HIP 67522 b

Last updated • 1 min readFrom Wikipedia, The Free Encyclopedia
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
0.8984±0.0419 RJ [3]
Mass <20 ME [5]
Mean density
<0.10  g/cm3 [5]
Temperature 1174±21 K [3]

    HIP 67522 b is a hot Jupiter exoplanet orbiting the G-type star [6] HIP 67522, located approximately 415 light-years from Earth [6] 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. 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. [7]

    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 rocky and icy materials usually takes place. [5]

    Related Research Articles

    <span class="mw-page-title-main">Scorpius–Centaurus association</span> The nearest OB association to Earth

    The Scorpius–Centaurus association is the nearest OB association to the Sun. This stellar association is composed of three subgroups and its distance is about 130 parsecs or 420 light-years. Analysis using improved Hipparcos data has brought the number of known members to 436. The cluster shows a continuous spread of stars with no apparent need for subclassification.

    The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

    <span class="mw-page-title-main">Hot Neptune</span> Planet with a mass similar to Uranus or Neptune orbiting close to its star

    A hot Neptune is a type of giant planet with a mass similar to that of Neptune or Uranus orbiting close to its star, normally within less than 1 AU. The first hot Neptune to be discovered with certainty was Gliese 436 b (Awohali) in 2007, an exoplanet about 33 light years away. Recent observations have revealed a larger potential population of hot Neptunes in the Milky Way than was previously thought. Hot Neptunes may have formed either in situ or ex situ.

    <span class="mw-page-title-main">Planet Hunters</span> Citizen science project to find exoplanets

    Planet Hunters is a citizen science project to find exoplanets using human eyes. It does this by having users analyze data from the NASA Kepler space telescope and the NASA Transiting Exoplanet Survey Satellite. It was launched by a team led by Debra Fischer at Yale University, as part of the Zooniverse project.

    <span class="mw-page-title-main">HATS-36b</span> Extrasolar planet in the constellation Sagittarius

    HATS-36b is a gas giant exoplanet that orbits an F-type star. Its mass is 3.216 Jupiters, it takes 4.2 days to complete one orbit of its star, and is 0.05425 AU from it. It was discovered on June 12, 2017 and was announced in 2018. Its discoverers were 23, namely Daniel Bayliss, Joel Hartman, George Zhou, Gaspar Á. Bakos, Andrew Vanderburg, J. Bento, L. Mancini, S. Ciceri, Rafael Brahm, Andres Jordán, N. Espinoza, M. Rabus, T. G. Tan, K. Penev, W. Bhatti, M. de Val-Borro, V. Suc, Z. Csubry, Th. Henning, P. Sarkis, J. Lázár, I. Papp, P. Sári.

    <span class="mw-page-title-main">TOI-700 d</span> Goldilocks terrestrial planet orbiting TOI-700

    TOI-700 d is a near-Earth-sized exoplanet, likely rocky, orbiting within the habitable zone of the red dwarf TOI-700, the outermost planet within the system. It is located roughly 101.4 light-years (31.1 pc) away from Earth in the constellation of Dorado. The exoplanet is the first Earth-sized exoplanet in the habitable zone discovered by the Transiting Exoplanet Survey Satellite (TESS).

    TESS Hunt for Young and Maturing Exoplanets (THYME) is an exoplanet search project. The researchers of the THYME collaboration are mainly from the United States and search for young exoplanets using data from the Transiting Exoplanet Survey Satellite (TESS). The new discoveries should help to understand the early evolution of exoplanets. As of March 2023 the collaboration produced 9 papers announcing the discovery of exoplanets.

    TOI-1227 b is one of the youngest transiting exoplanets discovered, alongside K2-33b and HIP 67522 b. The exoplanet TOI-1227 b is about 11±2 million years old and currently 9.6 R🜨 large. It will become a 3-5 R🜨 planet in about 1 billion years, because the planet is still contracting. TOI-1227 b orbits its host star every 27.36 days.

    <span class="mw-page-title-main">HD 63433 d</span> Exoplanet orbiting G-type star HD 63433

    HD 63433 d is a confirmed exoplanet orbiting HD 63433, a Sun-like star located 73 light-years away in the constellation Gemini. Its radius is measured at around 1.1 R🜨, which makes it similar to the Earth in size. It was the third exoplanet to be discovered in orbit around this star; the other two, HD 63433 b and c, were discovered in 2020. Orbiting its star at a distance of 0.0503 astronomical units (7,520,000 km), HD 63433 d is the innermost planet orbiting HD 63433, and completes an orbit around it just every 4 days. Due to the proximity of its star, the planet is scorching hot, having a temperature estimated at 1260 °C at daytime. The proximity of its star also causes it to be tidally locked.

    References

    1. 1 2 3 4 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 "HIP 67522 b". exoplanets.nasa.gov. Retrieved January 23, 2022.
    7. 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.