Neptune: Observations of the H2 Quadrupole Lines in the (4–0) Band

Trafton, Laurence M.

doi:10.1007/978-94-010-2206-4_45

Cited by 11 publications

(2 citation statements)

References 14 publications

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“…The first observations of the H 2 quadrupole features in Neptune's atmosphere have been reported by Trafton (1974). He derived an abundance of ~ 450 km amagats~ of H 2 using a simple homogeneous, semi-infinite scattering model.…”

Section: Compositionmentioning

confidence: 97%

The atmospheres of the outer planets

Hunt

1976

Advances in Physics

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Beyond the asteroid belt lie the giant planets, Jupiter, Saturn, Uranus and Neptune and their extensive satellite systems, and Pluto, which is more like a satellite than any of its giant companions. Those large planets are huge, rapidly rotating bodies and seem to Ibrm two separate families.Jupiter and Saturn appear to have an apparently permanently banded appearance of alternating light and dark clouds of rapidly changing colours. The composition of their atmospheres seems to be similar to that of the Sun. Present theories are unable to account for the banded structure, the origin of the colours and the Great Rod Spot situated in the southern Jovian hemisphere. These planets are surrounded by an extensive system of 23 satellites. Two of them, Io of the Galilean satellites, and Titan of the Saturnian system, have atmospheres. The Titan atmosphere is thought to be considerably larger than the present Martian atmosphere.Uranus and Neptune are thought to form a separate family of planets, with less than solar proportions of the light elements, and larger portions of methane than found on Jupiter and Saturn.In this article, which was completed in March 1976, we review our current understanding of the atmospheres of the major planets. CONTENTS

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Section: Compositionmentioning

confidence: 97%

The atmospheres of the outer planets

Hunt

1976

Advances in Physics

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“…In terms of spectroscopy, a notable workhorse of ground-based remote sensing at mid-infrared wavelengths over the past two decades is the Texas Echelon Cross Echelle Spectrograph (TEXES) [286]. Capable of the spectral resolving power of 15,000 to 100,000 (λ/∆λ) in windows between 5 and 25 µm, TEXES has been used to great effect on IRTF and Gemini North to map chemistry and temperatures in Jupiter [287][288][289][290][291][292], Saturn [293][294][295][296], and to a lesser extent Uranus [297,298] and Neptune [70,74], with the exceptionally high spectral resolution needed to resolve fine lines. The resulting quality of retrieved maps of temperature, composition, and aerosols have been noted to even surpass previous spacecraft results for Jupiter [52].…”

Section: Matured Mid-infrared Observing From the Groundmentioning

confidence: 99%

Mid-Infrared Observations of the Giant Planets

Roman

2023

Remote Sensing

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The mid-infrared spectral region provides a unique window into the atmospheric temperature, chemistry, and dynamics of the giant planets. From more than a century of mid-infrared remote sensing, progressively clearer pictures of the composition and thermal structure of these atmospheres have emerged, along with a greater insight into the processes that shape them. Our knowledge of Jupiter and Saturn has benefitted from their proximity and relatively warm temperatures, while the details of colder and more distant Uranus and Neptune are limited as these planets remain challenging targets. As the timeline of observations continues to grow, an understanding of the temporal and seasonal variability of the giant planets is beginning to develop with promising new observations on the horizon.

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