HIP 67522 b

Last updated
HIP 67522 b
Discovery [1]
Discovered by THYME (Rizzuto et al.)
Discovery date2020
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]
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
0.897±0.051 RJ [3]
Mass 13.8 ± 1.0, <20 M🜨 [5] [6]
Mean density
<0.10  g/cm3 [5] [6]
Temperature 1174±21 K [3]

    HIP 67522 b is a hot Neptune or sub-Saturn exoplanet orbiting the G-type star [7] HIP 67522, approximately 415 light-years from Earth [7] in the constellation Centaurus. [6] It was discovered using the Transiting Exoplanet Survey Satellite (TESS). It is 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 understanding how other hot Neptunes form.

    Due to its young age, it has not reached its final size. Also due to the Kelvin–Helmholtz mechanism, [4] which occurs as a result of the planet itself cooling, its internal pressure drops, which will in turn cause the planet to shrink. Its final size will depend on the composition of its core. [8]

    There is also evidence that another planet might also be present in the planetary system. [1]

    It was shown in 2024 that HIP 67522 b is one of the least dense known planets, with a density less than 0.10 g/cm3. It might have formed beyond the water-snowline, where the contamination by both rocky and icy materials frequently takes place. [5] [6] In 2025, it was revealed with certainty that HIP 67522 b triggers the increase in flare from the host star via the star-planet magnetic interactions. These flares might have caused the shrinkage of the planet's atmosphere. [9]

    References

    1. 1 2 3 Rizzuto, A. C.; Newton, E. R.; Mann, A. W.; Tofflemire, B. M.; Vanderburg, A.; Kraus, A. L.; Wood, M. L.; Quinn, S. N.; Zhou, G.; Thao, P. C.; Law, N. M.; Ziegler, C.; Briceño, César (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. arXiv: 2005.00013 . Bibcode:2020AJ....160...33R. doi: 10.3847/1538-3881/ab94b7 . S2CID   218470215.
    2. ↑ "HIP 67522". Open Exoplanet Catalogue. Retrieved January 25, 2022.
    3. 1 2 3 4 5 "Planet HIP 67522 b". Extrasolar Planets Encyclopaedia . 1995. Retrieved January 23, 2022.
    4. 1 2 3 Heitzmann, A.; Zhou, G.; Quinn, S. N.; Marsden, S. C.; Wright, D.; Petit, P.; Vanderburg, A. M.; Bouma, L. G.; Mann, A. W.; Rizzuto, A. C. (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. arXiv: 2109.04174 . Bibcode:2021ApJ...922L...1H. doi: 10.3847/2041-8213/ac3485 . S2CID   237452642.
    5. 1 2 3 Cowing, Keith (8 October 2024). "The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST". Astrobiology. Retrieved 11 October 2024.
    6. 1 2 3 4 Thao, Pa Chia; Mann, Andrew W.; Feinstein, Adina D.; Gao, Peter; Thorngren, Daniel; Rotman, Yoav; Welbanks, Luis; Brown, Alexander; Duvvuri, Girish M.; France, Kevin; Longo, Isabella; Sandoval, Angeli; Schneider, P. Christian; Wilson, David J.; Youngblood, Allison (2024-12-01). "The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST". The Astronomical Journal. 168 (6): 297. arXiv: 2409.16355 . Bibcode:2024AJ....168..297T. doi: 10.3847/1538-3881/ad81d7 . ISSN   0004-6256.
    7. 1 2 "HIP 67522 b". exoplanets.nasa.gov. 24 July 2020. Retrieved January 23, 2022.
    8. ↑ 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. arXiv: 1305.0269 . Bibcode:2013ApJ...776....2L. doi:10.1088/0004-637X/776/1/2. S2CID   118545757.
    9. ↑ Ilin, Ekaterina; Vedantham, Harish K.; Poppenhäger, Katja; Bloot, Sanne; Callingham, Joseph R.; Brandeker, Alexis; Chakraborty, Hritam (2025-07-02). "Close-in planet induces flares on its host star" . Nature: 1–4. doi:10.1038/s41586-025-09236-z. ISSN   1476-4687. PMID   40604272.


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