Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki

Y. J. Lee; A. Yamazaki; T. Imamura; M. Yamada; S. Watanabe; T. M. Sato; K. Ogohara; G. L. Hashimoto; S. Murakami

doi:10.3847/1538-3881/aa78a5

Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki

Y. J. Lee, A. Yamazaki, T. Imamura, M. Yamada, S. Watanabe, T. M. Sato, K. Ogohara, G. L. Hashimoto, S. Murakami

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27 Citations (Scopus)

Abstract

We analyze the albedo of Venus obtained from the UV Imager on board Akatsuki. A relative global mean albedo over phase angle is used in this study, and we confirm the glory feature at 283 and 365 nm in the data acquired in 2016 May. We successfully simulate the observation using a radiative transfer model. Our results show that cloud aerosols of μm and (mode 2) can explain the glory, consistent with a property of aerosols previously suggested by using the Venus Monitoring Camera on board Venus Express. We find that SO₂ and the unknown UV absorber are necessary factors to explain the decreasing trend of the observed relative albedo at phase angles larger than 10°. We suggest a range of possible SO₂ abundance from 80 to 400 ppbv at the cloud top level, depending on atmospheric conditions assumed.

Original language	English
Article number	44
Journal	Astronomical Journal
Volume	154
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/aa78a5
Publication status	Published - Aug 2017

Keywords

planets and satellites: atmospheres
ultraviolet: planetary systems

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-3881/aa78a5

Cite this

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title = "Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki",

abstract = "We analyze the albedo of Venus obtained from the UV Imager on board Akatsuki. A relative global mean albedo over phase angle is used in this study, and we confirm the glory feature at 283 and 365 nm in the data acquired in 2016 May. We successfully simulate the observation using a radiative transfer model. Our results show that cloud aerosols of μm and (mode 2) can explain the glory, consistent with a property of aerosols previously suggested by using the Venus Monitoring Camera on board Venus Express. We find that SO2 and the unknown UV absorber are necessary factors to explain the decreasing trend of the observed relative albedo at phase angles larger than 10°. We suggest a range of possible SO2 abundance from 80 to 400 ppbv at the cloud top level, depending on atmospheric conditions assumed.",

keywords = "planets and satellites: atmospheres, ultraviolet: planetary systems",

author = "Lee, {Y. J.} and A. Yamazaki and T. Imamura and M. Yamada and S. Watanabe and Sato, {T. M.} and K. Ogohara and Hashimoto, {G. L.} and S. Murakami",

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T1 - Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki

AU - Lee, Y. J.

AU - Yamazaki, A.

AU - Imamura, T.

AU - Yamada, M.

AU - Watanabe, S.

AU - Sato, T. M.

AU - Ogohara, K.

AU - Hashimoto, G. L.

AU - Murakami, S.

PY - 2017/8

Y1 - 2017/8

N2 - We analyze the albedo of Venus obtained from the UV Imager on board Akatsuki. A relative global mean albedo over phase angle is used in this study, and we confirm the glory feature at 283 and 365 nm in the data acquired in 2016 May. We successfully simulate the observation using a radiative transfer model. Our results show that cloud aerosols of μm and (mode 2) can explain the glory, consistent with a property of aerosols previously suggested by using the Venus Monitoring Camera on board Venus Express. We find that SO2 and the unknown UV absorber are necessary factors to explain the decreasing trend of the observed relative albedo at phase angles larger than 10°. We suggest a range of possible SO2 abundance from 80 to 400 ppbv at the cloud top level, depending on atmospheric conditions assumed.

AB - We analyze the albedo of Venus obtained from the UV Imager on board Akatsuki. A relative global mean albedo over phase angle is used in this study, and we confirm the glory feature at 283 and 365 nm in the data acquired in 2016 May. We successfully simulate the observation using a radiative transfer model. Our results show that cloud aerosols of μm and (mode 2) can explain the glory, consistent with a property of aerosols previously suggested by using the Venus Monitoring Camera on board Venus Express. We find that SO2 and the unknown UV absorber are necessary factors to explain the decreasing trend of the observed relative albedo at phase angles larger than 10°. We suggest a range of possible SO2 abundance from 80 to 400 ppbv at the cloud top level, depending on atmospheric conditions assumed.

KW - planets and satellites: atmospheres

KW - ultraviolet: planetary systems

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Scattering Properties of the Venusian Clouds Observed by the UV Imager on board Akatsuki

Abstract

Keywords

ASJC Scopus subject areas

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