Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb
Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Alissandrakis, C. E. [verfasserIn] Valentino, A. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2019 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 294(2019), 7 vom: 23. Juli |
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| Übergeordnetes Werk: |
volume:294 ; year:2019 ; number:7 ; day:23 ; month:07 |
| Links: |
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| DOI / URN: |
10.1007/s11207-019-1486-7 |
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| Katalog-ID: |
SPR017776597 |
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| 100 | 1 | |a Alissandrakis, C. E. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
| 264 | 1 | |c 2019 | |
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| 520 | |a Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona | ||
| 650 | 4 | |a Chromosphere, quiet |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Transition region |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Corona, quiet |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Corona, models |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Valentino, A. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Solar physics |d Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 |g 294(2019), 7 vom: 23. Juli |w (DE-627)269019162 |w (DE-600)1473830-2 |x 1573-093X |7 nnns |
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10.1007/s11207-019-1486-7 doi (DE-627)SPR017776597 (SPR)s11207-019-1486-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Alissandrakis, C. E. verfasserin aut Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 Valentino, A. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 294(2019), 7 vom: 23. Juli (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:294 year:2019 number:7 day:23 month:07 https://dx.doi.org/10.1007/s11207-019-1486-7 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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 39.51 ASE AR 294 2019 7 23 07 |
| spelling |
10.1007/s11207-019-1486-7 doi (DE-627)SPR017776597 (SPR)s11207-019-1486-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Alissandrakis, C. E. verfasserin aut Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 Valentino, A. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 294(2019), 7 vom: 23. Juli (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:294 year:2019 number:7 day:23 month:07 https://dx.doi.org/10.1007/s11207-019-1486-7 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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 39.51 ASE AR 294 2019 7 23 07 |
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10.1007/s11207-019-1486-7 doi (DE-627)SPR017776597 (SPR)s11207-019-1486-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Alissandrakis, C. E. verfasserin aut Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 Valentino, A. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 294(2019), 7 vom: 23. Juli (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:294 year:2019 number:7 day:23 month:07 https://dx.doi.org/10.1007/s11207-019-1486-7 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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 39.51 ASE AR 294 2019 7 23 07 |
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10.1007/s11207-019-1486-7 doi (DE-627)SPR017776597 (SPR)s11207-019-1486-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Alissandrakis, C. E. verfasserin aut Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 Valentino, A. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 294(2019), 7 vom: 23. Juli (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:294 year:2019 number:7 day:23 month:07 https://dx.doi.org/10.1007/s11207-019-1486-7 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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 39.51 ASE AR 294 2019 7 23 07 |
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10.1007/s11207-019-1486-7 doi (DE-627)SPR017776597 (SPR)s11207-019-1486-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Alissandrakis, C. E. verfasserin aut Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 Valentino, A. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 294(2019), 7 vom: 23. Juli (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:294 year:2019 number:7 day:23 month:07 https://dx.doi.org/10.1007/s11207-019-1486-7 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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 39.51 ASE AR 294 2019 7 23 07 |
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The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. 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Alissandrakis, C. E. |
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Alissandrakis, C. E. ddc 530 bkl 39.51 misc Chromosphere, quiet misc Transition region misc Corona, quiet misc Corona, models Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
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530 ASE 39.51 bkl Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb Chromosphere, quiet (dpeaa)DE-He213 Transition region (dpeaa)DE-He213 Corona, quiet (dpeaa)DE-He213 Corona, models (dpeaa)DE-He213 |
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Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
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Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
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structure of the transition region and the low corona from trace and sdo observations near the limb |
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Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
| abstract |
Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona |
| abstractGer |
Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona |
| abstract_unstemmed |
Abstract We examined the structure near the solar limb in TRACE images of the continuum and in the 1600 and 171 Å bands as well as in SDO images in the continuum (from HMI) and all AIA bands. The images in different wavelength bands were carefully coaligned by using the position of Mercury for TRACE and Venus for SDO during their transit in front of the solar disk in 1999 and 2012, respectively. Chromospheric absorbing structures in the TRACE 171-Å band are best visible $ 7^{′′} $ above the white-light limb, very close to the inner limb, defined as the inflection point of the rising part of the center-to-limb intensity variation. They are correlated with, but are not identical to, spicules in emission, seen in the 1600-Å band. Similar results were obtained from AIA and SOT images. Tall spicules in 304 Å are not associated with any absorption in the higher temperature bands. Performing azimuthal averaging of the intensity over $ 15^{∘} $ sectors near the N, S, E and W limbs, we measured the height of the limb and of the peak intensity in all AIA bands. We found that the inner limb height in the transition region AIA bands increases with wavelength, consistent with a bound–free origin of the absorption from neutral H and He. From that we computed the column density and the density of neutral hydrogen as a function of height. We estimated a height of $(2300\pm 500)~\mbox{km}$ for the base of the transition region. Finally, we measured the scale height of the AIA emission of the corona and associated it with the temperature; we deduced a value of $(1.24\pm 0.25)\times 10^{6}~\mbox{K}$ for the polar corona |
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| container_issue |
7 |
| title_short |
Structure of the Transition Region and the Low Corona from TRACE and SDO Observations Near the Limb |
| url |
https://dx.doi.org/10.1007/s11207-019-1486-7 |
| remote_bool |
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| author2 |
Valentino, A. |
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Valentino, A. |
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| doi_str |
10.1007/s11207-019-1486-7 |
| up_date |
2024-07-03T15:08:25.149Z |
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| score |
7.4020357 |