| Texto completo | |
| Autor(es): Mostrar menos - |
Frisch, P. C.
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Berdyugin, A. B.
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Piirola, V.
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Magalhaes, A. M.
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Seriacopi, D. B.
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Ferrari, T.
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Santos, F. P.
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Schwadron, N. A.
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Funsten, H. O.
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McComas, D. J.
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Heiles, C. E.
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Zank, GP
Número total de Autores: 12
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| Tipo de documento: | Artigo Científico |
| Fonte: | WAKE CONFERENCE 2021; v. 767, p. 11-pg., 2016-01-01. |
| Resumo | |
for tracing the structure of the very local interstellar magnetic field (ISMF). Two methods have been developed to recover the ISMF direction from polarized starlight, using data from an ongoing polarization survey. Both methods rely on the probability distribution function for polarized light. Method 1 calculates the ISMF direction from polarization position angles regardless of the data accuracy, while Method 2 relies on high-probability data points. The ISMF direction BTBEx recovered by Method 1 corresponds to the closest ISMF to the heliosphere, traced by the center of the IBEX Ribbon arc. Method 2 reveals a new direction for the more distant ISMF, B-new, toward =41.1 degrees +/- 4.1 degrees and b = 25.8 degrees +/- 3.0 degrees, which differs by 30.4 degrees +/- 5.6 degrees from the IBEX ISMF direction. Polarizations of filament stars that are located within 25 degrees of a pole of B-new, where background polarizations would be minimal, show the highest statistical probabilities of tracing the filament ISMF. The IBEX ISMF direction orders the kinematics of interstellar clouds within 15 pc, and B-new must therefore dominate beyond 15 pc. These new data are consistent with the location of the Sun in the rim of an expanding superbubble shell associated with the evolved Loop I superbubble. (AU) | |
| Processo FAPESP: | 10/19694-4 - SOUTH POL: descobrindo o céu Austral polarizado |
| Beneficiário: | Antônio Mário Magalhães |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |