Quasi-periodic variations in Doppler velocities of Hα spicules
Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Khutshishvili, E. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2014 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science+Business Media Dordrecht 2014 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Springer Netherlands, 1968, 354(2014), 2 vom: 15. Okt., Seite 259-266 |
|---|---|
| Übergeordnetes Werk: |
volume:354 ; year:2014 ; number:2 ; day:15 ; month:10 ; pages:259-266 |
| Links: |
|---|
| DOI / URN: |
10.1007/s10509-014-2100-y |
|---|
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OLC206627674X |
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| 520 | |a Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. | ||
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| 700 | 1 | |a Kakhiani, V. |4 aut | |
| 700 | 1 | |a Khutsishvili, D. |4 aut | |
| 700 | 1 | |a Sikharulidze, M. |4 aut | |
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10.1007/s10509-014-2100-y doi (DE-627)OLC206627674X (DE-He213)s10509-014-2100-y-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Khutshishvili, E. verfasserin aut Quasi-periodic variations in Doppler velocities of Hα spicules 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. Solar spicules Kulidzanishvili, V. aut Kvernadze, T. aut Zaqarashvili, T. V. aut Kakhiani, V. aut Khutsishvili, D. aut Sikharulidze, M. aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 354(2014), 2 vom: 15. Okt., Seite 259-266 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:354 year:2014 number:2 day:15 month:10 pages:259-266 https://doi.org/10.1007/s10509-014-2100-y lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 354 2014 2 15 10 259-266 |
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10.1007/s10509-014-2100-y doi (DE-627)OLC206627674X (DE-He213)s10509-014-2100-y-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Khutshishvili, E. verfasserin aut Quasi-periodic variations in Doppler velocities of Hα spicules 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. Solar spicules Kulidzanishvili, V. aut Kvernadze, T. aut Zaqarashvili, T. V. aut Kakhiani, V. aut Khutsishvili, D. aut Sikharulidze, M. aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 354(2014), 2 vom: 15. Okt., Seite 259-266 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:354 year:2014 number:2 day:15 month:10 pages:259-266 https://doi.org/10.1007/s10509-014-2100-y lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 354 2014 2 15 10 259-266 |
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10.1007/s10509-014-2100-y doi (DE-627)OLC206627674X (DE-He213)s10509-014-2100-y-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Khutshishvili, E. verfasserin aut Quasi-periodic variations in Doppler velocities of Hα spicules 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. Solar spicules Kulidzanishvili, V. aut Kvernadze, T. aut Zaqarashvili, T. V. aut Kakhiani, V. aut Khutsishvili, D. aut Sikharulidze, M. aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 354(2014), 2 vom: 15. Okt., Seite 259-266 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:354 year:2014 number:2 day:15 month:10 pages:259-266 https://doi.org/10.1007/s10509-014-2100-y lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 354 2014 2 15 10 259-266 |
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10.1007/s10509-014-2100-y doi (DE-627)OLC206627674X (DE-He213)s10509-014-2100-y-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Khutshishvili, E. verfasserin aut Quasi-periodic variations in Doppler velocities of Hα spicules 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. Solar spicules Kulidzanishvili, V. aut Kvernadze, T. aut Zaqarashvili, T. V. aut Kakhiani, V. aut Khutsishvili, D. aut Sikharulidze, M. aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 354(2014), 2 vom: 15. Okt., Seite 259-266 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:354 year:2014 number:2 day:15 month:10 pages:259-266 https://doi.org/10.1007/s10509-014-2100-y lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 354 2014 2 15 10 259-266 |
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10.1007/s10509-014-2100-y doi (DE-627)OLC206627674X (DE-He213)s10509-014-2100-y-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Khutshishvili, E. verfasserin aut Quasi-periodic variations in Doppler velocities of Hα spicules 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. Solar spicules Kulidzanishvili, V. aut Kvernadze, T. aut Zaqarashvili, T. V. aut Kakhiani, V. aut Khutsishvili, D. aut Sikharulidze, M. aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 354(2014), 2 vom: 15. Okt., Seite 259-266 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:354 year:2014 number:2 day:15 month:10 pages:259-266 https://doi.org/10.1007/s10509-014-2100-y lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 354 2014 2 15 10 259-266 |
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Quasi-periodic variations in Doppler velocities of Hα spicules |
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Quasi-periodic variations in Doppler velocities of Hα spicules |
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Khutshishvili, E. |
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Khutshishvili, E. Kulidzanishvili, V. Kvernadze, T. Zaqarashvili, T. V. Kakhiani, V. Khutsishvili, D. Sikharulidze, M. |
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quasi-periodic variations in doppler velocities of hα spicules |
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Quasi-periodic variations in Doppler velocities of Hα spicules |
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Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. © Springer Science+Business Media Dordrecht 2014 |
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Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. © Springer Science+Business Media Dordrecht 2014 |
| abstract_unstemmed |
Abstract New series of CCD spectral observations of spicules were obtained using 53-cm Lyot coronagraph of Abastumani Astrophysical Observatory (Georgia) at 5500 km height above the solar limb on October 17, 2012 in Hα spectral line. The line-of-sight Doppler velocities of 34 spicules were measured with the cadence of 4.5 s and standard error equal to ±0.3 km/s. Life times of almost all measured spicules were 5–6 min (and longer), therefore they resemble the type I spicules. No short lived structures (similar to type II spicules) were identified during the time series neither inside nor outside the observed spicules. The Doppler velocity time series were processed using Lomb Periodogram Algorithm revealing 4 types of dominating period intervals centered around: 254 s, 136 s, 94 s and 65 s having confidence levels over 95 %. The oscillations with periods around 254 s can be caused by quasi-periodic rebound shocks after the propagation of photospheric pulses. The oscillations with periods around 136 s can be caused by the oscillation of spicules axis at the kink cut-off frequency in gravitationally stratified magnetic tubes. In this case, seismological estimations give the density scale height as 380–540 km for the kink wave speed of 70–100 km/s in spicules. Shorter period oscillations are probably caused by propagating kink waves in spicules. © Springer Science+Business Media Dordrecht 2014 |
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Quasi-periodic variations in Doppler velocities of Hα spicules |
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