Evidences to the pulse like origin of double spicules based on Hinode/SOT observations
Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The lengt...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Ebadi, H. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2013 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968, 348(2013), 1 vom: 24. Juli, Seite 11-15 |
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| Übergeordnetes Werk: |
volume:348 ; year:2013 ; number:1 ; day:24 ; month:07 ; pages:11-15 |
| Links: |
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| DOI / URN: |
10.1007/s10509-013-1559-2 |
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| Katalog-ID: |
SPR010594078 |
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| 245 | 1 | 0 | |a Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
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| 520 | |a Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. | ||
| 650 | 4 | |a Sun: spicules |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Spicule formation |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Double spicules |7 (dpeaa)DE-He213 | |
| 773 | 0 | 8 | |i Enthalten in |t Astrophysics and space science |d Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 |g 348(2013), 1 vom: 24. Juli, Seite 11-15 |w (DE-627)268755868 |w (DE-600)1472548-4 |x 1572-946X |7 nnns |
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10.1007/s10509-013-1559-2 doi (DE-627)SPR010594078 (SPR)s10509-013-1559-2-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Ebadi, H. verfasserin aut Evidences to the pulse like origin of double spicules based on Hinode/SOT observations 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 348(2013), 1 vom: 24. Juli, Seite 11-15 (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:348 year:2013 number:1 day:24 month:07 pages:11-15 https://dx.doi.org/10.1007/s10509-013-1559-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 348 2013 1 24 07 11-15 |
| spelling |
10.1007/s10509-013-1559-2 doi (DE-627)SPR010594078 (SPR)s10509-013-1559-2-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Ebadi, H. verfasserin aut Evidences to the pulse like origin of double spicules based on Hinode/SOT observations 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 348(2013), 1 vom: 24. Juli, Seite 11-15 (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:348 year:2013 number:1 day:24 month:07 pages:11-15 https://dx.doi.org/10.1007/s10509-013-1559-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 348 2013 1 24 07 11-15 |
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10.1007/s10509-013-1559-2 doi (DE-627)SPR010594078 (SPR)s10509-013-1559-2-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Ebadi, H. verfasserin aut Evidences to the pulse like origin of double spicules based on Hinode/SOT observations 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 348(2013), 1 vom: 24. Juli, Seite 11-15 (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:348 year:2013 number:1 day:24 month:07 pages:11-15 https://dx.doi.org/10.1007/s10509-013-1559-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 348 2013 1 24 07 11-15 |
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10.1007/s10509-013-1559-2 doi (DE-627)SPR010594078 (SPR)s10509-013-1559-2-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Ebadi, H. verfasserin aut Evidences to the pulse like origin of double spicules based on Hinode/SOT observations 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 348(2013), 1 vom: 24. Juli, Seite 11-15 (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:348 year:2013 number:1 day:24 month:07 pages:11-15 https://dx.doi.org/10.1007/s10509-013-1559-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 348 2013 1 24 07 11-15 |
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10.1007/s10509-013-1559-2 doi (DE-627)SPR010594078 (SPR)s10509-013-1559-2-e DE-627 ger DE-627 rakwb eng 520 530 620 ASE 39.00 bkl 39.22 bkl Ebadi, H. verfasserin aut Evidences to the pulse like origin of double spicules based on Hinode/SOT observations 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 Enthalten in Astrophysics and space science Dordrecht [u.a.] : Springer Science + Business Media B.V, 1968 348(2013), 1 vom: 24. Juli, Seite 11-15 (DE-627)268755868 (DE-600)1472548-4 1572-946X nnns volume:348 year:2013 number:1 day:24 month:07 pages:11-15 https://dx.doi.org/10.1007/s10509-013-1559-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE 39.22 ASE AR 348 2013 1 24 07 11-15 |
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Enthalten in Astrophysics and space science 348(2013), 1 vom: 24. Juli, Seite 11-15 volume:348 year:2013 number:1 day:24 month:07 pages:11-15 |
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Enthalten in Astrophysics and space science 348(2013), 1 vom: 24. Juli, Seite 11-15 volume:348 year:2013 number:1 day:24 month:07 pages:11-15 |
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| author |
Ebadi, H. |
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Ebadi, H. ddc 520 bkl 39.00 bkl 39.22 misc Sun: spicules misc Spicule formation misc Double spicules Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
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520 530 620 ASE 39.00 bkl 39.22 bkl Evidences to the pulse like origin of double spicules based on Hinode/SOT observations Sun: spicules (dpeaa)DE-He213 Spicule formation (dpeaa)DE-He213 Double spicules (dpeaa)DE-He213 |
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ddc 520 bkl 39.00 bkl 39.22 misc Sun: spicules misc Spicule formation misc Double spicules |
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ddc 520 bkl 39.00 bkl 39.22 misc Sun: spicules misc Spicule formation misc Double spicules |
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Elektronische Aufsätze Aufsätze Elektronische Ressource |
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Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
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Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
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Ebadi, H. |
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Astrophysics and space science |
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Elektronische Aufsätze |
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Ebadi, H. |
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10.1007/s10509-013-1559-2 |
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520 530 620 |
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evidences to the pulse like origin of double spicules based on hinode/sot observations |
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Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
| abstract |
Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. |
| abstractGer |
Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. |
| abstract_unstemmed |
Abstract We analyze the time series of Hα line obtained from Hinode/SOT on the solar limb. The wavelet analysis shows that there are nice correlations between dynamical properties of the two parts of a double spicule. The dominant periods for height variations are estimated ∼90 and ∼180 s. The length of two parts of the spicule oscillates with the period of around ∼180 s. The mean distance between two parts of the spicule has a periodical treatment with the period of ∼90 s. Our results show that the strong pulses may lead to the quasi periodic rising of chromospheric plasma into the lower corona in the form of spicules. The periodicity may result from the nonlinear wake behind the pulse in the stratified atmosphere. |
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| title_short |
Evidences to the pulse like origin of double spicules based on Hinode/SOT observations |
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https://dx.doi.org/10.1007/s10509-013-1559-2 |
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| doi_str |
10.1007/s10509-013-1559-2 |
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2024-07-03T17:06:36.090Z |
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| score |
7.4009724 |