Studying the Venus terminator thermal structure observed by SOIR/VEx with a 1D radiative transfer...
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Studying the Venus terminator thermal structure observed by SOIR/VEx with a 1D radiative transfer model A. Mahieux 1,2,3 , J. T. Erwin 3 , S. Chamberlain 1 , S. Robert 1 , A. C. Vandaele 1 , V. Wilquet 1 , I. Thomas 1 , R. V. Yelle 3 1 Belgian Institute for Space Aeronomy, 3 av. Circulaire, B-1180 Brussels, Belgium 2 Fonds National de la Recherche Scientifique, rue d’Egmont 5, B- 1000 Brussels, Belgium 3 Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA ([email protected] / Fax: +32 2-374-8423 / Tel: +32 2-373-0475) The SOIR instrument is dedicated to sound the Venus terminator, using the solar occultation technique [1]. SOIR records spectra in the mesosphere and the thermosphere, at all latitudes from pole to pole. CO 2 number density profiles [2] are derived from the measured spectra, as well as CO [3], H 2 O/HDO [4], HCl, HF [5], SO 2 [6], see Figure 1. The extinction profiles due to aerosols are also calculated, and the aerosols composition and size distribution are studied [7]. The derived temperature profiles show a striking and permanent cold layer close to the homopause (~130 km), with temperatures as cold as 80-150 K. It is surrounded by two warm layers, at 100 km (200 to 250 k) and at 150 km (~250 K). Figure 1: Mean profiles derived from the SOIR measurements, as a function of the altitude, covering the 73 km to 143 km region. Panel A: mean temperature profile; Panel B: mean number density profiles of the considered species; Panel C: mean VMR profiles. Figure 2: Vertical profiles considering the default test at steady state, considering all cooling and heating mechanisms, except the aerosols, as a function of the altitude. In each panel: the model profiles are the solid lines, the SOIR mean profiles are the dashed lines A sensitivity study has been performed on most of the model parameters. Tuning the O production rate or modifying the 15 µm non-LTE parameter changes the thermospheric temperature. The temperature of the cold layer at 135 km and its altitude level are almost independent of the O production rate and the UV efficiency, weakly controlled by the 4.3 µm and 15 µm non-LTE parameters, and strongly dependent of the 2.8 µm non-LTE parameter. Finally, the temperature in the mesosphere only controlled by the 2.8 and 4.3 µm non- LTE parameters. No reasonable change of the parameters better fits the SOIR mean temperature profile. The 1-D model [8] calculates the temperature and composition by solving the coupled, time-dependent energy balance, diffusion, and continuity equations. The vertical scale considered in the model is the altitude, from 80 km to 180 km, and discretized on a 1 km grid. The atmosphere is treated as plane- parallel and the total pressure is calculated using the hydrostatic equilibrium at each time step. We consider thermal escape to space at the Jeans rate. The time dependent equations are solved using a Crank– Nicholson integration scheme until steady state is reached. The model considers the main species present in the Venus atmosphere in this altitude region: CO 2 , N 2 , CO, O, HCl, H 2 O, SO 2 and the aerosols. The number density of the species and the temperature are fixed at the lower boundary, while the upper boundary conditions are set by the Jeans escape velocities for the density and an isothermal temperature. The radiative terms are the UV heating, the non-LTE 2.8 µm and 4.3 µm CO 2 heating, the 15 µm CO 2 cooling and the H 2 O, HCl, CO, O rotational line cooling. To simulate the O transported from the dayside, an O production rate is considered in the computation process, modeled as a Chapman profile. It has a default peak maximum of 1.5×10 7 cm -3 ·s -1 , located at an altitude of 120 km. We first do not consider aerosols, see Figure 2. Venus aerosols have a strong cooling and a weaker heating effect. We propose to add them to the model to better fit the temperature profile. The cooling effect is larger by 3 orders of magnitude than the warming effect. The two first particle modes are considered here, i.e. with and . The particles are supposed to be spherical, with a composition of 75% H 2 SO 4 and 25% H 2 O. A ratio of 50 between the 2 modes is assumed. Since the aerosols mass loading is negligible compared to gas loading, since the aerosols VMR is of the order of 10 ‑18 , adding aerosols into the model does not change the hydrostatic equilibrium. For this reason, the aerosols number density profile can be calculated such that the model steady-state temperature profile perfectly matches the mean SOIR temperature profile, see Fig. 3 and 4. Figure 4: Vertical heating and cooling rates profiles considering the default test at steady state, considering all cooling and heating mechanisms, except the aerosols, as a function of the total pressure. Figure 3: Fit of the aerosols number density profiles to best match the SOIR measured temperature profile. A factor 50 is supposed between modes 1 and 2. The black line is a mode 1 mean profile from SOIR (Wilquet et al., 2009). References: [1] Nevejans et al., Applied Optics, 2006 [2] Mahieux et al., PSS, 2015 [3] Vandaele et al., PSS, 2015 [4] Chamberlain et al., EGU poster, 2015 [5] Mahieux et al., PSS, 2015 [6] Mahieux et al., PSS, 2015 [7] Wilquet et al., JGR, 2009 [8] Mahieux et al., Icarus, (submitted)
Transcript of Studying the Venus terminator thermal structure observed by SOIR/VEx with a 1D radiative transfer...
