Spatially resolved measurements of H<sub>2</sub>O, HCl, CO, OCS, SO<sub>2</sub>, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Arney, Giada; Meadows, Victoria; Crisp, David; Schmidt, Sarah J.; Bailey, Jeremy; Robinson, Tyler D.

doi:10.1002/2014je004662

Cited by 131 publications

(156 citation statements)

References 85 publications

Supporting

Mentioning

139

Contrasting

Unclassified

Order By: Relevance

“…Furthermore, the water vapor detected at this wavelength is from just below the clouds, while H 2 O absorption at 1-1.2 μm comes from the atmosphere immediately above the surface. OCS also absorbs in the 2.2-2.5 μm range, and has been observed Arney et al 2014). The most significant windows between CO 2 bands are between 1-1.2 μm where only H 2 O absorbs, at 1.7 μm where HCl and CO are also detectable, and between 2.2 and 2.5 μm, where absorption by CO and SO 2 may be seen.…”

Section: Greenhouse Effect and Climate Evolutionmentioning

confidence: 60%

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: Greenhouse Effect and Climate Evolutionmentioning

confidence: 60%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

View full text Add to dashboard Cite

show abstract

“…SMART has been validated against observations of multiple solar system planets (Robinson et al , 2011; Arney et al , 2014). The Line-by-Line Absorption Coefficients (LBLABC) code, a companion to SMART, creates line-by-line absorption files for input gas mixing ratios and temperature-pressure profiles using HITRAN 2012 line lists (Rothman et al , 2013).…”

Section: Models and Methodsmentioning

confidence: 99%

The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth

et al. 2016

Self Cite

View full text Add to dashboard Cite

Recognizing whether a planet can support life is a primary goal of future exoplanet spectral characterization missions, but past research on habitability assessment has largely ignored the vastly different conditions that have existed in our planet's long habitable history. This study presents simulations of a habitable yet dramatically different phase of Earth's history, when the atmosphere contained a Titan-like, organic-rich haze. Prior work has claimed a haze-rich Archean Earth (3.8–2.5 billion years ago) would be frozen due to the haze's cooling effects. However, no previous studies have self-consistently taken into account climate, photochemistry, and fractal hazes. Here, we demonstrate using coupled climate-photochemical-microphysical simulations that hazes can cool the planet's surface by about 20 K, but habitable conditions with liquid surface water could be maintained with a relatively thick haze layer (τ ∼ 5 at 200 nm) even with the fainter young Sun. We find that optically thicker hazes are self-limiting due to their self-shielding properties, preventing catastrophic cooling of the planet. Hazes may even enhance planetary habitability through UV shielding, reducing surface UV flux by about 97% compared to a haze-free planet and potentially allowing survival of land-based organisms 2.7–2.6 billion years ago. The broad UV absorption signature produced by this haze may be visible across interstellar distances, allowing characterization of similar hazy exoplanets. The haze in Archean Earth's atmosphere was strongly dependent on biologically produced methane, and we propose that hydrocarbon haze may be a novel type of spectral biosignature on planets with substantial levels of CO2. Hazy Archean Earth is the most alien world for which we have geochemical constraints on environmental conditions, providing a useful analogue for similar habitable, anoxic exoplanets. Key Words: Haze—Archean Earth—Exoplanets—Spectra—Biosignatures—Planetary habitability. Astrobiology 16, 873–899.

show abstract

“…The carbonyl sulfide molecule is found in the atmosphere of Venus (see Arney et al [90]) and in the interstellar medium [91]. Its shifts and broadening coefficients have been studied only sparingly until now.…”

Section: Ocsmentioning

confidence: 99%

H 2 , He, and CO 2 line-broadening coefficients, pressure shifts and temperature-dependence exponents for the HITRAN database. Part 1: SO 2 , NH 3 , HF, HCl, OCS and C 2 H 2

Wilzewski

Gordon

Kochanov

et al. 2016

Journal of Quantitative Spectroscopy and Radiative Transfer

View full text Add to dashboard Cite

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Abstract: We find considerable spatial variability suggesting active processes with conservation between species. The most variable regions are just below the Venus cloud deck, and these may be related to changes in atmospheric circulation or virga events.

Cited by 131 publications

References 85 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth

H 2 , He, and CO 2 line-broadening coefficients, pressure shifts and temperature-dependence exponents for the HITRAN database. Part 1: SO 2 , NH 3 , HF, HCl, OCS and C 2 H 2

Contact Info

Product

Resources

About

Spatially resolved measurements of H2O, HCl, CO, OCS, SO2, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Abstract: We find considerable spatial variability suggesting active processes with conservation between species. The most variable regions are just below the Venus cloud deck, and these may be related to changes in atmospheric circulation or virga events.

Cited by 131 publications

References 85 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth

H 2 , He, and CO 2 line-broadening coefficients, pressure shifts and temperature-dependence exponents for the HITRAN database. Part 1: SO 2 , NH 3 , HF, HCl, OCS and C 2 H 2

Contact Info

Product

Resources

About

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows