Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts
Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obta...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Croom, David L. [verfasserIn] |
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| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1971 |
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| Schlagwörter: |
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| Anmerkung: |
© D. Reidel Publishing Company 1971 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 19(1971), 1 vom: Aug., Seite 171-185 |
|---|---|
| Übergeordnetes Werk: |
volume:19 ; year:1971 ; number:1 ; month:08 ; pages:171-185 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00148832 |
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| Katalog-ID: |
OLC2033525368 |
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| 520 | |a Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. | ||
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10.1007/BF00148832 doi (DE-627)OLC2033525368 (DE-He213)BF00148832-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Croom, David L. verfasserin aut Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. Microwave Power Density Energy Range Time Characteristic Maximum Power Enthalten in Solar physics Kluwer Academic Publishers, 1967 19(1971), 1 vom: Aug., Seite 171-185 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:19 year:1971 number:1 month:08 pages:171-185 https://doi.org/10.1007/BF00148832 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 19 1971 1 08 171-185 |
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10.1007/BF00148832 doi (DE-627)OLC2033525368 (DE-He213)BF00148832-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Croom, David L. verfasserin aut Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. Microwave Power Density Energy Range Time Characteristic Maximum Power Enthalten in Solar physics Kluwer Academic Publishers, 1967 19(1971), 1 vom: Aug., Seite 171-185 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:19 year:1971 number:1 month:08 pages:171-185 https://doi.org/10.1007/BF00148832 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 19 1971 1 08 171-185 |
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10.1007/BF00148832 doi (DE-627)OLC2033525368 (DE-He213)BF00148832-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Croom, David L. verfasserin aut Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. Microwave Power Density Energy Range Time Characteristic Maximum Power Enthalten in Solar physics Kluwer Academic Publishers, 1967 19(1971), 1 vom: Aug., Seite 171-185 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:19 year:1971 number:1 month:08 pages:171-185 https://doi.org/10.1007/BF00148832 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 19 1971 1 08 171-185 |
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10.1007/BF00148832 doi (DE-627)OLC2033525368 (DE-He213)BF00148832-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Croom, David L. verfasserin aut Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. Microwave Power Density Energy Range Time Characteristic Maximum Power Enthalten in Solar physics Kluwer Academic Publishers, 1967 19(1971), 1 vom: Aug., Seite 171-185 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:19 year:1971 number:1 month:08 pages:171-185 https://doi.org/10.1007/BF00148832 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 19 1971 1 08 171-185 |
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10.1007/BF00148832 doi (DE-627)OLC2033525368 (DE-He213)BF00148832-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Croom, David L. verfasserin aut Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. Microwave Power Density Energy Range Time Characteristic Maximum Power Enthalten in Solar physics Kluwer Academic Publishers, 1967 19(1971), 1 vom: Aug., Seite 171-185 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:19 year:1971 number:1 month:08 pages:171-185 https://doi.org/10.1007/BF00148832 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 19 1971 1 08 171-185 |
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Croom, David L. |
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forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts |
| title_auth |
Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts |
| abstract |
Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. © D. Reidel Publishing Company 1971 |
| abstractGer |
Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. © D. Reidel Publishing Company 1971 |
| abstract_unstemmed |
Abstract A survey of the main characteristics of solar microwave bursts in relation to their usefulness for indicating the intensity of associated solar proton emissions suggests that time parameters give much better results than intensity or spectrum parameters. In particular, best results are obtained by using the effective, or mean, burst duration defined by $$T_M = 1/P_{max} \int_0^T {P(t)dt} $$ where T is the overall burst duration, P is the power density at time T, and Pmax is the maximum power density. For proton energies > 10 MeV the proton flux Np is given approximately by Np = 0.034 TM3 particles $ ster^{−1} $ $ cm^{−2} $ $ s^{−1} $, where Tm is in minutes, with a correlation factor of 0.8. Corresponding coefficients have been derived for a number of energy ranges. Using this parameter solar proton warnings and intensity estimates can be made with observations at only one frequency, preferably in the range 5–20 GHz. © D. Reidel Publishing Company 1971 |
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Forecasting the intensity of solar proton events from the time characteristics of solar microwave bursts |
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