The solar X-ray corona
Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical pa...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Golub, L. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1996 |
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| Schlagwörter: |
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| Anmerkung: |
© Kluwer Academic Publishers 1996 |
|---|
| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 237(1996), 1-2 vom: März, Seite 33-48 |
|---|---|
| Übergeordnetes Werk: |
volume:237 ; year:1996 ; number:1-2 ; month:03 ; pages:33-48 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF02424425 |
|---|
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OLC206620692X |
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| 520 | |a Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. | ||
| 650 | 4 | |a Magnetic Field | |
| 650 | 4 | |a Spatial Scale | |
| 650 | 4 | |a Physical Parameter | |
| 650 | 4 | |a Emergence Pattern | |
| 650 | 4 | |a Magnetic Flux | |
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10.1007/BF02424425 doi (DE-627)OLC206620692X (DE-He213)BF02424425-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Golub, L. verfasserin aut The solar X-ray corona 1996 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1996 Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. Magnetic Field Spatial Scale Physical Parameter Emergence Pattern Magnetic Flux Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 237(1996), 1-2 vom: März, Seite 33-48 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:237 year:1996 number:1-2 month:03 pages:33-48 https://doi.org/10.1007/BF02424425 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4027 GBV_ILN_4046 AR 237 1996 1-2 03 33-48 |
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10.1007/BF02424425 doi (DE-627)OLC206620692X (DE-He213)BF02424425-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Golub, L. verfasserin aut The solar X-ray corona 1996 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1996 Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. Magnetic Field Spatial Scale Physical Parameter Emergence Pattern Magnetic Flux Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 237(1996), 1-2 vom: März, Seite 33-48 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:237 year:1996 number:1-2 month:03 pages:33-48 https://doi.org/10.1007/BF02424425 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4027 GBV_ILN_4046 AR 237 1996 1-2 03 33-48 |
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10.1007/BF02424425 doi (DE-627)OLC206620692X (DE-He213)BF02424425-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Golub, L. verfasserin aut The solar X-ray corona 1996 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1996 Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. Magnetic Field Spatial Scale Physical Parameter Emergence Pattern Magnetic Flux Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 237(1996), 1-2 vom: März, Seite 33-48 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:237 year:1996 number:1-2 month:03 pages:33-48 https://doi.org/10.1007/BF02424425 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4027 GBV_ILN_4046 AR 237 1996 1-2 03 33-48 |
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10.1007/BF02424425 doi (DE-627)OLC206620692X (DE-He213)BF02424425-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Golub, L. verfasserin aut The solar X-ray corona 1996 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1996 Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. Magnetic Field Spatial Scale Physical Parameter Emergence Pattern Magnetic Flux Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 237(1996), 1-2 vom: März, Seite 33-48 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:237 year:1996 number:1-2 month:03 pages:33-48 https://doi.org/10.1007/BF02424425 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4027 GBV_ILN_4046 AR 237 1996 1-2 03 33-48 |
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10.1007/BF02424425 doi (DE-627)OLC206620692X (DE-He213)BF02424425-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Golub, L. verfasserin aut The solar X-ray corona 1996 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1996 Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. Magnetic Field Spatial Scale Physical Parameter Emergence Pattern Magnetic Flux Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 237(1996), 1-2 vom: März, Seite 33-48 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:237 year:1996 number:1-2 month:03 pages:33-48 https://doi.org/10.1007/BF02424425 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4027 GBV_ILN_4046 AR 237 1996 1-2 03 33-48 |
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Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. © Kluwer Academic Publishers 1996 |
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Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. © Kluwer Academic Publishers 1996 |
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Abstract The solar corona, and the coronae of solar-type stars, consist of a low-density magnetized plasma at temperatures exceeding $ 10^{6} $ K. The primary coronal emission is therefore in the UV and soft x-ray range. The observed close connection between solar magnetic fields and the physical parameters of the corona implies a fundamental role for the magnetic field in coronal structuring and dynamics. Variability of the corona occurs on all temporal and spatial scales—at one extreme, as the result of plasma instabilities, and at the other extreme driven by the global magnetic flux emergence patterns of the solar cycle. © Kluwer Academic Publishers 1996 |
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The solar X-ray corona |
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https://doi.org/10.1007/BF02424425 |
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| doi_str |
10.1007/BF02424425 |
| up_date |
2024-07-04T03:59:02.261Z |
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1803619446049210368 |
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7.4020357 |