A modernization of the analysis method for vertical structure of aerosol component in giant planet atmospheres
| 1Ovsak, AS 1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine |
| Kinemat. fiz. nebesnyh tel (Online) 2013, 29(6):53-67 |
| Start Page: Dynamics and Physics of Solar System Bodies |
| Language: Russian |
Abstract: We developed a program package to determine the nature of the depth change of aerosol optical thickness or the optical thickness ratio for aerosolic and gas components for spectral absorption bands of atmospheric gases. Structurally, the program package consists of the following units: the calculation program of M. I. Mischenko to determine coefficients xi of the scattering function expansion in a series of Legendre polynomials and volumetric scattering coefficient σ0 for the polydisperse media with a specified refractive index and function for the particle size distribution N(r); the formation of the interpolative array of calculated values for single scattering albedo ω and geometric albedo Ag in the case of a semi-infinite homogeneous layer with the parameters determined in the previous unit; determining the values of the single scattering albedo ω by comparing calculated and observed values of geometric albedo for each measuring points of the investigated absorption band of methane (including changes of scattering function due to the Rayleigh scattering); the calculation of spectral values of the effective optical depth τeff which forms the intensity field of light diffusely reflected by upper atmosphere gas-aerosol layer; finding the scattering (τseff) and absorbing (τveff) components of effective optical depth on the basis of and τeff data; the determination of the amount of methane NL (in km-amagat) on the line of sight with the use of τveff data and then an atmospheric pressure p(NL) and gas scattering component τg (λ0) of full optical depth at the wavelength λ0 = 887.2 nm; finding an aerosol component τa(λ,NL) according to the data on τseff (λ) and τg(λ,NL); building a graphical relationship between pressure p and values τa(λ) converted at λ0 = 887.2 nm or τa(λ)/τg(λ). The program package was validated to perform an analysis of spectrophotometric measurements of Jupiter’s integrated disk in strong absorption bands of methane centered at 841.6 nm, 864.0 nm, and 887.2 nm. This analysis was carried out for two versions of function of particle size distribution (the modified gamma distribution and normal-logarithmic one). We found that the analysis in the gamma distribution model is performed several times faster for the same environment and with close results. |
| Keywords: aerosol, planet-giants |
References:
1.V. V. Avramchuk, “Estimation of the optical parameters of the Jovian atmosphere,” Astron. Tsirkulyar, No. 484, 4–6 (1968).
2.V. V. Avramchuk, L. A. Bugaenko, A. V. Morozhenko, et al., “The results of the investigations of Jupiter fulfilled at the Main astronomical observatory of the Ukrainian Academy of Sciences,” Astrometry Astrophys., No. 31, 54–68 (1977).
3.M. S. Dement’ev and A. V. Morozhenko, “Zones and belts in the disk of Jupiter. The difference in the vertical structure of cloud layers,” Astron. Vestn. 24(4), 275–287 (1990).
4.K. Yu. Ibragimov, Numerical Modeling of the Stratified Cloudiness in the Atmospheres of Giant Planets (Nauka, Alma-Ata, 1990) [in Russian].
5.A. V. Morozhenko, “On the structure of the cloud layer of Jupiter,” Pis’ma Astron. Zh. 10(10), 775–779 (1984).
6.A. V. Morozhenko, “The vertical structure of the latitudinal cloud belts of Jupiter,” Astron. Vestn. 24(1), 64–76 (1985).
7.A. V. Morozhenko, “Problems in the study of the vertical structure of the atmospheres of giant planets,” Kin. Fiz. Nebes. Tel 9(6), 3–26 (1993).
8.A. V. Morozhenko, “Probable ranges for the sizes of particles and relative concentrations of aerosols and methane at the levels of formation of the centers of methane absorption bands at λλ727, 619, 543, and 441 nm,” Kin. Fiz. Nebes. Tel 15(2), 110–122 (1999).
9.A. V. Morozhenko, “The difference in the vertical structures of the cloud layers in the atmospheres of giant planets,” Kin. Fiz. Nebes. Tel 17(3), 261–278 (2001).
10.O. V. Morozhenko, Methods and Results of Remote Sensing of the Planetary Atmospheres (Naukova Dumka, Kiev, 2004) [in Ukrainian].
