File:Gasdwarf.jpg

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Simulated view of a mini-Neptune or "gas dwarf"

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DescriptionGasdwarf.jpg	English: Simulated view of a mini-Neptune or "gas dwarf"
Date	13 November 2021, 17:04:08
Source	Own work
Author	Pablo Carlos Budassi

Planet concept illustrated especially for Wikimedia Commons by Pablo Carlos Budassi. Source: https://www.pablocarlosbudassi.com/2021/02/planet-types.html Background image by ESO/Serge Brunier: https://commons.wikimedia.org/wiki/File:ESO_-_Milky_Way.jpg Suggestions for improving this image are welcome: pablocarlosbudassi@gmail.com

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	Date/Time	Dimensions	User	Comment
current	12:50, 15 August 2023	1,080 × 1,080 (394 KB)	Celestialobjects (talk \| contribs)	improved cloud colors
	15:28, 11 July 2023	1,080 × 1,080 (585 KB)	Celestialobjects (talk \| contribs)	more detail and stars background
	23:08, 13 November 2021	1,080 × 1,080 (236 KB)	Celestialobjects (talk \| contribs)	Uploaded own work with UploadWizard

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The following other wikis use this file:

Usage on af.wikipedia.org
- Mini-Neptunus
Usage on ca.wikipedia.org
- Minineptú
Usage on en.wikipedia.org
- Mini-Neptune
Usage on fi.wikipedia.org
- Kaasukääpiö
Usage on fi.wikibooks.org
- Wikijunior Tähtitiede/Mini-Neptunus
Usage on gl.wikipedia.org
- Mini-Neptuno
Usage on th.wikipedia.org
- ดาวมินิเนปจูน
Usage on uk.wikipedia.org
- Мінінептун
Usage on vi.wikipedia.org
- Tiểu Sao Hải Vương

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Author	Pablo Carlos Budassi
Copyright holder	1080px x 1080px version lisenced under Creative Commons Attribution-Share Alike 4.0 International. Background image by ESO/S. Brunier - Creative Commons Attribution 4.0 International
Headline	Artist's impression of Mini-Neptune (gas dwarf)
Credit/Provider	Created by artist Pablo Carlos Budassi in 2023 (@pablocarlosbudassi)
Source	https://pablocarlosbudassi.com
Image title	A Mini-Neptune (sometimes known as a gas dwarf or transitional planet) is a planet less massive than Neptune but resembling Neptune in that it has a thick hydrogen–helium atmosphere, probably with deep layers of ice, rock or liquid oceans (made of water, ammonia, a mixture of both, or heavier volatiles).A gas dwarf is a gas planet with a rocky core that has accumulated a thick envelope of hydrogen, helium, and other volatiles, having, as a result, a total radius between 1.7 and 3.9 Earth radii. The term is used in a three-tier, metallicity-based classification regime for short-period exoplanets, which also includes the rocky, terrestrial-like planets with less than 1.7 RE and planets greater than 3.9 RE, namely ice giants and gas giants.Theoretical studies of such planets are loosely based on knowledge about Uranus and Neptune. Without a thick atmosphere, it would be classified as an ocean planet instead. An estimated dividing line between a rocky planet and a gaseous planet is around 1.6–2.0 Earth radii. Planets with larger radii and measured masses are mostly low-density and require an extended atmosphere to simultaneously explain their masses and radii, and observations show that planets larger than approximately 1.6 Earth-radius (and more massive than approximately 6 Earth-masses) contain significant amounts of volatiles or H–He gas, likely acquired during formation. Such planets appear to have a diversity of compositions that is not well-explained by a single mass–radius relation as that found for denser, rocky planets.The lower limit for mass can vary widely for different planets depending on their compositions; the dividing mass can vary from as low as one to as high as 20 ME. Smaller gas planets and planets closer to their star will lose atmospheric mass more quickly via hydrodynamic escape than larger planets and planets farther out. A low-mass gas planet can still have a radius resembling that of a gas giant if it has the right temperature.Neptune-like planets are considerably rarer than sub-Neptunes, despite being only slightly bigger. This "radius cliff" separates sub-Neptunes (radius<3 Earth radii) from Neptunes (radius>3 Earth radii). This is thought to arise because, during formation when gas is accreting, the atmospheres of planets of that size reach the pressures required to force the hydrogen into the magma ocean, stalling radius growth. Then, once the magma ocean saturates, radius growth can continue. However, planets that have enough gas to reach saturation are much rarer, because they require much more gas.The smallest known extrasolar planet that might be a gas dwarf is Kepler-138d, which is less massive than Earth but has a 60% larger volume and therefore has a density 2.1 g/cm3) that indicates either a substantial water content or possibly a thick gas envelope. However, more recent evidence suggests that it may be more dense than previously thought, and could be an ocean planet instead.Image created by Pablo Carlos Budassi in 2023 (pablocarlosbudassi.com)
Usage terms	Please attribute the author when reusing this image. If possible, please link to: https://pablocarlosbudassi.com
Date and time of data generation	26 March 2021
Width	1,080 px
Height	1,080 px
Bits per component	8 8 8
Pixel composition	RGB
Orientation	Normal
Number of components	3
Horizontal resolution	72 dpi
Vertical resolution	72 dpi
Software used	Adobe Photoshop CS6 (Macintosh)
File change date and time	09:50, 12 August 2023
Exif version	2.21
Color space	sRGB
Date metadata was last modified	06:50, 12 August 2023
Date and time of digitizing	09:09, 30 May 2008
Unique ID of original document	xmp.did:0080117407206811B65FEE6CD4839DCA
Type of item	13000000 science and technology
Keywords	mini-Neptune mini Neptune gas dwarf transitional planet world planet world exoplanet atmosphere mass radius Earth sub-Neptune Neptune-like ocean hydrogen helium dense gas ice giant planetary science space astronomy astrobiology astrochemistry cosmology celestial body astronomical object class type sphere Kepler-138d
Contact information	pablocarlosbudassi@gmail.com www.pablocarlosbudassi.com https://www.pablocarlosbudassi.com/2021/02/planet-types.html Provincia del Chaco 2925 P.A. Mendoza, Mendoza, M5502 Argentina +54(261)5320315

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