Astronomy:Jupiter analogue
Jupiter analogues, also known as Jupiter-like planets, are exoplanets that are similar to the planet Jupiter, the fifth and largest planet in the Solar System. They are often defined as planets that has at least 1 Jupiter mass or larger and orbits its host star at a distance 3 to 12 astronomical units (AU), roughly one to a few times that of the systems snow line. The lower limit of mass for Jupiter-like planets is not well defined as it can be as low of 0.8-0.3 Jupiter masses to include planets like Saturn.[1]
Formation and evolution
While the exact formation of Jupiter-like exoplanets are not known,[2] models of gas giant planet formation predict that Jupiter-like planets should easily form around stars similar to the Sun through core-accretion mechanisms. This therefore should make planets similar to Jupiter a common occurrence in the universe with roughly 6-20% of Sun-like stars having Jupiter-like planets. But this number varies from low rates like 6.9% to higher rates like 25%.[1][clarification needed] It has been found that Jupiter analogues are very rare in mid to late type M-dwarf stars with 0.1-0.3 solar masses.[3] There has been some detections of Jupiter-like planets around red dwarf stars such as TOI-4860b with 0.67 Jupiter masses.[4]
The time it takes for form Jupiter-like planets is typically 3-5 million years but some estimates place the formation of Jupiter-like exoplanets to around 1-2 million years.[5]
Effect on their systems
Jupiter has played a major role in the evolution of the Solar System, determining much of its structure and the configuration of Solar System bodies. It is likely that Jupiter-like exoplanets play a similar role in their systems.[2]
Examples
The nearby exoplanet Epsilon Eridani b, 10.5 light-years away, has been described as "a remarkably close analog to our own planet Jupiter" and "one of the closest analogs to a Solar System planet yet detected around a nearby star".[6] Kepler-167e is a exoplanet orbiting the K-type main sequence star Kepler-167. Its mass and radius is very similar to Jupiter with about 1 Jupiter mass and 0.9 Jupiter radii.[7] Around the young F-type main sequence star 51 Eridani, there is a Jupiter-like planet named 51 Eridani b. This exoplanet has been directly imaged.[8]
References
- ↑ 1.0 1.1 Gratton, Raffaele; Mesa, Dino; Bonavita, Mariangela; Zurlo, Alice; Marino, Sebastian; Kervella, Pierre; Desidera, Silvano; D’Orazi, Valentina et al. (2023-10-17). "Jupiter-like planets might be common in a low-density environment" (in en). Nature Communications 14 (1): 6232. doi:10.1038/s41467-023-41665-0. ISSN 2041-1723. PMID 37848416. Bibcode: 2023NatCo..14.6232G.
- ↑ 2.0 2.1 Buchhave, Lars A.; Bitsch, Bertram; Johansen, Anders; Latham, David W.; Bizzarro, Martin; Bieryla, Allyson; Kipping, David M. (March 2018). "Jupiter Analogs Orbit Stars with an Average Metallicity Close to That of the Sun" (in en). The Astrophysical Journal 856 (1): 37. doi:10.3847/1538-4357/aaafca. ISSN 0004-637X. Bibcode: 2018ApJ...856...37B.
- ↑ Cowing, Keith (2023-06-14). "Mid-to-Late M Dwarfs Lack Jupiter Analogs" (in en-US). https://astrobiology.com/2023/06/mid-to-late-m-dwarfs-lack-jupiter-analogs.html.
- ↑ Triaud, Amaury H M J; Dransfield, Georgina; Kagetani, Taiki; Timmermans, Mathilde; Narita, Norio; Barkaoui, Khalid; Hirano, Teruyuki; Rackham, Benjamin V et al. (2023-10-11). "An M dwarf accompanied by a close-in giant orbiter with SPECULOOS". Monthly Notices of the Royal Astronomical Society: Letters 525 (1): L98–L104. doi:10.1093/mnrasl/slad097. ISSN 1745-3925. https://academic.oup.com/mnrasl/article/525/1/L98/7235807?login=false.
- ↑ Malewar, Amit (2025-03-06). "Gas giant exoplanets formed earlier than previously thought" (in en-US). https://www.techexplorist.com/gas-giant-exoplanets-formed-earlier-previously-thought/97577/.
- ↑ Thompson, William; Nielsen, Eric; Ruffio, Jean-Baptiste; Blunt, Sarah; Marois, Christian (2025-02-27). "Revised Mass and Orbit of $\varepsilon$ Eridani b: A 1 Jupiter-Mass Planet on a Near-Circular Orbit". The Astronomical Journal.
- ↑ Changeat, Quentin; Ikoma, Masahiro; Bocchieri, Andrea; Cassese, Ben; Edwards, Billy; Girard, Julien; Ito, Yuichi; Kimura, Tadahiro et al. (February 2024). "Contextualizing our solar-system: Atmospheric characterization of the Jupiter-analogue Kepler-167e" (in en). JWST Proposal. Cycle 3: 5531. Bibcode: 2024jwst.prop.5531C. https://ui.adsabs.harvard.edu/abs/2024jwst.prop.5531C/abstract.
- ↑ Macintosh, B.; Graham, J. R.; Barman, T.; De Rosa, R. J.; Konopacky, Q.; Marley, M. S.; Marois, C.; Nielsen, E. L. et al. (2015-10-02). "Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager". Science 350 (6256): 64–67. doi:10.1126/science.aac5891. PMID 26272904. Bibcode: 2015Sci...350...64M. https://www.science.org/doi/full/10.1126/science.aac5891.
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