11.A. V. Morozhenko, “New determination of monochromatic methane absorption coefficients with regard to the thermal conditions in the atmospheres of giant planets. IV. Jupiter and Saturn,” Kin. Phys. Cel. Bodies 23(6), 245–257 (2007).
https://doi.org/10.3103/S0884591307060025
12.A. V. Morozhenko and A. S. Ovsak, “Dependence of the aerosol component of optical thickness and the relative concentration of methane on depth in atmospheres of giant planets,” Kin. Phys. Cel. Bodies 25(4), 173–181 (2009).
https://doi.org/10.3103/S0884591309040011
13.A. V. Morozhenko, A. S. Ovsak, and P. P. Korsun, “The vertical structure of the cloud layer of Jupiter before and after the comet Shoemaker-Levy 9 impact,” Kin. Fiz. Nebes. Tel 11(4), 3–20 (1995).
14.A. V. Morozhenko and E. G. Yanovitskii, “Parameters of the vertical structure of the upper layers in the atmosphere of Jupiter,” Pis’ma Astron. Zh. 2(11), 549–553 (1976).
15.A. S. Ovsak, “Calculation of effective optical depth of absorption line formation in homogeneous semi-infinite planetary atmosphere during anisotropic scattering,” Kin. Phys. Cel. Bodies 26(2), 86–88 (2010).
https://doi.org/10.3103/S0884591310020066
16.E. G. Yanovitskii and A. S. Ovsak, “The effective optical depth of forming the absorption band in a semi-infinite planetary atmosphere,” Kin. Fiz. Nebes. Tel 13(4), 3–21 (1997).
17.S. K. Atreya, T. M. Donahue, and M. C. Festou, “Jupiter-Structure and composition of the upper atmosphere,” Astrophys. J. 247(1), L43–L47 (1981).
https://doi.org/10.1086/183586
18.L. Axel, “Inhomogenous model of the atmosphere of Jupiter,” Astrophys. J. 173(2), 451–468 (1972).
https://doi.org/10.1086/151437
19.J. T. Bergstralh, “Methane absorption in the Jovian atmosphere. II. Absorption line formation,” Icarus 19(3), 390–418 (1973).
https://doi.org/10.1016/0019-1035(73)90116-4
20.J. W. Chamberlain, “The atmosphere of Venus near cloud top,” Astrophys. J. 141(4), 1184–1205 (1965).
https://doi.org/10.1086/148207
21.D. S. Choi and A. A. Simon-Miller, “An analysis of Cassini observations regarding the structure of Jupiter’s equatorial atmosphere,” presented at American Geophysical Union’s 45th Annual Fall Meeting, December 3–7, 2012, San Francisco, CA. http://ntrs.nasa.gov/search.jsp?N=0&Ntk=All&Ntx=mode+matchallany&Ntt=Jup....
22.R. E. Danielson and M. G. Tomasko, “A two-layer model of the Jovian clouds,” J. Atmos. Sci. 26(5), 889–897 (1969).
https://doi.org/10.1175/1520-0469(1969)026<0889:ATLMOT>2.0.CO;2
23.J. M. Dlugach and E. G. Yanovitskiy, “The optical properties of Venus and the Jovian planets. II. Methods and results of calculations of the intensity of radiation diffusely reflected from semi-infinite homogeneous atmosphere,” Icarus 22(1), 66–81 (1974).
https://doi.org/10.1016/0019-1035(74)90167-5
24.L. P. Giver, “Intensity measurements of the CH4 bands in the region of 4350 to 10600” J. Quant. Spectrosc. Radiat. Transfer 19(2), 311–322 (1978).
https://doi.org/10.1016/0022-4073(78)90064-X
25.S. L. Hess, “Variations in atmospheric absorption over the disk of Jupiter and Saturn,” Astrophys. J. 18(1), 151–160 (1953).
https://doi.org/10.1086/145735
26.P. G. J. Irwin, S. B. Calcutt, F. W. Taylor, and A. L. Weirand, “Calculated k distribution coefficients for hydrogen- and self-broadened methane in the range 2000–9500 cm−1 from exponential sum fitting to band-modelled spectra,” J. Geophys. Res. 101(E11), 26137–26154 (1996).
https://doi.org/10.1029/96JE02707
27.E. Karkoschka, “Spectrophotometry of the Jovian planets and Titan at 300 to 1000 nm wavelength: The methane spectrum,” Icarus 111(3), 967–982 (1994).
