ဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများ

Wikipedia မှ
ဤနေရာသို့သွားရန် - အ​ညွှန်း​, ရှာ​ဖွေ​ရန်​
Translation to english arrow icon This article needs translation into Burmese.

This article is written in a language other than Burmese.

Please see this article's entry on Pages needing translation into Burmese for discussion. If the article is not rewritten in Burmese within the next two weeks it will be listed for deletion.
နေအဖွဲ့အစည်းရှိ ဓာတ်ငွေ့ဂြိုဟ်ဘီလူး၄ခုအားနေနှင့်စကေးကိုက်နှိုင်းယှဉ်ပြထားပုံ
ဂျူပီတာ၊ ကွင်းများနှင့်စေတန်၊ ယူရေးနပ်စ်၊ နက်ပကျွန်းဂြိုဟ်များပုံ

ဓာတ်ငွေ့ဂြိုဟ်ဘီလူးဆိုသည်မှာကျောက်သို့မဟုတ်အခြားအခဲပစ္စည်းများမပါဘဲ ဓာတ်ငွေ့သက်သက်ပြီးသော ကြီးမားလှသောဂြိုဟ်ကြီးဖြစ်သည်။ နေအဖွဲ့အစည်းတွင် ဓာတ်ငွေ့ဂြိုဟ်ဘီလူးနှစ်ခုပါဝင်သည်။ ဂျူပီတာ(ကြာသပတေးဂြိုဟ်)နှင့်စေတန်(စနေဂြိုဟ်)တို့ဖြစ်ကြသည်။ အခြားဂြိုဟ်ဘီလူးနှစ်ခု ယူရေးနပ်စ်နှင့်နက်ပကျွန်းတို့မှာ ဓာတ်ငွေ့ဂြိုဟ်များမဟုတ်ဘဲ ရေခဲဂြိုဟ်ဘီလူးများဖြစ်ကြသည်။ များစွာသော နေအဖွဲ့အစည်းပြင်ပဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများတွင် ထပ်တူကျသောဂြိုဟ်ပတ်လမ်းများရှိကြသည်။

ကမ္ဘာ့ဒြပ်ထု၁၀ထက်ကျော်လျှင် ဂြိုဟ်ဘီလူများဟုသတ်မှတ်သည်။ [၁] Lower-mass gassy planets are sometimes called "gas dwarfs".[၂]

Objects large enough to start deuterium fusion (above 13 Jupiter masses for solar composition) are called brown dwarfs and these occupy the mass range between that of large gas giants and the lowest-mass stars. The 13 Jupiter mass (MJ) cutoff is a rule of thumb rather than something of precise physical significance. Larger objects will burn most of their deuterium and smaller ones will burn only a little, and the Template:Jupiter mass value is somewhere in between. The amount of deuterium burnt depends not only on mass but also on the composition of the planet, especially on the amount of helium and deuterium present.[၃] The Extrasolar Planets Encyclopaedia includes objects up to 25 Jupiter masses, and the Exoplanet Data Explorer up to 24 Jupiter masses.

ဖော်ပြချက်[ပြင်​ဆင်​ရန်​]

ဂြိုဟ်များ၏အတွင်းဖက်ဖြတ်ပိုင်းပုံ၊ ဂျူပီတာဂြိုဟ်အတွင်းဖက်တွင် သတ္ထုဟိုက်ဒရိုဂျင်အလွှာပါဝင်သည်

ဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများသည် အလေးချိန်များပြားပြီး ဟိုက်ဒရိုဂျင်နှင့်ဟီလီယမ်ဓာတ်ငွေ့များပါသည့် ထူထပ်သောလေထုရှိကြသည်။ They may have a dense molten core of rocky elements or the core may have completely dissolved and dispersed throughout the planet if the planet is hot enough.[၄] The hydrogen and helium in "traditional" gas giants like Jupiter and Saturn constitutes most of the planet, whereas the hydrogen/helium only makes up an outer envelope on Uranus and Neptune which are sometimes called ice giants, as they are mostly composed of water, ammonia, and methane molten ices.

Among extrasolar planets, Hot Jupiters are gas giants that orbit very close to their stars and thus have a very high surface temperature. Hot Jupiters are currently the most common form of extrasolar planet known, perhaps due to the relative ease of detecting them.

ဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများသည် အခဲမျက်နှာပြင်မရှိဟုဆိုနိုင်သည်။ Gas giants are commonly said to lack solid surfaces, but it is closer to the truth to say that they lack surfaces altogether since the gases that make them up simply become thinner and thinner with increasing distance from the planets' centers, eventually becoming indistinguishable from the interplanetary medium. Therefore landing on a gas giant may or may not be possible, depending on the size and composition of its core.

