Venus Monitoring Camera for Venus Express

Markiewicz, W. J.; Titov, D. V.; Ignatiev, N.; Keller, H. U.; Crisp, David; Limaye, S. S.; Jaumann, R.; Moissl, R.; Thomas, N.; Esposito, L. W.; Watanabe, Shigeto; Fiethe, Björn; Behnke, Thomas; Szemerey, I.; Michalik, H.; Perplies, H.; Wedemeier, M; Sebastian, Ilse; Boogaerts, W.; Hviid, S. F.; Dierker, C.; Osterloh, B.; Böker, W; Koch, Mirja; Michaelis, H.; Belyaev, Denis; Dannenberg, Andrew L.; Tschimmel, M.; Russo, Pedro; Roatsch, T.; Matz, Klaus-Dieter

doi:10.1016/j.pss.2007.01.004

Cited by 98 publications

(59 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Previously, have reviewed the observations and gaps in our knowledge of the solar and thermal radiation fluxes in the Venus atmosphere just prior to the beginning of the Venus Express coverage. The VIRTIS (Piccioni et al 2007a) and VMC on Venus Express (Markiewicz et al 2007a(Markiewicz et al , 2007b have provided reflected solar and near infrared emission from Venus, however the coverage is not global due to the elliptic polar orbit from which the measurements were made, and provide a better coverage of the Southern hemisphere. VIRTIS near infrared observations ended after two years of operation but continued to provide reflected solar observations (0.25-1.0 μm).…”

Section: Radiative Balancementioning

confidence: 99%

“…The absorption at longer wavelengths (0.32-0.5 μm) is attributed to the presence of unknown absorbers in the upper cloud (58-65 km). Variability of the upper cloud structure and abundance of the absorbing species produces the wellknown UV markings on the Venus disc with albedo variations of up to 30% (Coffeen 1971;Limaye 1984;Rossow et al 1980;Markiewicz et al 2007aMarkiewicz et al , 2007b). In the near infrared (1-2 μm), sharp spectral features associated with absorption by CO 2 and H 2 O within and above the cloud tops are clearly seen in the Venus spectrum.…”

Section: Reflected Spectrummentioning

confidence: 99%

“…The Venus Monitoring Camera (VMC) imaged the planet in the narrow band filter centered at the characteristic band of the unknown UV absorber (365 nm) (Markiewicz et al 2007a(Markiewicz et al , 2007b which is responsible for deposition of about half of the solar energy that Venus receives from the Sun. Inhomogeneous distribution of the absorber at the cloud tops produces famous UV markings and strongly affects the radiative energy deposition pattern (see Titov et al, this issue).…”

Section: Infrared Emissionmentioning

confidence: 99%

“…The peak emission is seen in the core region of the hemispheric vortex roughly centered over the pole corresponding to lower cloud tops and descending air (and concurrent adiabatic warming) as the mean meridional flow converges a mechanism similar to the mesoscale winds at the sea coasts on Earth or at the edge of the Martian polar cap. Such rare global brightening events, when bright haze almost completely covered Venus in about a day (Markiewicz et al 2007a(Markiewicz et al , 2007b cause global changes of the planetary albedo that affects the radiative energy deposition pattern and thus has an impact on the atmospheric dynamics. Figure 32 shows the outgoing thermal flux in the near infrared on the night side and the clouds/aerosol distribution on the day side.…”

Section: Infrared Emissionmentioning

confidence: 99%

See 3 more Smart Citations

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

View full text Add to dashboard Cite

From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet's extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in [1411][1412][1413][1414] 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595-4622, 1996) from 1 μm observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.

show abstract

Section: Radiative Balancementioning

confidence: 99%

Section: Reflected Spectrummentioning

confidence: 99%

Section: Infrared Emissionmentioning

confidence: 99%

Section: Infrared Emissionmentioning

confidence: 99%

See 2 more Smart Citations

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

View full text Add to dashboard Cite

show abstract

“…These two spacecraft are capable of revealing complementary aspects of the Venusian atmosphere. On Venus Express, the Venus monitoring camera (VMC) (Markiewicz et al 2007) with four narrowband filters from ultraviolet (UV) to near infrared (IR) made similar observations, but as Venus Express was in a polar orbit, it could not track the cloud patterns appearing on Venus. AKATSUKI is on a westward equatorial orbit and is capable of taking successive images in the low-and midlatitudes of Venus, which is advantageous for studies of the atmosphere.…”

Section: Introductionmentioning

confidence: 99%

AKATSUKI returns to Venus

et al. 2016

View full text Add to dashboard Cite

AKATSUKI is the Japanese Venus Climate Orbiter that was designed to investigate the climate system of Venus. The orbiter was launched on May 21, 2010, and it reached Venus on December 7, 2010. Thrust was applied by the orbital maneuver engine in an attempt to put AKATSUKI into a westward equatorial orbit around Venus with a 30-h orbital period. However, this operation failed because of a malfunction in the propulsion system. After this failure, the spacecraft orbited the Sun for 5 years. On December 7, 2015, AKATSUKI once again approached Venus and the Venus orbit insertion was successful, whereby a westward equatorial orbit with apoapsis of ~440,000 km and orbital period of 14 days was initiated. Now that AKATSUKI's long journey to Venus has ended, it will provide scientific data on the Venusian climate system for two or more years. For the purpose of both decreasing the apoapsis altitude and avoiding a long eclipse during the orbit, a trim maneuver was performed at the first periapsis. The apoapsis altitude is now ~360,000 km with a periapsis altitude of 1000-8000 km, and the period is 10 days and 12 h. In this paper, we describe the details of the Venus orbit insertion-revenge 1 (VOI-R1) and the new orbit, the expected scientific information to be obtained at this orbit, and the Venus images captured by the onboard 1-µm infrared camera, ultraviolet imager, and long-wave infrared camera 2 h after the successful initiation of the VOI-R1.

show abstract

Active volcanism on Venus in the Ganiki Chasma rift zone

Shalygin

Markiewicz

Basilevsky

et al. 2015

Geophysical Research Letters

136

114

View full text Add to dashboard Cite

Venus is known to have been volcanically resurfaced in the last third of solar system history and to have undergone a significant decrease in volcanic activity a few hundred million years ago. However, fundamental questions remain: Is Venus still volcanically active today, and if so, where and in what geological and geodynamic environment? Here we show evidence from the Venus Express Venus Monitoring Camera for transient bright spots that are consistent with the extrusion of lava flows that locally cause significantly elevated surface temperatures. The very strong spatial correlation of the transient bright spots with the extremely young Ganiki Chasma, their similarity to locations of rift‐associated volcanism on Earth, provide strong evidence for their volcanic origin and suggests that Venus is currently geodynamically active.

show abstract

Venus Monitoring Camera for Venus Express

Cited by 98 publications

References 35 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

AKATSUKI returns to Venus

Active volcanism on Venus in the Ganiki Chasma rift zone

Contact Info

Product

Resources

About