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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.
Transiting Exoplanet Survey Satellite is a space telescope for NASA's Explorer program, designed to search for exoplanets using the transit method in an area 400 times larger than that covered by the Kepler mission. It was launched on 18 April 2018, atop a Falcon 9 launch vehicle and was placed into a highly elliptical 13.70-day orbit around the Earth. The first light image from TESS was taken on 7 August 2018, and released publicly on 17 September 2018.
A hot Neptune or Hoptune is a type of giant planet with a mass similar to that of Uranus or Neptune orbiting close to its star, normally within less than 1 AU. The first hot Neptune to be discovered with certainty was Gliese 436 b 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.
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.
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V1298 Tauri is a young weakly-lined T Tauri star that is part of the Taurus-Auriga association in the Taurus Molecular Cloud. Alternatively it is part of a proposed moving group, called Group 29 that is slightly older. The system has four transiting exoplanets, discovered with the Kepler space telescope in the K2 mission. One of the planets was discovered in August 2019 and the other three were discovered in November 2019 by the same team.
WD 1856+534 is a white dwarf located in the constellation of Draco. At a distance of about 25 parsecs (80 ly) from Earth, it is the outer component of a visual triple star system consisting of an inner pair of red dwarf stars. The white dwarf displays a featureless absorption spectrum, lacking strong optical absorption or emission features in its atmosphere. It has an effective temperature of 4,700 K, corresponding to an age of approximately 5.8 billion years. WD 1856+534 is approximately half as massive as the Sun, while its radius is much smaller, being 40% larger than Earth.
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 September 2022 the collaboration produced 7 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 Myrs old and currently 9.5 REarth large. It will become a 3-5 REarth planet in about 1 billion years, because the planet is still contracting. TOI-1227 b orbits a very low-mass star every 27.36 days.
References
- 1 2 3 4 5 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.
- ↑ "HIP 67522". Open Exoplanet Catalogue. Retrieved January 25, 2022.
- 1 2 3 4 5 "Planet HIP 67522 b". exoplanet.eu. Retrieved January 23, 2022.
- 1 2 3 4 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.
- 1 2 "HIP 67522 b". exoplanets.nasa.gov. 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. arXiv: 1305.0269 . Bibcode:2013ApJ...776....2L. doi:10.1088/0004-637X/776/1/2. S2CID 118545757.
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