Belt-zone circulation[ပြင်​ဆင်​ရန်​]

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 an internal updraft, and are high-pressure regions. The belts are the darker bands. They are lower in the atmosphere, and have an internal downdraft. They are low-pressure regions. These structures are somewhat analogous to high- and low-pressure cells in Earth's atmosphere, but they have a very 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 is 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.

ဂျူပီတာနှင့်စေတန်ဂြိုဟ်[ပြင်​ဆင်​ရန်​]

စေတန်ဂြိုဟ်မြောက်ဝင်ရိုးစွန်းရှိဝဲကတော့ပုံ

ဂျူပီတာဂြိုဟ် နှင့် စေတန်ဂြိုဟ် တို့တွင် အဓိကအားဖြင့် ဟိုက်ဒရိုဂျင်နှင့်ဟီလီယမ်ဓာတ်ငွေ့များပါဝင်သည်။ , with heavier elements making up between 3 and 13 percent of the mass.[၅] Their structures are thought to consist of an outer layer of molecular hydrogen, surrounding a layer of liquid metallic hydrogen, with a probable molten core with a rocky composition. The outermost portion of the hydrogen atmosphere is characterized by many layers of visible clouds that are mostly composed of 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 is thought to consist of heavier elements at such high temperatures (20,000 K) and pressures that their properties are poorly understood.[၅]

ယူရေးနပ်စ်နှင့်နက်ပကျွန်း[ပြင်​ဆင်​ရန်​]

Template:See also

Uranus and Neptune have distinctly different interior compositions from Jupiter and Saturn. Models of their interior begin with a hydrogen-rich atmosphere that extends from the cloud-tops down to about 85% of Neptune's radius and 80% of Uranus's. Below the point is predominantly "icy", composed of water, methane and ammonia. There is also some rock and gas but various proportions of ice/rock/gas could mimic pure ice so the exact proportions are unknown.[၆]

Very hazy atmosphere layers with a small amount of methane gives them aquamarine colors such as baby blue and ultramarine colors respectively. Both have magnetic fields that are sharply inclined to their axes of rotation.

Unlike the other gas giants, Uranus has an extreme tilt that causes its seasons to be severely pronounced. The two planets have other subtle but important differences. Uranus has more hydrogen and helium than Neptune, despite being less massive overall. Neptune is therefore denser and has much more internal heat, and a more active atmosphere. The Nice model in fact suggests that Neptune formed closer to the Sun than Uranus did, and would therefore have more heavy elements.

နေအဖွဲ့အစည်းအပြင်ဖက်ရှိဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများ[ပြင်​ဆင်​ရန်​]

Comparison of sizes of planets of a given mass with different compositions

Template:See also 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.

အေးခဲနေသောဓာတ်ငွေ့ဂြိုဟ်ဘီလူးများ[ပြင်​ဆင်​ရန်​]

A cold hydrogen-rich gas giant more massive than Jupiter but less than about Template:Earth mass (Template:Jupiter mass), will be just slightly larger in volume than Jupiter.[၇] For masses above Template:Earth mass, degenerate pressure will cause the planet to shrink.[၇] Kelvin–Helmholtz heating can cause a gas giant, such as Jupiter, to radiate more energy than it receives from its host star.[၈][၉]

သေးငယ်သောဓာတ်ငွေ့ဂြိုဟ်များ[ပြင်​ဆင်​ရန်​]

ပန်းချီဆရာ၏စိတ်ကူးယဉ်ဖော်ပြချက် 79 Ceti b, the first extrasolar gas giant found with a minimum mass less than Saturn.

Although the words "gas" and "giant" are often combined, hydrogen planets need not be as large as the familiar gas giants from the Solar System. However, smaller gas planets and planets closer to their star will lose atmospheric mass more quickly via hydrodynamic escape than larger planets or planets farther out.[၁၀][၁၁]

The smallest known extrasolar planet that is likely a "gas planet" is Kepler-11f, at about 2.3 Earth masses.

Terminology[ပြင်​ဆင်​ရန်​]

Jupiter

The term gas giant was coined in 1952 by the science fiction writer James Blish. Arguably it is something of a misnomer, since throughout most of the volume of these planets all the components (other than solid materials in the core) are above the critical point and therefore there is no distinction between liquids and gases. Fluid planet would be a more accurate term. Jupiter is an exceptional case, having metallic hydrogen near the center, but much of its volume is hydrogen, helium and traces of other gases above their critical points. The observable atmospheres of any of these planets (at less than unit optical depth) are quite thin compared to the planetary radii, only extending perhaps one percent of the way to the center. Thus the observable portions are gaseous (in contrast to Mars and Earth, which have gaseous atmospheres through which the crust may be seen).

