Feasibility of Determining the Composition of Planetary Ices by Far Infrared Observations: Application to Martian Cloud and Surface Ices

Johnson, Brian R.; Atreya, S. K.

doi:10.1006/icar.1996.0027

Cited by 18 publications

(11 citation statements)

References 40 publications

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“…Many studies of water ice indices of refraction have indicated that a broad, lattice absorption feature is present in the 225-230 cm −1 range (Zimmermann and Pimentel 1962, Irvine and Pollack 1968, Bertie et al 1969, Warren 1984, Johnson and Atreya 1996. Such a feature has been seen in spectra taken of martian clouds, and some efforts have been made to model the ice indices in martian-like conditions (Johnson and Atreya 1996).…”

Section: Water Ice Featurementioning

confidence: 97%

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A Detection of Water Ice on Jupiter with Voyager IRIS

Simon-Miller

Conrath

Gierasch

et al. 2000

Icarus

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Section: Water Ice Featurementioning

confidence: 97%

“…Such a feature has been seen in spectra taken of martian clouds, and some efforts have been made to model the ice indices in martian-like conditions (Johnson and Atreya 1996). The existing laboratory measurements span the temperatures that exist in Jupiter's upper atmosphere and troposphere.…”

Section: Water Ice Featurementioning

confidence: 98%

A Detection of Water Ice on Jupiter with Voyager IRIS

Simon-Miller

Conrath

Gierasch

et al. 2000

Icarus

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“…The refractive index for these bands was published by Johnson & Atreya (1996), Hudgins et al (1993), Ehrenfreund et al (1996), or Baratta & Palumbo (1998), among others. The wavelengths positions of these absorption bands agree overall with those of the Hansen (1997Hansen ( , 2005 and Warren (1986) data compilations.…”

Section: Refractive Index Of Co 2 Icementioning

confidence: 99%

Clouds in the atmospheres of extrasolar planets

Kitzmann

Patzer

Rauer

2013

A&A

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Context. Owing to their wavelength-dependent absorption and scattering properties, clouds have a strong impact on the climate of planetary atmospheres. The potential greenhouse effect of CO 2 ice clouds in the atmospheres of terrestrial extrasolar planets is of particular interest because it might influence the position and thus the extension of the outer boundary of the classic habitable zone around main sequence stars. Such a greenhouse effect, however, is a complicated function of the CO 2 ice particles' optical properties. Aims. We study the radiative effects of CO 2 ice particles obtained by different numerical treatments to solve the radiative transfer equation. To determine the effectiveness of the scattering greenhouse effect caused by CO 2 ice clouds, the radiative transfer calculations are performed over the relevant wide range of particle sizes and optical depths, employing different numerical methods. Methods. We used Mie theory to calculate the optical properties of particle polydispersion. The radiative transfer calculations were done with a high-order discrete ordinate method (DISORT). Two-stream radiative transfer methods were used for comparison with previous studies. Results. The comparison between the results of a high-order discrete ordinate method and simpler two-stream approaches reveals large deviations in terms of a potential scattering efficiency of the greenhouse effect. The two-stream methods overestimate the transmitted and reflected radiation, thereby yielding a higher scattering greenhouse effect. For the particular case of a cool M-type dwarf, the CO 2 ice particles show no strong effective scattering greenhouse effect by using the high-order discrete ordinate method, whereas a positive net greenhouse effect was found for the two-stream radiative transfer schemes. As a result, previous studies of the effects of CO 2 ice clouds using two-stream approximations overrated the atmospheric warming caused by the scattering greenhouse effect. Consequently, the scattering greenhouse effect of CO 2 ice particles seems to be less effective than previously estimated. In general, higher order radiative transfer methods are needed to describe the effects of CO 2 ice clouds accurately as indicated by our numerical radiative transfer studies.

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“…(e) From Gerakines et al (1995). Johnson & Atreya (1996), Trotta (1996), Schmitt et al (1998), Maldoni et al (1999), Coustenis et al (1999), and Moore et al (2001). These studies focused mainly on the determination of optical constants and the analysis of the spectral differences between the amorphous and crystalline structures.…”

Section: Introductionmentioning

confidence: 99%

Interstellar ice analogs: band strengths of H₂O, CO₂, CH₃OH, and NH₃in the far-infrared region

Giuliano

Escribano

Martín-Doménech

et al. 2014

A&A

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Context. Whereas observational astronomy now routinely extends to the far-infrared region of the spectrum, systematic laboratory studies are sparse. In particular, experiments on laboratory analogs performed through the years have provided information mainly about the band positions and shapes, while information about the band strengths are scarce and derivable principally from the optical constants. Aims. We measure the band strengths in the far-infrared region of interstellar ice analogs of astrophysically relevant species, such as H 2 O, CO 2 , CH 3 OH, and NH 3 , deposited at low temperature (8-10 K), followed by warm-up, to induce amorphous-crystalline phase transitions when relevant. Methods. The spectra of pure H 2 O, NH 3 , and CH 3 OH ices have been measured in the near-, mid-and far-infrared spectroscopic regions using the Interstellar Astrochemistry Chamber (ISAC) ultra-high-vacuum setup. In addition, far-infrared spectra of NH 3 and CO 2 were measured using a different set-up equipped with a bolometer detector. Band strengths in the far-infrared region were estimated using the corresponding near-and mid-infrared values as a reference. We also performed theoretical calculations of the amorphous and crystalline structures of these molecules using solid state computational programs at density functional theory (DFT) level. Vibrational assignment and mode intensities for these ices were predicted. Results. Infrared band strengths in the 25-500 μm range have been determined for the considered ice samples by direct comparison in the near-and mid-infrared regions. Our values were compared to those we calculated from the literature complex index of refraction. We found differences of a factor of two between the two sets of values. Conclusions. The calculated far-infrared band strengths provide a benchmark for interpreting the observational data from future space telescope missions, allowing the estimation of the ice column densities.

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Feasibility of Determining the Composition of Planetary Ices by Far Infrared Observations: Application to Martian Cloud and Surface Ices

Cited by 18 publications

References 40 publications

A Detection of Water Ice on Jupiter with Voyager IRIS

A Detection of Water Ice on Jupiter with Voyager IRIS

Clouds in the atmospheres of extrasolar planets

Interstellar ice analogs: band strengths of H₂O, CO₂, CH₃OH, and NH₃in the far-infrared region

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Feasibility of Determining the Composition of Planetary Ices by Far Infrared Observations: Application to Martian Cloud and Surface Ices

Cited by 18 publications

References 40 publications

A Detection of Water Ice on Jupiter with Voyager IRIS

A Detection of Water Ice on Jupiter with Voyager IRIS

Clouds in the atmospheres of extrasolar planets

Interstellar ice analogs: band strengths of H2O, CO2, CH3OH, and NH3in the far-infrared region

Contact Info

Product

Resources

About

Interstellar ice analogs: band strengths of H₂O, CO₂, CH₃OH, and NH₃in the far-infrared region