HST Imaging of Atmospheric Phenomena Created by the Impact of Comet Shoemaker-Levy 9

Hammel, Heidi B.; Beebe, R. F.; Ingersoll, Andrew P.; Orton, Glenn S.; Mills, J. R.; Simon-Miller, A. A.; Chodas, P. W.; Clarke, J. T.; Jong, E. De; Dowling, T. E.; Harrington, J.; Huber, L. F.; Karkoschka, Erich; Santori, Charles; Toigo, A. D.; Yeomans, Donald K.; West, Robert A.

doi:10.1126/science.7871425

Cited by 215 publications

(169 citation statements)

References 20 publications

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“…Application of results of our consideration is possible for studying, analytically, the collision of comet SL 9 with Jupiter in July 1994: "plumes" have been detected up to maximum heights around 3500 km by the HST (e.g., Hammel et al 1995).…”

Section: Impulse Aerodynamic Deceleration Of Crushed Comet Nuclei In mentioning

confidence: 99%

Stellar ejecta from falling comet-like bodies: young stars

Ibodov

Ibadov

2013

Proc. IAU

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High-resolution spectral observations of young stars with dense protoplanetary discs like Beta Pictoris led to the discovery of variable emission lines of metal atoms, Na, Fe etc., that indicate the presence of fluxes of comet-like evaporating bodies falling onto the stars, FEBs. Assuming the presence of stellar atmospheres similar to the solar one, we show that passages of the FEBs through the stellar chromosphere and photosphere with velocities around 600 km/s will be accompanied by aerodynamic crushing of the nuclei, transverse expansion of the crushed matter, “explosion” of the flattened nuclei in a relatively very thin sub-photosphere layer due to sharp deceleration, and impulse production of a hot plasma. The impulsive rise of the layer's temperature and density lead to the generation of a strong “blast” shock wave and shock wave-induced ejection/eruption of hot plasma into space above the chromosphere. Observations of such impact-induced high-temperature phenomena are of interest for the physics/prognosis of stellar/solar flares as well as physics of comets.

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Section: Impulse Aerodynamic Deceleration Of Crushed Comet Nuclei In mentioning

confidence: 99%

Stellar ejecta from falling comet-like bodies: young stars

Ibodov

Ibadov

2013

Proc. IAU

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“…"Solar" and "lOxsolar" refer to the speed of a gravity wave in the water cloud with solar and lOx solar abundance of water. Redrawn from Hammel et al (1995). r = 2000 km and t = 7000 sec.…”

Section: Observationsmentioning

confidence: 99%

“…A colored version of t he same fi gure appeared in 'Nest et al (1995) and as the cover photo accompanying Ingersoll & K a namori (1995). Hammel et al (1995) show singlefilter images of rings around other impact sites. In Fig .…”

Section: Introductionmentioning

confidence: 99%

“…The dark streak outside and to the west of the ring is the site of the D impact , which occurred 20 hours earlier. Figure 2, which is re-drawn from Hammel et al (1995), shows measurements of the radii of the circular rings that were seen spreading outward from the impact sites. The A. P. Ingersoll & H. Kanamori: Waves from the SL9 impacts 331 FIGURE 1 .…”

Section: Introductionmentioning

confidence: 99%

“…The implications and a comparison of results from the Galileo probe are d escribed in § 5. Hammel et al (1995) analyzed t he atmospheric: waves seen in the HST images . Figure 1 is an orthonormal projection of an image taken in a filt er at 555 nm of the G impact site.…”

Section: Introductionmentioning

confidence: 99%

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Waves from the Shoemaker-Levy 9 impacts

Ingersoll

Kanamori

1996

The Collision of Comet Shoemaker-Levy 9 and Jupiter

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Images of Jupiter taken by the Hubble Space Telescope (HST) reveal two concentric circular rings surrounding five of the impact sites from comet Shoemaker-Levy 9 (SL9). The rings are visible 1.0 to 2.5 hours after the impacts. The outer ring expands at a constant rate of 450 ms-1 . The inner ring expands at about half that speed. The rings appea1· to be waves. Other features (diffuse rings and crescent) further out appear to be debris thrown out by the impact. Sound waves (p-modes), internal gravity waves (g-modes), surface gravity waves (!-modes), and rotational waves ( r-modes) all are excited by the impacts. Most of these waves do not match the slow speed, relatively large amplitude, and narrow width of the observed rings. Ingersoll and Kanamori have argued that internal gravity waves trapped in a stable layer within the putative water cloud are the only waves that can match the observations. If they a re correct, and if moist convection in the water cloud is producing the stable layer, then the 0 /H ratio on Jupite1· is roughly ten times that on the Sun.

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The influence of deep jets on Jupiter's weather layer in a 1.5‐layer shallow‐water model

Thomson

2020

Quart J Royal Meteoro Soc

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The depth of the jet streams seen in Jupiter's outer weather layer has long been debated, with alternative suggestions of confinement to the weather layer and extensions deep into the planet being considered. Interpretation of measurements from NASA's Juno probe have suggested that weather‐layer jets do extend deep into the planet, down to depths of 𝒪 (3,000 km). However, this relies on the assumption that the jet profile does not change its spatial structure with depth, which may not be the case. In this work, we consider a simple 1.5‐layer shallow‐water model of Jupiter‐like jet streams, with prescribed deep jets in the lower layer, and look at the parameters affecting the strength of the coupling between the layers. We find the value of the Rossby deformation scale, L D, to be particularly important, not just in setting the magnitude of variations in layer depth, but also in dictating the effectiveness of radiative damping. We also find the radiative damping timescales, the energy injection rate, and the spacing of deep jets to be important. We combine these findings into our best‐guess simulations of the real Jupiter and find that low latitudes are relatively uncoupled between the layers, with high latitudes being more tightly coupled. These effects can be tied to the smallness of Jupiter's L D and the effectiveness of radiative damping as a coupling mechanism. These simulations do, however, produce equatorial subrotation and eddy‐momentum fluxes unlike those on the real planet. It may be, therefore, that spatially varying forcing and very long radiative damping timescales are required for this model to be more Jupiter‐like.

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HST Imaging of Atmospheric Phenomena Created by the Impact of Comet Shoemaker-Levy 9

Cited by 215 publications

References 20 publications

Stellar ejecta from falling comet-like bodies: young stars

Stellar ejecta from falling comet-like bodies: young stars

Waves from the Shoemaker-Levy 9 impacts

The influence of deep jets on Jupiter's weather layer in a 1.5‐layer shallow‐water model

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