The rather misleading term has caught on because planetary scientists typically use "rock", "gas", and "ice" as shorthands for classes of elements and compounds commonly found as planetary constituents, irrespective of what phase the matter may appear in. In the outer solar system, hydrogen and helium are referred to as "gases"; water, methane, and ammonia as "ices"; and silicates and metals as "rock". When deep planetary interiors are considered, it may not be far off to say that, by "ice" astronomers mean oxygen and carbon, by "rock" they mean silicon, and by "gas" they mean hydrogen and helium.

The alternative term jovian planet refers to the Roman god Jupiter—the genitive form of which is Jovis, hence Jovian—and was intended to indicate that all of these planets were similar to Jupiter. However, the many ways in which Uranus and Neptune differ from Jupiter and Saturn have led some to use the term only for the planets similar to the latter two.

With this terminology in mind, some astronomers are starting to refer to Uranus and Neptune as "ice giants" to indicate the apparent predominance of the "ices" (in liquid form) in their interior composition.[၁၂]

See also[ပြင်​ဆင်​ရန်​]

Template:Portal

Notes[ပြင်​ဆင်​ရန်​]

Relative masses of the gas giants of the Solar System
  1. (June 2008) "The quest for very low-mass planets", A Decade of Extrasolar Planets around Normal Stars, Space Telescope Science Institute Symposium Series (No. 19). Cambridge University Press, 20. ISBN 978-0-521-89784-6. 
  2. StarGen - Solar System Generator, 2003
  3. The Deuterium-Burning Mass Limit for Brown Dwarfs and Giant Planets, David S. Spiegel, Adam Burrows, John A. Milsom
  4. Rocky core solubility in Jupiter and giant exoplanets, Hugh F. Wilson, Burkhard Militzer, 2011
  5. ၅.၀ ၅.၁ The Interior of Jupiter, Guillot et al., in Jupiter: The Planet, Satellites and Magnetosphere, Bagenal et al., editors, Cambridge University Press, 2004
  6. L. McFadden, P. Weissman, T. Johnson (2007). Encyclopedia of the Solar System (2nd ed.). Academic Press. ISBN 978-0-12-088589-3. 
  7. ၇.၀ ၇.၁ Seager, S.; Kuchner, M.; Hier-Majumder, C. A.; Militzer, B. (2007). "Mass-Radius Relationships for Solid Exoplanets". The Astrophysical Journal 669 (2): 1279–1297. doi:10.1086/521346. Bibcode2007ApJ...669.1279S. 
  8. Patrick G. J. Irwin (2003). Giant Planets of Our Solar System: Atmospheres, Composition, and Structure. Springer. ISBN 3-540-00681-8. 
  9. Class 12 - Giant Planets - Heat and Formation. 3750 - Planets, Moons & Rings. Colorado University, Boulder (2004). Retrieved on 2008-03-13
  10. "TRANSONIC HYDRODYNAMIC ESCAPE OF HYDROGEN FROM EXTRASOLAR PLANETARY ATMOSPHERES" (March 10, 2005). The Astrophysical Journal 621: 1049–1060. doi:10.1086/427204. Bibcode2005ApJ...621.1049T. Template:Citeseerx. 
  11. Mass-radius relationships for exoplanets, Damian C. Swift, Jon Eggert, Damien G. Hicks, Sebastien Hamel, Kyle Caspersen, Eric Schwegler, and Gilbert W. Collins
  12. Jack J. Lissauer, David J. Stevenson (2006). Formation of Giant Planets (PDF). NASA Ames Research Center; California Institute of Technology. Retrieved on 2006-01-16

References[ပြင်​ဆင်​ရန်​]

  • Episode "Giants" on The Science Channel TV show Planets
  • SPACE.com: Q&A: The IAU's Proposed Planet Definition 16 August 2006 2:00 am ET
  • BBC News: Q&A New planets proposal Wednesday, 16 August 2006, 13:36 GMT 14:36 UK

External links[ပြင်​ဆင်​ရန်​]

မြန်မာဝစ်ရှင်နရီ
မြန်မာ ဝစ်ရှင်နရီ တွင် ဤစကားလုံးများအတွက်
အဓိပ္ပါယ်ဖွင့်ဆိုချက် ရှိသည် -

Template:Solar System Template:Exoplanet