millimeter-wavelength remote sensing of the tropospheric structure of venus ... · 2018. 12....

Millimeter-Wavelength Remote Sensing of the Tropospheric Structure of Venus:

Exploratory SimulationsAlex B. Akins, Paul G. Steffes

November 7th, 201816th VEXAG Meeting

Correspondence: [email protected], [email protected]

mailto:[email protected]

mailto:[email protected]

Remote Observations of Venus

11/7/2018Millimeter-Wavelength Remote Sensing of the Tropospheric Structure of

Venus: Exploratory Simulations1

Peralta, et al. in Icarus (2017)

Cloud Base

Passive remote sensing of sub-cloud atmospheric structure limited to narrow IR bands, microwave/millimeter emission

8 GHz

20 GHz40 GHz

70 GHz

110 GHz

Microwave Emission Weighting Functions

(Microns)

Millimeter-Wavelength Continuum Images

11/7/2018 Millimeter-Wavelength Remote Sensing of the Tropospheric Structure of Venus: Exploratory Simulations 2

Encrenaz et al. (2015), 346 GHz, Phase: 0.902, Upper CloudSagawa (2008), 103 GHz,

Phase: 0.272, Cloud Basede Pater et al. (1991), 115 GHz,

Phase: 0.527, Cloud Base

• Longitudinal brightness temperature variations on the order of 30-80 K are observed in disk images

• 8-22% of the disk-average• Only observed on nightside • Uncorrelated with topographical features

• Is this a measurement artifact or the result of a physical process?

Microwave Radiative Transfer Model

• Temperature and pressure profiles from VIRA (Seiff 1985), PV entry probes

• CO2/N2 absorption• Ho, Kaufman, Thaddeus (1966)• Valid for 2-4 mm wavelengths

• SO2 and H2SO4 vapor absorption• Other contributing absorbers

• Abundances derived from remote sensing observations and inferred from chemical modeling• Krasnopolsky (2007)

• H2SO4 liquid aerosol – Absorption model of Fahd and Steffes (1991)• Scattering is negligible based on aerosol size distributions from Pioneer Venus LCPS results

• H2O – Modelled with modified opacity formalism of Karpowicz and Steffes (2011)• CO – Van Vleck-Weisskopf model, parameters from Bauer et al. (1989)• OCS - Van Vleck-Weisskopf model, parameters from Feeny et al. (1954)


↵CO2/N2= 1.12 · 108

�q2CO2

+ 0.25qCO2qN2 + 0.0054q2N2

�f2p2T�5

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SO2 Millimeter–Wavelength Absorption

• Measured from 2-4 mm under simulated Venus conditions

• Bellotti and Steffes (2015)• 0 – 2 bar CO2, 308-343 K

• Matches Van-Vleck Weisskopf absorption model• Fahd (1992)• This model is valid from microwave to millimeter

wavelengths under cloud-base to surface conditions (Steffes et al. 2015)


Venus: Exploratory Simulations 4

2–3 mm absorp,on of 76 mbar SO2 broadened with 833 mbar CO2 at 345 K

H2SO4 Vapor Millimeter-Wavelength Absorption

• Measured with a semi-confocal corrosion-resistant open resonator from 2–4 mm

• 0 – 3 bar CO2, 533-550K• Measurements at lower temperatures are prohibitive

• Microwave measurements of Kolodner and Steffes(1998) overstates absorption at millimeter-wavelengths

• Closer fit to lineshape model• Using JPL catalog (Cohen and Drouin 2013)• Δ"#$%&' = 97.17 -.//1233, Δ"4&$ = 4.86 -.//1233


Absorp'on spectra of 2̴0 mbar H2SO4broadened with 2.975 bar CO2 at 550 K

What is Causing Continuum Emission Longitudinal Variability?

