Formation of the Ionosphere of Mars

Ivanov-Kholodnyĭ, G. S.; Mikhailov, A.V.; Savich, N.A.

doi:10.3367/ufnr.0111.197310m.0373

Cited by 2 publications

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“…The period of cyclicity of brightness variations of the star has been determined; it is 2.7 years [6], which is consistent with our computational results for 33 stars and confirms the widespread phenomenon of quasi-biennial variations of solar-type stars. In a recent paper devoted to the quasi-biennial variations (QBV) of solar radiation fluxes [7] the importance of the QBV problem studying was em-phasized. It turned out that QBV modulations of total flux of solar radiation are closely related to various quasi-biennial variations QBV processes on the Earth, in particular with the QBV of the Earth's rotation speed, the QBV of the velocity of the stratospheric wind, etc.…”

Section: The Results Of Calculations Of the Variation Periods Of The mentioning

confidence: 99%

The activity of the solar atmosphere and solar-type stars at 11-year and quasi-biennial timescales

Бруевич

Kononovich

2011

Moscow Univ. Phys.

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We studied new simultaneous observations of the flux variations of the photospheric and chromospheric emissions of 33 solar-type stars and Sun during the HK-project that were conducted over the past 20 years. In addition to the known cyclic chromospheric emission variations of stars at the 11-year time scale, which were discovered at the Mount Wilson Observatory, we found a recurrences that are similar to the quasi-biennial variations of solar radiation. The results of calculations of the radiation fluxes variations periods of stars at the quasi-biennial scale are given.

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Section: The Results Of Calculations Of the Variation Periods Of The mentioning

confidence: 99%

The activity of the solar atmosphere and solar-type stars at 11-year and quasi-biennial timescales

Бруевич

Kononovich

2011

Moscow Univ. Phys.

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Peculiarities of the solar wind interaction with the upper atmospheres of Venus and Mars

Бреус

1980

Geofis Int

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Mediciones de plasma y de campos magnéticos en Venus y Marte así como observaciones de radio ocultamiendo 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 proegida 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 efecivo en Venus. En Marte, el campo magnético intrínseco domina y jueg un papel importante en la información del obstáculo y en la desaceleración del viento solar.

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Formation of the Ionosphere of Mars

Cited by 2 publications

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The activity of the solar atmosphere and solar-type stars at 11-year and quasi-biennial timescales

The activity of the solar atmosphere and solar-type stars at 11-year and quasi-biennial timescales

Peculiarities of the solar wind interaction with the upper atmospheres of Venus and Mars

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