Super-Neptune

Short description: Planet larger than Neptune but smaller than Saturn

Artist's interpretation of a super-Neptune.

A super-Neptune is a planet that is more massive than the planet Neptune. These planets are generally described as being around 5–7 times as large as Earth with estimated masses of 20–80 M⊕;[1] beyond this they are generally referred to as gas giants. A planet falling within this mass range may also be referred to as a sub-Saturn.[2]

There have been relatively few discoveries of planets of this kind. The mass gap between Neptune-like and Jupiter-like planets is thought to exist because of "runaway accretion" occurring for protoplanets of more than 20 M⊕—once this mass threshold is crossed, they accumulate much additional mass (due to gravity increasing with mass and the presence of material in an accretion disk) and grow into planets the size of Jupiter or even larger.[2]

Known examples include Kepler-101b, HAT-P-11b, and K2-33b.[3][4]

## Mass-radius relationship

Through modelling, and analysis of discovered exoplanets, the relationship between mass and radius has given a much higher upper limit for the transition boundary between Neptune and Jupiter worlds than had been previously defined empirically from observing the planets within our solar system, for example Chen & Kipping (2017) defined the transition point between Neptunian and Jovian worlds at around 130 M⊕.[5] In studies looking into this relationship between mass-radius, Saturn, though never defined as an ice giant, is however found to sit just within the mass-radius limits for a Neptunian world, close to the transition point between super-Neptune and Jupiter world.[6]

## See also

* Super-Earth

## References

1. ↑ "Super-Neptune Planet Found". 14 March 2009. http://www.space.com/6338-super-neptune-planet.html.
2. ↑ 2.0 2.1 "'Sub-Saturns' May Force Scientists to Revise Idea of How Planets Form". 12 January 2019. https://www.space.com/42958-sub-saturn-exoplanets-are-common-after-all.html.
3. ↑ Bonomo, A. S.Expression error: Unrecognized word "etal". (2014). "Characterization of the planetary system Kepler-101 with HARPS-N". Astronomy & Astrophysics 572: A2. doi:10.1051/0004-6361/201424617. Bibcode: 2014A&A...572A...2B.
4. ↑ "Young super-Neptune offers clues to the origin of close-in exoplanet". http://phys.org/news/2016-06-young-super-neptune-clues-close-in-exoplanet.html.
5. ↑ Chen, Jingjing; Kipping, David (2017). "Probabilistic Forecasting of the Masses and Radii of Other Worlds". The Astrophysical Journal (American Astronomical Society) 834 (1): 17. doi:10.3847/1538-4357/834/1/17. ISSN 1538-4357. Bibcode: 2017ApJ...834...17C.
6. ↑ Edmondson, Kathryn; Norris, Jordan; Kerins, Eamonn (2023). "Breaking up with the continuous exoplanet mass-radius relation". arXiv:2310.16733 [astro-ph.EP].

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Exoplanetology

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Main topics|

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Sizes
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|

Gaseous|

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Other types|

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