Studying the Venus terminator thermal structure observed by SOIR/VEx with a 1D radiative transfer model
A. Mahieux1,2,3, J. T. Erwin3, S. Chamberlain1, S. Robert1, A. C. Vandaele1, V. Wilquet1, I. Thomas1, R. V. Yelle3
1 Belgian Institute for Space Aeronomy, 3 av. Circulaire, B-1180 Brussels, Belgium 2 Fonds National de la Recherche Scientifique, rue d’Egmont 5, B-1000 Brussels, Belgium 3 Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA ([email protected] / Fax: +32 2-374-8423 / Tel: +32 2-373-0475)
The SOIR instrument is dedicated to sound the Venus terminator, using the solar occultation technique [1]. SOIR records spectra in the mesosphere and the thermosphere, at all latitudes from pole to pole. CO2 number density profiles [2] are derived from the measured spectra, as well as CO [3], H2O/HDO [4], HCl, HF [5], SO2 [6], see Figure 1. The extinction profiles due to aerosols are also calculated, and the aerosols composition and size distribution are studied [7]. The derived temperature profiles show a striking and permanent cold layer close to the homopause (~130 km), with temperatures as cold as 80-150 K. It is surrounded by two warm layers, at 100 km (200 to 250 k) and at 150 km (~250 K).
Figure 1: Mean profiles derived from the SOIR measurements, as a function of the altitude, covering the 73 km to 143 km region. Panel A: mean temperature profile; Panel B: mean number density profiles of the considered species; Panel C: mean VMR profiles.
Figure 2: Vertical profiles considering the default test at steady state, considering all cooling and heating mechanisms, except the aerosols, as a function of the altitude. In each panel: the model profiles are the solid lines, the SOIR mean profiles are the dashed lines
A sensitivity study has been performed on most of the model parameters. Tuning the O production rate or modifying the 15 µm non-LTE parameter changes the thermospheric temperature. The temperature of the cold layer at 135 km and its altitude level are almost independent of the O production rate and the UV efficiency, weakly controlled by the 4.3 µm and 15 µm non-LTE parameters, and strongly dependent of the 2.8 µm non-LTE parameter. Finally, the temperature in the mesosphere only controlled by the 2.8 and 4.3 µm non-LTE parameters. No reasonable change of the parameters better fits the SOIR mean temperature profile.
The 1-D model [8] calculates the temperature and composition by solving the coupled, time-dependent energy balance, diffusion, and continuity equations. The vertical scale considered in the model is the altitude, from 80 km to 180 km, and discretized on a 1 km grid. The atmosphere is treated as plane-parallel and the total pressure is calculated using the hydrostatic equilibrium at each time step. We consider thermal escape to space at the Jeans rate. The time dependent equations are solved using a Crank–Nicholson integration scheme until steady state is reached. The model considers the main species present in the Venus atmosphere in this altitude region: CO2, N2, CO, O, HCl, H2O, SO2 and the aerosols. The number density of the species and the temperature are fixed at the lower boundary, while the upper boundary conditions are set by the Jeans escape velocities for the density and an isothermal temperature. The radiative terms are the UV heating, the non-LTE 2.8 µm and 4.3 µm CO2 heating, the 15 µm CO2 cooling and the H2O, HCl, CO, O rotational line cooling. To simulate the O transported from the dayside, an O production rate is considered in the computation process, modeled as a Chapman profile. It has a default peak maximum of 1.5×107 cm-3·s-1, located at an altitude of 120 km. We first do not consider aerosols, see Figure 2.
Venus aerosols have a strong cooling and a weaker heating effect. We propose to add them to the model to better fit the temperature profile. The cooling effect is larger by 3 orders of magnitude than the warming effect. The two first particle modes are considered here, i.e. with and . The particles are supposed to be spherical, with a composition of 75% H2SO4 and 25% H2O. A ratio of 50 between the 2 modes is assumed. Since the aerosols mass loading is negligible compared to gas loading, since the aerosols VMR is of the order of 10 18‑ , adding aerosols into the model does not change the hydrostatic equilibrium. For this reason, the aerosols number density profile can be calculated such that the model steady-state temperature profile perfectly matches the mean SOIR temperature profile, see Fig. 3 and 4.
Figure 4: Vertical heating and cooling rates profiles considering the default test at steady state, considering all cooling and heating mechanisms, except the aerosols, as a function of the total pressure.
Figure 3: Fit of the aerosols number density profiles to best match the SOIR measured temperature profile. A factor 50 is supposed between modes 1 and 2. The black line is a mode 1 mean profile from SOIR (Wilquet et al., 2009).
References:[1] Nevejans et al., Applied Optics, 2006[2] Mahieux et al., PSS, 2015[3] Vandaele et al., PSS, 2015[4] Chamberlain et al., EGU poster, 2015[5] Mahieux et al., PSS, 2015[6] Mahieux et al., PSS, 2015[7] Wilquet et al., JGR, 2009[8] Mahieux et al., Icarus, (submitted)
