HIP 41378 f
| Discovery | |
|---|---|
| Discovery date | June 2016 |
| Transit | |
| Orbital characteristics | |
| 1.37±0.02 au | |
| 542.07975±0.00014 | |
| Star | HIP 41378[1] |
| Physical characteristics | |
| 9.2 ± 0.1 R🜨 | |
| Mass | 12 ± 3 ME |
Mean density | 0.09 ± 0.02 g cm−3 |
| Temperature | Teq: 294 K (21 °C; 70 °F) |
HIP 41378 f (also known as EPIC 211311380 f) is an exoplanet orbiting around the F-type star HIP 41378. It is the outermost planet of its system and notable for the possibility that the planet may host circumplanetary debris rings[2]. It has an anomalously large radius (9.2 R🜨) for a planet of its size and temperature. This radius, combined with its measured mass of (12 ME[3]), suggest that its core is a maximum of 3 ME and subsequently the planet has an envelope fraction of 75% or greater[4]. This envelope fraction is larger than would be possible in the core accretion model of planet formation for a planet with its core mass, which is consistent with the hypothesis that the planet's radius may be observed to be larger than it actually is due to an optically thick ring system[2][5]. One proposed origin for such a ring system is an exomoon, which migrated and disintegrated in the past[6]. It is located within the optimistic habitable zone of its parent star.[3] No atmospheric signatures were found as in 2022, further reinforcing the hypothesis of opaque circumplanetary rings.[7]
See also
[edit]- Lists of exoplanets
- GJ 1132 b, rocky exoplanet with a confirmed atmosphere.
- Mu Arae c, in the constellation Ara
- Planetary system
References
[edit]- ^ "HIP 41378 f CONFIRMED PLANET OVERVIEW PAGE". NASA Exoplanet Archive. Retrieved 2016-07-08.
- ^ a b Akinsanmi, B.; Santos, N. C.; Faria, J. P.; Oshagh, M.; Barros, S. C. C.; Santerne, A.; Charnoz, S. (2020-03-01). "Can planetary rings explain the extremely low density of HIP 41378 𝑓?". Astronomy & Astrophysics. 635: L8. arXiv:2002.11422. doi:10.1051/0004-6361/202037618. ISSN 0004-6361.
- ^ a b Santerne, A.; Malavolta, L.; Kosiarek, M. R.; Dai, F.; Dressing, C. D.; Dumusque, X.; Hara, N. C.; Lopez, T. A.; Mortier, A.; Vanderburg, A.; Adibekyan, V.; Armstrong, D. J.; Barrado, D.; Barros, S. C. C.; Bayliss, D.; Berardo, D.; Boisse, I.; Bonomo, A. S.; Bouchy, F.; Brown, D. J. A.; Buchhave, L. A.; Butler, R. P.; Collier Cameron, A.; Cosentino, R.; Crane, J. D.; Crossfield, I. J. M.; Damasso, M.; Deleuil, M. R.; Delgado Mena, E.; et al. (2019). "An extremely low-density and temperate giant exoplanet". arXiv:1911.07355 [astro-ph.EP].
- ^ Belkovski, M.; Becker, J.; Howe, A.; Malsky, I.; Batygin, K. (2022). "A Multiplanet System's Sole Super-puff: Exploring Allowable Physical Parameters for the Cold Super-puff HIP 41378 f". The Astronomical Journal. 163 (6): 277. arXiv:2203.17180. Bibcode:2022AJ....163..277B. doi:10.3847/1538-3881/ac6353.
- ^ Piro, A. L.; Vissapragada, S. (2020). "Exploring Whether Super-puffs can be Explained as Ringed Exoplanets". The Astronomical Journal. 159 (4): 131. arXiv:1911.09673. Bibcode:2020AJ....159..131P. doi:10.3847/1538-3881/ab7192.
- ^ Saillenfest, M.; Sulis, S.; Charpentier, P.; Santerne, A. (2023). "Oblique rings from migrating exomoons: A possible origin for long-period exoplanets with enlarged radii". Astronomy and Astrophysics. 675. doi:10.1051/0004-6361/20234674 (inactive 2024-08-13).
((cite journal)): CS1 maint: DOI inactive as of August 2024 (link) - ^ Alam, Munazza K.; Kirk, James; Dressing, Courtney D.; López-Morales, Mercedes; Ohno, Kazumasa; Gao, Peter; Akinsanmi, Babatunde; Santerne, Alexandre; Grouffal, Salomé; Adibekyan, Vardan; Barros, Susana C. C.; Buchhave, Lars A.; Crossfield, Ian J. M.; Dai, Fei; Deleuil, Magali; Giacalone, Steven; Lillo-Box, Jorge; Marley, Mark; Mayo, Andrew W.; Mortier, Annelies; Santos, Nuno C.; Sousa, Sérgio G.; Turtelboom, Emma V.; Wheatley, Peter J.; Vanderburg, Andrew M. (2022), "The First Near-infrared Transmission Spectrum of HIP 41378 f, A Low-mass Temperate Jovian World in a Multiplanet System", The Astrophysical Journal Letters, 927 (1): L5, arXiv:2201.02686, Bibcode:2022ApJ...927L...5A, doi:10.3847/2041-8213/ac559d, S2CID 245837282
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