Solar Field Mapping and Dynamo Behavior
We discuss the importance of the Sun’s large-scale magnetic field to the Sun-Planetary environment. This paper narrows its focus down to the motion and evolution of the photospheric large-scale magnetic field which affects many environments throughout this region. For this purpose we utilize a newly...
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| Format: | Article |
| Language: | English |
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Wiley
2012-01-01
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| Series: | Advances in Astronomy |
| Online Access: | http://dx.doi.org/10.1155/2012/923578 |
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| author | Kenneth H. Schatten |
| author_facet | Kenneth H. Schatten |
| author_sort | Kenneth H. Schatten |
| collection | DOAJ |
| description | We discuss the importance of the Sun’s large-scale magnetic field to the Sun-Planetary environment. This paper narrows its focus down to the motion and evolution of the photospheric large-scale magnetic field which affects many environments throughout this region. For this purpose we utilize a newly developed Netlogo cellular automata model. The domain of this algorithmic model is the Sun’s photosphere. Within this computational space are placed two types of entities or agents; one may refer to them as bluebirds and cardinals; the former carries outward magnetic flux and the latter carries out inward magnetic flux. One may simply call them blue and red agents. The agents provide a granularity with discrete changes not present in smooth MHD models;
they undergo three processes: birth, motion, and death within the photospheric domain. We discuss these processes, as well as how we are able to develop a model that restricts its domain to the photosphere and allows the deeper layers to be considered only through boundary conditions. We show the model’s ability to mimic a number of photospheric magnetic phenomena: the solar cycle (11-year) oscillations, the Waldmeier effect, unipolar magnetic regions (e.g. sectors and coronal holes), Maunder minima, and the march/rush to the poles involving the geometry of magnetic field reversals. We also discuss why the Sun sometimes appears as a magnetic monopole, which of course requires no alteration of Maxwell’s equations. |
| format | Article |
| id | doaj-art-1d881cbfaefe489988e2ebe07a303125 |
| institution | Kabale University |
| issn | 1687-7969 1687-7977 |
| language | English |
| publishDate | 2012-01-01 |
| publisher | Wiley |
| record_format | Article |
| series | Advances in Astronomy |
| spelling | doaj-art-1d881cbfaefe489988e2ebe07a3031252025-02-03T01:27:11ZengWileyAdvances in Astronomy1687-79691687-79772012-01-01201210.1155/2012/923578923578Solar Field Mapping and Dynamo BehaviorKenneth H. Schatten0Solar Physics, a.i. solutions, Inc., Suite 215, 10001 Derekwood Lane, Lanham, MD 20706, USAWe discuss the importance of the Sun’s large-scale magnetic field to the Sun-Planetary environment. This paper narrows its focus down to the motion and evolution of the photospheric large-scale magnetic field which affects many environments throughout this region. For this purpose we utilize a newly developed Netlogo cellular automata model. The domain of this algorithmic model is the Sun’s photosphere. Within this computational space are placed two types of entities or agents; one may refer to them as bluebirds and cardinals; the former carries outward magnetic flux and the latter carries out inward magnetic flux. One may simply call them blue and red agents. The agents provide a granularity with discrete changes not present in smooth MHD models; they undergo three processes: birth, motion, and death within the photospheric domain. We discuss these processes, as well as how we are able to develop a model that restricts its domain to the photosphere and allows the deeper layers to be considered only through boundary conditions. We show the model’s ability to mimic a number of photospheric magnetic phenomena: the solar cycle (11-year) oscillations, the Waldmeier effect, unipolar magnetic regions (e.g. sectors and coronal holes), Maunder minima, and the march/rush to the poles involving the geometry of magnetic field reversals. We also discuss why the Sun sometimes appears as a magnetic monopole, which of course requires no alteration of Maxwell’s equations.http://dx.doi.org/10.1155/2012/923578 |
| spellingShingle | Kenneth H. Schatten Solar Field Mapping and Dynamo Behavior Advances in Astronomy |
| title | Solar Field Mapping and Dynamo Behavior |
| title_full | Solar Field Mapping and Dynamo Behavior |
| title_fullStr | Solar Field Mapping and Dynamo Behavior |
| title_full_unstemmed | Solar Field Mapping and Dynamo Behavior |
| title_short | Solar Field Mapping and Dynamo Behavior |
| title_sort | solar field mapping and dynamo behavior |
| url | http://dx.doi.org/10.1155/2012/923578 |
| work_keys_str_mv | AT kennethhschatten solarfieldmappinganddynamobehavior |