• ~8 K decrease from disk center to near-limb emission

• Physical processes in the 40-55 km range

• Changes in temperature and pressure conditions due to dynamic processes• However, minimal evidence for significant longitudinal variations in this range (Limaye et al. 2018)

• Some unknown spatially-variable absorber• Unlikely

Considered here

• Variations in H2SO4 vapor or SO2 vertical abundance structure with longitude

• Variations in cloud bulk density• Larger aerosol

• Sizes are unlikely to be large enough (McGouldrick et al. 2011) to result in significant 2-4 mm scattering

Disclaimer: Thermal structure, cloud cover, and constituent abundances are all linked!



(Assuming it is physical)

Abundances of SO2

and H2SO

4 Below the Clouds

• H2SO

4profiles retrieved from radio occultation profiles

• Mariner 10, Pioneer Venus, Magellan, Venus Express,

Akatsuki

• Possible supersaturation suggested by VeRa results

• Previously, SO2 vertical abundance profile assumed

uniform below clouds

• Latitudinally dependent, ranges from 50-150 ppm (Marcq et

al. 2008, Jenkins et al. 2002)

• Results from ISAV-1 and ISAV-2 experiments call this into

question (Bertraux et al. 1996)

• Upper troposphere dynamics may result in radical variations

11/7/2018Millimeter-Wavelength Remote Sensing of the Tropospheric Structure of Venus:

Exploratory Simulations7

Mariner 10 low latitude occultation

Abundances of H2SO4 Below the Clouds

• Abundance scaling representative of possible H2SO4 supersaturation

• Lower SO2 abundance should lead to enhanced effect of H2SO4 abundance variation

• Physical conditions are prohibitive to high vapor abundance above 52 km

• H2SO4 abundance variations would not (directly) result in substantial brightness temperature variations


Exploratory Simulations 8

Thermal dissocia.on to

SO3, H2O

Decreasing SVP and

condensationShift

Shift

Scale

Variation of equatorial nadir brightness (103 GHz) with 5x scaled and shifting H2SO4

abundance profile (50 ppm SO2)

Abundances of SO2 Below the Clouds


• Scaling SO2 abundance features seen in the ISAV UV results from Vega 1 and Vega 2 landers

• Nightside measurements• Potential issue with cloud condensation on

mirrors

• Spatial variations in the SO2 mixing ratio below 40 kilometers would not be observable from 2-4 mm

• Opaque due to CO2/N2 absorption

• Substantial SO2 abundance variations in the clouds could explain variations in millimeter-wavelength continuum images

ISAV 1

ISAV 2

High Peak

Low Peak

Variations in Cloud Structure

• Scaled from PV Large Probe• Knollenberg and Hunten (1980)

• Substantial variations in the bulk density of the lower cloud would result in 30-40K brightness temperature variations

• Cloud scattering is not significant for previously observed particle sizes

• Larger particle sizes are unlikely (McGouldrick et al. 2011)


Exploratory Simulations 10

300 micron

Conclusions

• Variations in H2SO4 vapor are not likely responsible for millimeter wavelength features

• ALMA observations with long baselines can provide precise constraints on brightness temperature variations

• Multi-band coordinated microwave and millimeter-wavelength observations can retrieve regional constituent abundance and temperature profiles

• Future microwave/millimeter radiometer on Venera-D?• Further measurements of pressure broadened H2SO4 absorption

could be key to interpret future Ka band radio occultations


Backup Slides

Distinguishing between SO2 and cloud variations



Frequency dependence of lower cloud bulk density variations

Frequency dependence of 52 km SO2

mole frac<on varia<ons

Multi-wavelength observations would help tell the sources apart, particularly between 130 and 140 GHz

Vertical Wave Propagation


Imamura et al. 2014

2013 CARMA Images (Preliminary)


99.2 GHz 114.8 GHz

• Concurrently imaged at elongation• Disclaimer: Heterogeneous array

makes imaging particularly difficult

Devaraj, CookNCSA CARMA Data Archive

millimeter-wavelength remote sensing of the tropospheric structure of venus ... · 2018. 12....

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