3 edition of Dynamics of the atmospheres of the outer planets found in the catalog.
Dynamics of the atmospheres of the outer planets
1992 by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va.? .
Written in English
|Statement||Peter J. Gierasch.|
|Series||NASA-CR -- 190084., NASA contractor report -- NASA CR-190084.|
|Contributions||United States. National Aeronautics and Space Administration.|
|The Physical Object|
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Reta Beebe, Characteristic zonal winds and long‐lived vortices in the atmospheres of the outer planets, Chaos: An Interdisciplinary Journal of Nonlinear Science, /, 4, 2, (), ().Cited by: "The atmospheres of the four major outer planets involves somewhat different physical processes.
present a summary of current scientific knowledge of both the structure and the dynamics of these atmospheres, moving from the nature of the core to the details of the transfer of radiation and energy in the atmospheres. Brand: Springer-Verlag Berlin Heidelberg. Current knowledge about dynamics and thermal structure on the outer planets is reviewed with the aim of identifying important measurements which sould be made in the post-Voyager era.
The existence of jets and cloud bands is the puzzle that underlies all others. Discussion focuses on the particular case of Jupiter because documentation is most by: The interpretation in terms of basic hydrodynamical Processes of certain prominent observational features exhibited by the atmospheres of major planets should lead in due course to accurate information about the internal structure of these bodies (e.g.
atmospheric depth, angular momentum transfer, energy sources) that may be obtainable in no other by: Email your librarian or administrator to recommend adding this book to your organisation's collection. Planetary Sciences. 2nd edition Atmospheres and Ionospheres of the Outer Planets and Their Satellites.
Springer-Verlag, Heidelberg. pp Jovian atmospheric dynamics: An update after Galileo and Cassini. Rep. Prog. Physics, 68, Comparative Study of the Dynamics of the Outer Planets.
Reta F. Beebe. Pages a comparative study of the atmospheres of the outer planets and Titan, (3) the study of the planetary magnetospheres and their interactions with the solar wind, and (4) the formation and properties of satellites and rings, including their interiors.
Long time base observations of the outer planets are critical in understanding the atmospheric dynamics and evolution of the gas giants.
We propose yearly monitoring of each giant planet for the remainder of Hubble's lifetime to provide a lasting legacy of increasingly valuable data for time-domain studies. The Hubble Space Telescope is a unique asset to planetary science, allowing high.
This comprehensive volume summarises Dynamics of the atmospheres of the outer planets book understanding of the Jovian system, in the light of recent scientific results from the Galileo spacecraft, the Galileo probe, the Cassini spacecraft, the Hubble Space Telescope, and numerous ground-based and theoretical studies.
Chapters are written by leading authorities in the field and cover all aspects of Jupiter, its satellites and s: 1. OPAL is a project to obtain long time baseline observations of the outer planets in Dynamics of the atmospheres of the outer planets book to understand their atmospheric dynamics and evolution as gas giants.
The yearly observations from OPAL throughout the remainder of Hubble's operation will provide a legacy of time-domain images for use by planetary scientists.
All of the outer planets have considerable left over energy from their formation to drive the dynamics of their respective atmospheres. By studying turbulence at the upper cloud layers of these planets, we will learn about how planets transfer heat vertically and evolve in time. The diagrams in Figure show the structure and clouds in the atmospheres of all four jovian planets.
On both Jupiter and Saturn, the temperature near the cloud tops is about K (only a little cooler than the polar caps of Mars). Describe key features of the outer planets and their moons. Compare the outer planets to each other and to Earth. Vocabulary. Galilean moons; Check out NASA’s world book to learn more about Jupiter: Jupiter’s atmosphere is composed of hydrogen and helium.
Deeper within the planet, pressure compresses the gases into a liquid. The elements oxygen, carbon, nitrogen, and sulfur are the most abundant molecule-forming elements in the Sun (after hydrogen), and all are observed in the atmospheres of the giant planets, mostly as H 2 O, CH 4, NH 3, and (for Jupiter) H 2 S.
Water condenses even in Jupiter's atmosphere, at levels that are difficult to probe with infrared. Formation of outer planet atmospheres • Unlike the terrestrial planets, the gas giants were too massive, cold, and distant from the Sun to have lost their original atmospheres • If so, the giant planets are made up of primitive material from the solar nebula - > primary atmospheres • Both Jupiter and the Sun are ~85% hydrogen, ~15% helium.
"The atmospheres of the four major outer planets involves somewhat different physical processes. present a summary of current scientific knowledge of both the structure and the dynamics of these atmospheres, moving from the nature of the core to the details of the transfer of radiation and energy in the atmospheres.
The presentation is. Gravity waves have also been observed in the atmospheres of outer planets. In the Galileo probe, as it descended through the thermosphere and stratosphere of Jupiter, measured a temperature profile that revealed a gravity wavepacket propagating upward.
14. Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others.
Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in. This book has been cited by the following publications. Atmospheres and Ionospheres of the Outer Planets and Their Satellites.
Springer-Verlag, Heidelberg. Atreya, Neutral atmospheres of the giant planets: An overview of composition measurements. Space Sci. Rev., Reviews the state of knowledge of the atmospheres of the giant gaseous planets: Jupiter, Saturn, Uranus, and Neptune.
This work reviews the theories of their formation and contrasts their observed temperature, composition and cloud structures and compares with simple thermodynamic, radiative transfer and dynamical models. The outer planets and their satellites offer several environments of interest to the general problem of the origin and evolution of life.
The characteristics of these environments are reviewed with special emphasis on the structure and composition of planetary and satellite atmospheres. Atmospheric dynamics of the outer planets. Ingersoll AP. Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams.
Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Figure 1 The giant planets Jupiter, Saturn, Uranus, and Neptune (bottom to top, respectively) shown to scale.
PLANETARY ATMOSPHERES / Jupiter and the Outer Planets –1 bar cloud is overlaid by an optically thin. The result is that the outer planets became far more massive and were able to hold very extensive atmospheres of light gases such as hydrogen, as well as light, icy substances such as water (H 2 O), ammonia (NH 3), and methane (CH 4).
The Outer Planets. why does it happen planets outer space and the atmosphere planets book for kids childrens astronomy and space books Posted By Rex Stout Public Library TEXT ID cd1b5 Online PDF Ebook Epub Library dominate the two largest planets jupiter and saturn hence their nickname gas giants uranus and neptune are called ice giants because their interiors contain far more.
The Committee on Space Research (COSPAR) was established in by the International Council for Scientific Unions (ICSU). Among COSPAR's objectives are the promotion of scientific research in space on an international level, with emphasis on the free exchange of results, information, and opinions, and providing a forum, open to all scientists, for the discussion of problems that may affect.
Figure Our Star. The Sun—our local star—is quite average in many ways. However, that does not stop it from being a fascinating object to study. From solar flares and coronal mass ejections, like the one seen coming from the Sun in the top right of this image, the Sun is a highly dynamic body at the center of our solar system.
The four giant planets have generally similar atmospheres, composed mostly of hydrogen and helium. Their atmospheres contain small quantities of methane and ammonia gas, both of which also condense to form clouds.
Deeper (invisible) cloud layers consist of water and possibly ammonium hydrosulfide (Jupiter and Saturn) and hydrogen sulfide (Neptune). Mark Hofstadter Dr. Mark Hofstadter is a Planetary Scientist working at NASA's Jet Propulsion Laboratory in Pasadena, California.
His research focuses on the atmospheres of planets, primarily the giants of the outer solar system (Jupiter, Saturn, Uranus, and Neptune), and on comets. Hofstadter uses both ground- and space-based radio telescopes in the course of his work. The study of extraterrestrial atmospheres is an active field of research, both as an aspect of astronomy and to gain insight into Earth's atmosphere.
In addition to Earth, many of the other astronomical objects in the Solar System have include all the gas giants, as well as Mars, Venus, and l moons and other bodies also have atmospheres, as do comets and the Sun.
The outer or Jovian planets have reducing atmospheres containing large amounts of hydrogen, which strongly suggest an origin similar to that of the solar system itself. Comets probably represent a distinct third category, originating from evaporated icy conglomerate material.
Worse, the inner planet atmospheres would be much warmer than the outer planets so the lighter elements (e.g. hydrogen) would be bouncing around at speeds beyond any of our inner planet's escape velocities.
So, for the terrestrial planets, it was only the heavier elements that stuck. Uranus and Neptune, respectively the seventh and eighth planets from the Sun, are estimated to contain 10 percent to 15 percent methane under an outer atmosphere. This book reviews the current state of knowledge of the atmospheres of the giant gaseous planets: Jupiter, Saturn, Uranus, and Neptune.
The current theories of their formation are reviewed and their recently observed temperature, composition and cloud structures are contrasted and compared with simple thermodynamic, radiative transfer and dynamical models.
Atmospheric entry is the movement of an object from outer space into and through the gases of an atmosphere of a planet, dwarf planet, or natural are two main types of atmospheric entry: uncontrolled entry, such as the entry of astronomical objects, space debris, or bolides; and controlled entry (or reentry) of a spacecraft capable of being navigated or following a.
why does it happen planets outer space and the atmosphere planets book for kids Posted By Stephenie Meyer Publishing TEXT ID fd Online PDF Ebook Epub Library concussion wave from the proto suns initial ignition is thought to have blown away the thick atmospheres of the inner protoplanets but left the outer planets untouched.
Only the Sun and the massive outer planets had enough gravity to keep hydrogen and helium from drifting away. All of the outer planets have numerous moons. All of the outer planets also have planetary rings, which are rings of dust and other small particles encircling a planet in a thin plane. Only the rings of Saturn can be easily seen from Earth.
why does it happen planets outer space and the atmosphere planets book for kids Posted By Paulo Coelho Public Library TEXT ID a Online PDF Ebook Epub Library our solar system space junk made entirely of elements from the solar nebula the asteroids and meteorites orbiting our sun offer incredible insight into the origin of our solar.
The outer layer of Saturn, Jupiter, Neptune and Uranus, are hot just like the Earth’s likely due to electric current at the planets’ poles, according to a study, which is the most complete mapping yet of both temperature and density of a gas giant’s upper atmosphere.
extra solar planets the detection formation evolution and dynamics of planetary systems scottish graduate series Posted By Gérard de Villiers Publishing TEXT ID cff9 Online PDF Ebook Epub Library solar system planets exoplanet detection observation of exoplanet atmospheres biomarkers and detection of life planet earth remote sensing techniques and new planetary.
All of the terrestrial planets have densities around 4 - 5 g/cc. The planet with the lowest density is Saturn. Its density is so low that a planet of solid water or ice would be more dense. That includes the dynamics and chemical makeup of planets in orbit around the hyperdense remains of a white dwarf.
If planetary material enters the atmosphere, we .Our planetary science program focuses on solar system bodies and their atmospheres. Using observational data from space- and ground-based instruments and numerical and theoretical analysis, we investigate the origin, evolution, and current state of solar system objects including Mars and Venus, Earth’s Moon, asteroids, comets, jovian Trojans, the satellites of the outer planets, and Pluto.