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Vásquez, A.M. "Solar corona magnetic structure and stagnated wind outflow" (2005) MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. 784:582-590
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Abstract:

Solar observations made with the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliosphere Observatory (SoHO) spacecraft, have revealed that coronal protons and heavier ions have anisotropic temperature distributions. In a recent work we developed semi-empirical models for the solar minimum corona to investigate the effect of the observed proton anisotropy on the coronal magnetic structure and the bimodal solar wind. Here we highlight the effect that the resulting particular geometry of the magnetic field around the streamer belt has on the solar wind. The open magnetic field lines surrounding the streamer belt (streamer legs) have non-monotonic expansion factors. This feature produces a stagnated outflow around the streamer magnetic cusp point, located at the top of the streamer belt closed magnetic field lines (streamer core). We find that this flow stagnation effect extends over quite important distances (of order 1R⊙) from the streamer cusp location. © 2005 American Institute of Physics.

Registro:

Documento: Conferencia
Título:Solar corona magnetic structure and stagnated wind outflow
Autor:Vásquez, A.M.
Ciudad:Angra dos Reis
Filiación:Instituto de Astronomía y Física del Espacio, CC 67 - Suc 28, Ciudad de Buenos Aires, Argentina
Palabras clave:Corona; Solar wind plasma; Streamers
Año:2005
Volumen:784
Página de inicio:582
Página de fin:590
DOI: http://dx.doi.org/10.1063/1.2077222
Título revista:MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures
Título revista abreviado:AIP Conf. Proc.
ISSN:0094243X
Registro:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0094243X_v784_n_p582_Vasquez

Referencias:

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Citas:

---------- APA ----------
(2005) . Solar corona magnetic structure and stagnated wind outflow. MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures, 784, 582-590.
http://dx.doi.org/10.1063/1.2077222
---------- CHICAGO ----------
Vásquez, A.M. "Solar corona magnetic structure and stagnated wind outflow" . MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures 784 (2005) : 582-590.
http://dx.doi.org/10.1063/1.2077222
---------- MLA ----------
Vásquez, A.M. "Solar corona magnetic structure and stagnated wind outflow" . MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures, vol. 784, 2005, pp. 582-590.
http://dx.doi.org/10.1063/1.2077222
---------- VANCOUVER ----------
Vásquez, A.M. Solar corona magnetic structure and stagnated wind outflow. AIP Conf. Proc. 2005;784:582-590.
http://dx.doi.org/10.1063/1.2077222