Peculiarities of the solar wind interaction with the upper atmospheres of Venus and Mars
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Resumen
Mediciones de plasma y de campos magnéticos en Venus y Marte así como observaciones de radio ocultamiento de satélites por sus atmósferas y ionosferas superiores revelan algunas diferencias y semejanzas en la configuración del flujo del viento solar alrededor de estos planetas. Ambos planetas tienen campos magnéticos muy débiles comparados con el de la Tierra y sus ionosferas están caracterizadas por un máximo de densidad electrónica similar. Sin embargo, la ionosfera Marciana está más protegida de la acción directa del viento solar que la de Venus y algunas propiedades de la ionosfera superior Marciana se asemejan a las de la ionosfera superior de la Tierra. Se concluye que la ionosfera de Venus y el campo magnético inducido (el campo magnético del viento solar acumulado alrededor de la ionosfera del planeta) son elementos decisivos para la formación del obstáculo efectivo en Venus. En Marte, el campo magnético intrínseco domina y juega un papel importante en la formación del obstáculo y en la desaceleración del viento solar.
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