sec, thus the spatial distance 3800-8700 km above the photosphere was covered.…”

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confidence: 99%

Observation of kink waves in solar spicules

et al. 2004

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Abstract. Height series of Doppler observation in Hα and D3 spectral lines of solar spicules obtained by big coronagraph (53 cm) of Abastumani Astrophysical Observatory have been analyzed. Time duration of each height series was 7 s. Totally 8 different heights from the photosphere were covered. Spatial difference between neighboring heights was 1 arc sec. We found the periodic spatial distribution of Doppler velocities during height series in certain spicules. We suggest that the periodic spatial distributions are caused by propagating or standing kink waves. The wave length is found to be in the range 3500-4000 km which probably indicates to the granular origin of the waves.The big 53 cm coronagraph and universal spectrograph have been used to obtain chromospheric H α and D 3 line spectra at different heights (8 heights) from the photosphere (instrumental spectral resolution -0.04 A; dispersion -1 A/mm; spatial resolution -1 arc sec). Observations were carried out as height series beginning at 3800 km height from the photosphere and upwards (Khutsishvili 1986). The distance between neighboring heights was 1 arc sec, thus the spatial distance 3800-8700 km above the photosphere was covered. The exposure time was 0.4 s at lower heights and 0.8 at higher ones for H α . While the exposure time for D 3 was 1 s at lower heights and 2 at higher ones. The total time duration of one height series in H α was 7 s. The consequent height series begins immediately. The total duration of the observation was 44 min. Therefore at one height we have a continuous H α spectra with time intervals of 7 s. Approximately 300 height series was taken.We preliminary analyzed the spatial distribution of Doppler velocities in both spectral lines for certain spicules. Nearly 20% of spicules show periodic spatial distributions of Doppler velocities in height series. The Doppler velocity spatial distributions in two height series of two different spicules in H α spectral line are shown on Fig.1. The periodic spatial distributions are clearly seen. So the transversal velocity in that particular spicules is periodically redistributed with height at certain moment of time (the maximal time difference between the observations at different heights is 7 s, which is the duration of one height series).In order to explain the phenomenon we model spicules as thin magnetic flux tubes anchored in the photosphere and persisted towards the corona. Kink waves propagating along the magnetic tube lead to the oscillation of the tube axis and thus will lead to the periodic spatial and temporal variations of Doppler shift if we observe in the plane of oscillations. So the observed spatial periodicity of Doppler velocity can be caused by either propagating or standing kink waves.If the tube radius is much smaller than the wavelength of waves (i.e. ka << 1, where k is wave number and a is tube radius), then the dispersion relation for the kink waves is (Edwin and Roberts, 1983)

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Identification of D3 and Hα spicules

Khutsishvili

1995

Astron Nachr

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Basing on the analysis of observational material obtained with the 53-cm coronagraph in Abastumani, the author concludes that chromospheric spicules in hydrogen and helium lines are one and the same formation. Besides, it should be noted that, as a result of radial velocity measurements, it was found that hydrogen and helium D3 lines are emitted from different areas of the same spicule.Key words: Sun: chromospheric spicules -D3 and H 1' ines AAA subject classification: 073 IntroductionSpicules, observed in various spectral lines, behave differently; their main characteristics vary. A question arises: are spicules, observed in different spectral lines, one and the same phenomena? To answer this question, it is necessary to receive spectral observational material simultaneously, at least in two spectral lines. The observations must be conducted at the same time at different heights of the chromosphere during a long time interval.Gulyaev (1965) was the first, who pointed at the identity of spicules during the observations of two blending lines, X 3888.65 A of helium and A 3889.65 A of hydrogen. On the photograph, presented in the above mentioned paper, it is seen that, as a rule, "helium" and "hydrogen" spicules coincide within the resolution. Proceeding from this the author presumes that helium and hydrogen may radiate in the same spicules, but in our mind this does not yet mean that hydrogen and helium radiating areas coincide inside of special spicules. Observational techniquesThe question of an identical character of spicules has not been specially studied. Proceeding from this we have conducted observations at one height to obtain spectrograms of spicules in the D3 line of helium and H, of hydrogen with a minimum time interval between the moments of taking the photographs. Due to the high chromatism of the coronagraph, it is not possible to get spectrograms simultaneously without special optics, compensating for chromatic aberration. The large out-of-eclipse coronagraph of the Abastumani Observatory is not equipped with such optics. Observational dataOn 28 and 29 May, 1982 observational material was obtained with the 53-cm coronagraph of the Abastumani Astrophysical Observatory in the helium D3 line and the H, hydrogen line with a time difference between the moments of exposure of 20 sec. The exposure times of the first series of spectrograms on May 28 amount to 1 sec for helium D3 and 0.4 sec for hydrogen H,, while for the second series on May 29 they were 1.5 sec and 0.8 sec, respectively. Observations of the first series of spectrograms were taken at a height of about 4.500 km above the disk and of the second series at a height of 6.000 km. The observations were carried out according to the method, described by Kulijanishvili and Khutsishvili (1981) and Khutsishvili (1986). The exposures were taken just at

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Continuous spectral observations of spicules

Cited by 11 publications

References 8 publications

Observation of kink waves in solar spicules

Observation of kink waves in solar spicules

Observation of kink waves in solar spicules

Identification of D3 and Hα spicules

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