28.E. Karkoschka, “Methane, ammonia, and temperature measurements of the Jovian planets and Titan from CCD-spectrophotometry,” Icarus 133(1), 133–146 (1998).
https://doi.org/10.1006/icar.1998.5913
29.E. Karkoschka and M. G. Tomasko, “Methane absorption coefficients for the Jovian planets from laboratory, Huygens, and HST data,” Icarus 205(2), 674–694 (2010).
https://doi.org/10.1016/j.icarus.2009.07.044
30.J. S. Lewis, “The clouds of the Jupiter’s and the NH3-H2O and NH3-H2S systems,” Icarus 10(3), 365–378 (1969).
https://doi.org/10.1016/0019-1035(69)90091-8
31.M. I. Mishchenko, “Physical properties of the upper troposphere aerosols in the equatorial region of Jupiter,” Icarus 84(2), 296–304 (1990).
https://doi.org/10.1016/0019-1035(90)90039-C
32.A. Molina, F. Moreno, and J. J. Lopes-Moreno, “Equatorial cloud structure of Jupiter derived from high resolution spectroscopy in the λλ 6300–6825” Astron. Astrophys. 226(1), 311–317 (1989).
33.F. Moreno and A. Molina, “Jupiter’s atmospheric parameters derived from spectroscopic observations in the red region during the 1988 opposition,” Astron. Astrophys. 241(1), 243–250 (1991).
34.A. V. Morozhenko, Monochromatic absorption coefficients of methane and ammonia with regard to thermal conditions in giant planet atmospheres. http://www.mao.kiev.ua/eng/dept/ssystem-morozhenko-e.html.
35.A. V. Morozhenko and E. G. Yanovitskij, “The optical properties of Venus and Jovian planets. I. The atmosphere of Jupiter according to polarimetric observations,” Icarus 18(4), 583–592 (1973).
https://doi.org/10.1016/0019-1035(73)90060-2
36.J. B. Pollack, K. Rages, K. H. Baines, et al., “Estimations of the bolometric albedo and radiance balance of Uranus and Neptune,” Icarus 65(2–3), 442–466 (1986).
https://doi.org/10.1016/0019-1035(86)90147-8
37.M. J. Price, J. S. Hall, P. B. Boyse, et al., “The physical properties of the Jovian atmosphere inferred from eclipses of the Galilean satellites. II. 1971 apparition,” Icarus 17(1), 49–56 (1972).
https://doi.org/10.1016/0019-1035(72)90045-0
38.B. Ragent, S. Colburn, K. A. Rages, et al., “The clouds of Jupiter: Results of the Galileo Jupiter mission probe nephelometer experiment,” J. Geophys. Res. 103(E10), 22891–22909 (1998).
https://doi.org/10.1029/98JE00353
39.K. Rages, R. Beebe, and D. Senske, “Jovian stratospheric hazes: The high phase view from Galileo,” Icarus 139(2), 211–226 (1999).
https://doi.org/10.1006/icar.1999.6103
40.T. Saton and K. Kawabata, “Methane band photometry of the faded south equatorial band of Jupiter,” Astrophys. J. 384(1), 298–304 (1992).
41.P. H. Smith, “The vertical structure of the Jovian atmosphere,” Icarus 65(2–3), 264–279 (1986).
https://doi.org/10.1016/0019-1035(86)90139-9
42.C. R. Stoker, “Vertical cloud structure of Jupiter’s equatorial plumes,” Icarus 64, 557–575 (1985).
https://doi.org/10.1016/0019-1035(85)90076-4
43.M. G. Tomasko, B. Bezard, L. Doose, et al., “Measurements of methane absorption by the descent imager/spectral radiometer (DISR) during Its descent through Titan’s atmosphere,” Planet. Space Sci. 56(5), 624–647 (2008).
https://doi.org/10.1016/j.pss.2007.10.009
44.M. G. Tomasko, R. A. West, and N. D. Castillo, “Photometry and polarimetry of Jupiter at large phase angle. I. Analysis of imaging data of a prominent belt and a zone from Pioneer 10,” Icarus 33(3), 558–592 (1978).
https://doi.org/10.1016/0019-1035(78)90191-4
45.S. J. Weidenscilling and J. S. Lewis, “Atmospheric and cloud structures of the Jovian planets,” Icarus 20(4), 465–476 (1973).
https://doi.org/10.1016/0019-1035(73)90019-5
46.R. A. West and M. G. Tomasko, “Spatially resolved methane band photometry of Jupiter. III. Cloud vertical structures for several axisymmetric bands and the Great Red Spot,” Icarus 41(2), 278–292 (1980).
https://doi.org/10.1016/0019-1035(80)90011-1
47.J. H. Woodman, W. D. Cohran, and D. B. Slavsky, “Spatially resolved reflectivities of Jupiter during the 1976 opposition,” Icarus 37, 73–83 (1979).
https://doi.org/10.1016/0019-1035(79)90116-7