Solar Photosphere: Structure, Convection, and Magnetic Fields: Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989
Gespeichert in:
| Weitere Verfasser: | |
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| Format: | Elektronisch E-Book |
| Sprache: | English |
| Veröffentlicht: |
Dordrecht
Springer Netherlands
1990
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| Schriftenreihe: | International Astronomical Union
138 |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Beschreibung: | Solar and stellar photospheres constitute the layers most accessible to observations, forming the interface between the interior and the outside of the stars. The solar atmosphere is a rich physics laboratory, in which the whole spectrum of radiative, dynamical, and magnetic processes that tranfer energy into space can be observed. As the fundamental processes take place on very small spatial scales, we need high resolution observations to explore them. On the other hand the small-scale processes act together to form global properties of the sun, which have their origins in the solar interior. The rapid advances in observational techniques and theoretical modelling over the past decade made it very timely to bring together scientists from east and west to the first IAU Symposium on this topic. The physics of the photosphere involves complicated interactions between magnetic fields, convection, waves, and radiation. During the past decade our understanding of these gener ally small-scale structures and processes has been dramatically advanced. New instrumentations, on ground and in space, have given us new means to study the granular convection. Diagnostic methods in Stokes polarimetry have allowed us to go beyond the limitations of spatial resolution to explore the structure and dynamics of the subarcsec magnetic structures. Extensive numerical simulations of the interaction between convection and magnetic fields using powerful supercomputers are providing deepened physical insight. Granulation, magnetic fields, and dynamo processes are being explored in the photospheres of other stars, guided by our improved understanding of the solar photosphere |
| Beschreibung: | 1 Online-Ressource (XII, 560 p) |
| ISBN: | 9789400910614 9780792305309 |
| DOI: | 10.1007/978-94-009-1061-4 |
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| 245 | 1 | 0 | |a Solar Photosphere: Structure, Convection, and Magnetic Fields |b Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 |c edited by J. O. Stenflo |
| 246 | 1 | 3 | |a Proceedings of the 138th Symposium of the International Astronomical Union, held in Kiev, U.S.S.R., May 15-20, 1989 |
| 264 | 1 | |a Dordrecht |b Springer Netherlands |c 1990 | |
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| 490 | 1 | |a International Astronomical Union |v 138 | |
| 500 | |a Solar and stellar photospheres constitute the layers most accessible to observations, forming the interface between the interior and the outside of the stars. The solar atmosphere is a rich physics laboratory, in which the whole spectrum of radiative, dynamical, and magnetic processes that tranfer energy into space can be observed. As the fundamental processes take place on very small spatial scales, we need high resolution observations to explore them. On the other hand the small-scale processes act together to form global properties of the sun, which have their origins in the solar interior. The rapid advances in observational techniques and theoretical modelling over the past decade made it very timely to bring together scientists from east and west to the first IAU Symposium on this topic. The physics of the photosphere involves complicated interactions between magnetic fields, convection, waves, and radiation. During the past decade our understanding of these gener ally small-scale structures and processes has been dramatically advanced. New instrumentations, on ground and in space, have given us new means to study the granular convection. Diagnostic methods in Stokes polarimetry have allowed us to go beyond the limitations of spatial resolution to explore the structure and dynamics of the subarcsec magnetic structures. Extensive numerical simulations of the interaction between convection and magnetic fields using powerful supercomputers are providing deepened physical insight. Granulation, magnetic fields, and dynamo processes are being explored in the photospheres of other stars, guided by our improved understanding of the solar photosphere | ||
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Datensatz im Suchindex
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| discipline | Physik |
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| illustrated | Not Illustrated |
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| institution | BVB |
| isbn | 9789400910614 9780792305309 |
| language | English |
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| spelling | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 edited by J. O. Stenflo Proceedings of the 138th Symposium of the International Astronomical Union, held in Kiev, U.S.S.R., May 15-20, 1989 Dordrecht Springer Netherlands 1990 1 Online-Ressource (XII, 560 p) txt rdacontent c rdamedia cr rdacarrier International Astronomical Union 138 Solar and stellar photospheres constitute the layers most accessible to observations, forming the interface between the interior and the outside of the stars. The solar atmosphere is a rich physics laboratory, in which the whole spectrum of radiative, dynamical, and magnetic processes that tranfer energy into space can be observed. As the fundamental processes take place on very small spatial scales, we need high resolution observations to explore them. On the other hand the small-scale processes act together to form global properties of the sun, which have their origins in the solar interior. The rapid advances in observational techniques and theoretical modelling over the past decade made it very timely to bring together scientists from east and west to the first IAU Symposium on this topic. The physics of the photosphere involves complicated interactions between magnetic fields, convection, waves, and radiation. During the past decade our understanding of these gener ally small-scale structures and processes has been dramatically advanced. New instrumentations, on ground and in space, have given us new means to study the granular convection. Diagnostic methods in Stokes polarimetry have allowed us to go beyond the limitations of spatial resolution to explore the structure and dynamics of the subarcsec magnetic structures. Extensive numerical simulations of the interaction between convection and magnetic fields using powerful supercomputers are providing deepened physical insight. Granulation, magnetic fields, and dynamo processes are being explored in the photospheres of other stars, guided by our improved understanding of the solar photosphere Physics Astrophysics and Astroparticles Stenflo, J. O. edt International Astronomical Union 138 (DE-604)BV000000364 138 https://doi.org/10.1007/978-94-009-1061-4 Verlag Volltext |
| spellingShingle | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 International Astronomical Union Physics Astrophysics and Astroparticles |
| title | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 |
| title_alt | Proceedings of the 138th Symposium of the International Astronomical Union, held in Kiev, U.S.S.R., May 15-20, 1989 |
| title_auth | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 |
| title_exact_search | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 |
| title_full | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 edited by J. O. Stenflo |
| title_fullStr | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 edited by J. O. Stenflo |
| title_full_unstemmed | Solar Photosphere: Structure, Convection, and Magnetic Fields Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 edited by J. O. Stenflo |
| title_short | Solar Photosphere: Structure, Convection, and Magnetic Fields |
| title_sort | solar photosphere structure convection and magnetic fields proceedings of the 138th symposium of the international astronomical union held in kiev u s s r may 15 20 1989 |
| title_sub | Proceedings of the 138th Symposium of the International Astronomical Union, Held in Kiev, U.S.S.R., May 15–20, 1989 |
| topic | Physics Astrophysics and Astroparticles |
| topic_facet | Physics Astrophysics and Astroparticles |
| url | https://doi.org/10.1007/978-94-009-1061-4 |
| volume_link | (DE-604)BV000000364 |
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