Coordinated 1996 HST and IRTF Imaging of Neptune and Triton III. Neptune's Atmospheric Circulation and Cloud Structure

Sromovsky, Lawrence A.; Fry, P. M.; Dowling, T. E.; Baines, K. H.; Limaye, S. S.

doi:10.1006/icar.2000.6564

Cited by 80 publications

(85 citation statements)

References 43 publications

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“…We immediately note that atmospheric features tend to be distributed preferentially along bands of constant latitude, with increased prevalence at mid-latitudes, in agreement with previous observations (e.g. Sromovsky et al 2001b;Max et al 2003;Irwin et al 2011;Martin et al 2012). In addition to clouds at roughly the same latitudes as Martin et al (2012), we observe clouds at ∼40 • N. In all images there is an absence of cloud features just south of the equator, in agreement with previous observations (e.g.…”

Section: Observations and Data Reductionsupporting

confidence: 92%

“…Feature morphology changes so dramatically that we cannot with certainty identify the same features present on both nights, as has been noted in previous observations (e.g. Sromovsky et al 2001b;Karkoschka 2011b).…”

Section: Observations and Data Reductionmentioning

confidence: 54%

“…The wind velocities derived from individual features in Neptune's atmosphere since Voyager 2 are observed to remain consistent with this smooth Voyager wind profile, with the exception of features which display significant deviation in zonal velocity, presumably due to mechanisms such as vertical wind shear, wave phenomena, or eddy motions, and which have sometimes been associated with structures such as dark spots (e.g. Hammel & Lockwood 1997;Sromovsky et al 2001bSromovsky et al ,c, 2002. Sromovsky et al (2001c) found deviations from the smooth Voyager wind profile in 1998 HST observations which were consistent with observations in 1995 and 1996 (Sromovsky et al 2001b), but they concluded that more measurements are needed to confirm a change in Neptune's zonal wind structure.…”

Section: Introductionmentioning

confidence: 67%

“…Hammel & Lockwood (1997) studied the zonal motions of cloud features in 1995 HST images, along with those for features found in Voyager images (Limaye & Sromovsky 1991;Hammel 1989), Voyager radio occultation data (Lindal et al 1990), 1991 HST data (Sromovsky et al 1995), and ground-based data (see Sromovsky et al (1993) Table VII) and noted that all measurements show dispersion in velocities in narrow bands of latitude, which the authors indicated as evidence for shear, wave phenomena, or other local disturbances. Sromovsky et al (2001b) found significant deviation in zonal velocities from the smooth Voyager wind profile for features tracked in HST data from 1994, 1995, and 1996. The authors found deviation in 1996 HST data to be mostly associated with a Great Dark Spot at 32 • N, thought to be the same dark spot seen in 1994 HST images of Neptune at 30 • N (Hammel et al 1995).…”

Section: Introductionmentioning

confidence: 82%

“…Hammel & Lockwood 1997;Sromovsky et al 2001bSromovsky et al ,c, 2002. Sromovsky et al (2001c) found deviations from the smooth Voyager wind profile in 1998 HST observations which were consistent with observations in 1995 and 1996 (Sromovsky et al 2001b), but they concluded that more measurements are needed to confirm a change in Neptune's zonal wind structure.…”

Section: Introductionmentioning

confidence: 99%

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Dispersion in Neptune’s zonal wind velocities from NIR Keck AO observations in July 2009

Fitzpatrick

Pater

Luszcz‐Cook

et al. 2013

Astrophys Space Sci

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We report observations of Neptune made in H-(1.4-1.8 µm) and K'-(2.0-2.4 µm) bands on 14 and 16 July 2009 from the 10-m W.M. Keck II Telescope using the near-infrared camera NIRC2 coupled to the Adaptive Optics (AO) system. We track the positions of 54 bright atmospheric features over a few hours to derive their zonal and latitudinal velocities, and perform radiative transfer modeling to measure the cloud-top pressures of 50 features seen simultaneously in both bands.We observe one South Polar Feature (SPF) on 14 July and three SPFs on 16 July at ∼65 • S. The SPFs observed on both nights are different features, consistent with the high variability of Neptune's storms.There is significant dispersion in Neptune's zonal wind velocities about the smooth Voyager wind profile fit of Sromovsky et al., Icarus 105, 140 (1993), much greater than the upper limit we expect from vertical wind shear, with the largest dispersion seen at equatorial and southern mid-latitudes. Comparison of feature pressures vs. residuals in zonal velocity from the smooth Voyager wind profile also directly reveals the dominance of mechanisms over vertical wind shear in causing dispersion in the zonal winds.Vertical wind shear is not the primary cause of the difference in dispersion and deviation in zonal veloc-

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Section: Observations and Data Reductionsupporting

confidence: 92%

Section: Observations and Data Reductionmentioning

confidence: 54%

Section: Introductionmentioning

confidence: 67%

Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Dispersion in Neptune’s zonal wind velocities from NIR Keck AO observations in July 2009

Fitzpatrick

Pater

Luszcz‐Cook

et al. 2013

Astrophys Space Sci

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Uranus and Neptune

Sromovsky

2003

Encyclopedia of Space Science and Technology

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Uranus and Neptune, were the first planets discovered by telescopic observation. They are of Jovian Planets similar size and much more massive than Earth (by factors of 14.5 and 17) but are still far less massive than Jupiter (by factors of 22 and 18). Both have deep atmospheres dominated by hydrogen, but unlike Jupiter and Saturn, most of their mass consists of rocky and icy components, which are in fluid form due to high interior temperatures. Both have ring systems, a diverse system of satellites, unusual tilted and offset magnetic fields, and similar atmospheric circulations. Their blue colors distinguish them from the pale tans of Jupiter and Saturn. But they also differ significantly from each other; they have very different obliquities (spin axis inclinations relative to their orbital planes), vastly different internal heat fluxes, and remarkably different weather patterns. These simularities and differences are discussed in detail in this article.

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Coordinated 1996 HST and IRTF Imaging of Neptune and Triton II. Implications of Disk-Integrated Photometry

Sromovsky

Fry

Baines

et al. 2001

Icarus

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Coordinated 1996 HST and IRTF Imaging of Neptune and Triton III. Neptune's Atmospheric Circulation and Cloud Structure

Cited by 80 publications

References 43 publications

Dispersion in Neptune’s zonal wind velocities from NIR Keck AO observations in July 2009

Dispersion in Neptune’s zonal wind velocities from NIR Keck AO observations in July 2009

Uranus and Neptune

Coordinated 1996 HST and IRTF Imaging of Neptune and Triton II. Implications of Disk-Integrated Photometry

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