Astronomy:HIP 67522 b
Coordinates: 
13h 50m 06.28s, −40° 50′ 08.89″
| Discovery[1] | |
|---|---|
| Discovered by | THYME (Rizzuto et al.) |
| Discovery date | 2020 |
| Primary Transit | |
| Designations | |
| HD 120411 b, Gaia DR2 6113920619134019456 b, TYC 7794-2268-1 b[2] | |
| Orbital characteristics | |
| Eccentricity | 0.059+0.193 −0.046[3] |
| Orbital period | 6.959503±0.000016 d[3] |
| Inclination | 89.34°+0.45° −0.54° (to plane of sky)[1] 5.8+2.8 −5.7 ° (to host star's equator, projected)[4] |
| 343.0+92.0 −140.0 °[3] | |
| Star | HIP 67522 |
| Physical characteristics | |
| Mean radius | 0.8984±0.0419 |♃|J}}}}}}[3] |
| Mass | <5 |♃|J}}}}}}[4] |
| Mean density | 0.455+0.052 −0.049 times that of the Sun[1] |
| Physics | 1174±21 K[3] |
HIP 67522 b is a hot Jupiter exoplanet orbiting the G-type star[5] HIP 67522, located approximately 415 light-years from Earth[5] in the constellation Centaurus, discovered using the Transiting Exoplanet Survey Satellite (TESS). It is currently the youngest hot Jupiter discovered, at an age of only 17 million years;[1] it is also one of the youngest transiting planets of any type, and one of only four others less than 100 million years old (along with AU Mic b, V1298 Tau c, DS Tuc Ab and TOI-942 b) to have the angle between its orbit and its host star's rotation measured, at 5.8+2.8
−5.7 degrees.[4] This planet, in turn, may help in knowing how other hot Jupiters form.
Due to its young age, it has not reached its final size, due to the Kelvin–Helmholtz mechanism,[4] which occurs as a result of the planet itself cooling, causing its internal pressure to drop, which will in turn cause the planet to shrink. Its final size will depend on the composition of its core.[6]
There is also evidence that another planet might also be present in the planetary system.[1]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Rizzuto, A. C.; Newton, E. R.; Mann, A. W.; Tofflemire, B. M.; Vanderburg, A.; Kraus, A. L.; Wood, M. L.; Quinn, S. N. et al. (June 22, 2020). "TESS Hunt for Young and Maturing Exoplanets (THYME). II. A 17 Myr Old Transiting Hot Jupiter in the Sco-Cen Association". The Astronomical Journal 160 (1): 33. doi:10.3847/1538-3881/ab94b7. Bibcode: 2020AJ....160...33R.
- ↑ "HIP 67522". Open Exoplanet Catalogue. http://www.openexoplanetcatalogue.com/planet/HIP%2067522%20b/. Retrieved January 25, 2022.
- ↑ 3.0 3.1 3.2 3.3 3.4 "Planet HIP 67522 b". Extrasolar Planets Encyclopaedia. 1995. https://exoplanet.eu/catalog/hip_67522_b--7401/.
- ↑ 4.0 4.1 4.2 4.3 Heitzmann, A.; Zhou, G.; Quinn, S. N.; Marsden, S. C.; Wright, D.; Petit, P.; Vanderburg, A. M.; Bouma, L. G. et al. (November 12, 2021). "The Obliquity of HIP 67522 b: A 17 Myr Old Transiting Hot, Jupiter-sized Planet". The Astrophysical Journal Letters 922 (1): L1. doi:10.3847/2041-8213/ac3485. Bibcode: 2021ApJ...922L...1H.
- ↑ 5.0 5.1 "HIP 67522 b". exoplanets.nasa.gov. https://exoplanets.nasa.gov/exoplanet-catalog/7659/hip-67522-b/. Retrieved January 23, 2022.
- ↑ Lopez, E. D.; Fortney, J. J. (September 17, 2013). "The Role of Core Mass in Controlling Evaporation: The Kepler Radius Distribution and the Kepler-36 Density Dichotomy". The Astrophysical Journal 776 (1): 2. doi:10.1088/0004-637X/776/1/2. Bibcode: 2013ApJ...776....2L. https://iopscience.iop.org/article/10.1088/0004-637X/776/1/2/meta.
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