Four micron infrared observations of the comet Shoemaker‐Levy 9 collision with Jupiter at the Zelenchuk Observatory: Spectral evidence for a stratospheric haze and determination of its physical properties

Rosenqvist, J.; Biraud, Y.; Cuisenier, M.; Marten, A.; Hidayat, Taufiq; Chountonov, G. A.; Moreau, D.; Müller, C.; Maslov, I. A.; Ackerman, M.; Balega, Y. Y.; Korablev, Oleg

doi:10.1029/95gl00950

Cited by 6 publications

(2 citation statements)

References 3 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A worldwide observing campaign brought forth many interesting results on the physical properties of the debris Ortiz et al, 1995;Rosenqvist et al, 1995;Banfield et al, 1996;Muñoz et al, 1996;Molina et al, 1997;Pryor et al, 1997b). The review by West (1996) indicates the following characteristics: The mean particle radius is in the range 0.1-0.3 µm.…”

Section: Aftermath Of the Sl9 Collisionmentioning

confidence: 98%

Aerosols on the Giant Planets and Titan

Courtin

2005

Space Sci Rev

View full text Add to dashboard Cite

On the giant planets and Titan, like on the terrestrial planets, aerosols play an important part in the physico-chemistry of the upper atmosphere (P ≤ 0.5 bar). Above all, aerosols significantly affect radiative transfer processes, mainly through light scattering, thus influencing the atmospheric energy budget and dynamics. Because there is usually significant coupling between atmospheric circulation and haze production, aerosols may constitute useful tracers of atmospheric dynamics. More generally, since their production is directly linked to some kind of energy deposition, their study may also provide clues to external sources of energy as well as their variability. Finally, aerosols indirectly influence other processes such as cloud formation and disequilibrium chemistry, by acting either as condensation nuclei or as reaction sites for surface chemistry. Here, I present a review of observational and modeling results based on remote sensing data, and also some insights derived from laboratory simulations. Despite our knowledge of the effects of aerosols in outer planetary atmospheres, however, relatively little is understood about the pathways which produce them, either endogenously (as end-products of gas-phase photochemical or shock reactions) or exogenously (as residues of meteroid ablation).

show abstract

Section: Aftermath Of the Sl9 Collisionmentioning

confidence: 98%

Aerosols on the Giant Planets and Titan

Courtin

2005

Space Sci Rev

View full text Add to dashboard Cite

show abstract

“…Palomar. Rosenqvist et al (1995) obtained spectra near 4 /jm of the area around the W and K impact sites with the 6 m telescope of the Special Astronomical Observatory of Zelenchuk.…”

Section: Introductionmentioning

confidence: 99%

Particles in Jupiter's atmosphere from the impacts of Comet P/Shoemaker-Levy 9

West

1996

International Astronomical Union Colloquium

View full text Add to dashboard Cite

The dark clouds that were easily seen in small telescopes after the comet impacts were caused by small particles which were deposited in Jupiter's stratosphere. Observations from the Hubble Space Telescope and from ground-based instruments at visible and infrared wavelengths indicate that the mean radius of the particles is in the range 0.1 to 0.3 /im, and the total volume of particles is approximately the same as that for a 1-km diameter sphere. In the dark core regions of freshly-formed impacts, the particles are distributed over a large vertical extent, between about 1 mb and 200 mb or deeper. The diffuse outlying haze is confined to the high-altitude end of the range. Such a distribution probably reflects different methods of emplacement of the debris as a function of distance from the impact. The color of the particles, and their volatility as required to make waves visible, suggest an organic material as the main constituent. These relatively volatile materials are thought to have condensed onto more refractory grains after the plume material cooled, some 30 minutes or more after impact. The most refractory materials expected to condense from an evolving fireball are AI2O3, magnesium and iron silicates, and soot, depending on the C/O ratio. A silicate spectral feature was observed, confirming that cometary material was incorporated into the grains, although silicate grains make up only 10-

show abstract

Nature and Source of Organic Matter in the Shoemaker–Levy 9 Jovian Impact Blemishes

Wilson¹,

Sagan²

1997

Icarus

View full text Add to dashboard Cite

Four micron infrared observations of the comet Shoemaker‐Levy 9 collision with Jupiter at the Zelenchuk Observatory: Spectral evidence for a stratospheric haze and determination of its physical properties

Cited by 6 publications

References 3 publications

Aerosols on the Giant Planets and Titan

Aerosols on the Giant Planets and Titan

Particles in Jupiter's atmosphere from the impacts of Comet P/Shoemaker-Levy 9

Nature and Source of Organic Matter in the Shoemaker–Levy 9 Jovian Impact Blemishes

Contact Info

Product

Resources

About