Gas giant Totally Explained

Everything about Gas Giant totally explained

A gas giant (sometimes also known as a Jovian planet or Jovial planet after the planet Jupiter) is a large planet that isn't primarily composed of rock or other solid matter. There are four gas giants in our Solar System; Jupiter, Saturn, Uranus, and Neptune. Uranus and Neptune may be considered a separate subclass of giant planets, 'ice giants', as they're mostly composed of ice, rock, as well as gases of water, ammonia, and methane, unlike the "traditional" gas giants Jupiter or Saturn. While all four planets lack a solid surface, Uranus and Neptune have a lower proportion of hydrogen and helium.
A gas giant may have a rocky or metallic core—in fact, such a core is thought to be required for a gas giant to form—but the majority of its mass is hydrogen and helium, with traces of water, methane, ammonia, and other hydrogen compounds. (Although familiar to us as gases on Earth, these constituents are assumed to be compressed into liquids or solids deep in a gas giant's atmosphere.)
Unlike rocky planets, which have a clearly defined surface, gas giants do not; their atmospheres simply become gradually denser toward the core, perhaps with liquid or liquid-like states in between. Therefore, one can't "land on" such planets in the traditional sense. Terms such as diameter, surface area, volume, surface temperature, and surface density may refer only to the outermost layer visible from space.

Common features

The four solar system gas giants share a number of features. All have atmospheres that are mostly hydrogen and helium and that gradually blend into the liquid interior at pressures greater than the critical pressure, so that there's no clear boundary between atmosphere and body. In this regard, our four gas giants exemplify the classic "matter phase-gradient" in the materials sciences. They have very hot interiors, ranging from about 7,000 kelvin (K) for Uranus and Neptune to over 20,000 K for Jupiter. This great heat means that beneath their atmospheres the planets are most likely entirely liquid. Thus, when discussions refer to a "rocky core," one shouldn't picture a ball of solid rock, or even (at 20,000 K) liquid rock. Rather, what is meant is a region in which the concentration of heavier elements such as iron and nickel is greater than that in the rest of the planet.
All four planets rotate relatively rapidly, which causes wind patterns to break up into east-west bands or stripes. These bands are prominent on Jupiter, muted on Saturn and Neptune, and barely detectable on Uranus.
All four planets are accompanied by elaborate systems of rings and moons. Saturn's rings are the most spectacular and were the only ones known before the 1970s. As of 2006, Jupiter is known to have the most moons with sixty-three.

Belt-Zone Circulation

The bands seen in the Jovian atmosphere are due to counter-circulating streams of material called zones and belts, encircling the planet parallel to its equator.
The zones are the lighter bands, and are at higher altitudes in the atmosphere. They have internal updraft, and are high-pressure regions. The belts are the darker bands. They are lower in the atmosphere, and have internal downdraft. They are low-pressure regions. These structures are somewhat analogous to high- and low-pressure cells in Earth's atmosphere, but they've a much different structure — latitudinal bands that circle the entire planet, as opposed to small confined cells of pressure. This appears to be a result of the rapid rotation and underlying symmetry of the planet. There are no oceans or landmasses to cause local heating, and the rotation speed is much faster than it's on Earth.
There are smaller structures as well; spots of different sizes and colors. On Jupiter, the most noticeable of these features is the Great Red Spot, which has been present for at least 300 years. These structures are huge storms. Some such spots are thunderheads as well. Astronomers have observed lightning from a number of them.

Jupiter and Saturn

Jupiter and Saturn consist mostly of hydrogen and helium, with heavier elements making up between 3 and 13 percent of the mass . Their structures are thought to consist of an outer layer of molecular hydrogen, surrounding a layer of liquid metallic hydrogen, with a probable rocky core. The outermost portion of the hydrogen atmosphere is characterized by many layers of visible clouds (mostly water and ammonia). The metallic hydrogen layer makes up the bulk of each planet, and is described as "metallic" because the great pressure turns hydrogen into an electrical conductor. The core, if it exists, consists of heavier elements at such high temperatures (20000K) and pressures that their properties are poorly understood

Extrasolar gas giants

Because of the limited techniques currently available to detect extrasolar planets, many of those found to date have been of a size associated, in our solar system, with gas giants. Because these large planets are inferred to share more in common with Jupiter than with the other gas giant planets, some have claimed that "Jovian planet" is a more accurate term for them. Many of the extrasolar planets are much closer to their parent stars and hence much hotter than gas giants in the solar system, making it possible that some of those planets are a type not observed in our solar system. Considering the relative abundances of the elements in the universe (approximately 98% hydrogen and helium), it would be surprising to find a predominantly rocky planet more massive than Jupiter. On the other hand, previous models of planetary system formation suggested that gas giants would be inhibited from forming as close to their stars as have many of the new planets that have been observed.

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