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Sagittarius A*, abbreviated as Sgr A*, is the supermassive black hole at the Galactic Center of the Milky Way. Viewed from Earth, it is located near the border of the constellations Sagittarius and Scorpius, about 5.6° south of the ecliptic, visually close to the Butterfly Cluster (M6) and Lambda Scorpii.
MS 0735.6+7421 is a galaxy cluster located in the constellation Camelopardalis, approximately 2.6 billion light-years away. It is notable as the location of one of the largest central galactic black holes in the known universe, which has also apparently produced one of the most powerful active galactic nucleus eruptions discovered.
An extragalactic planet, also known as an extragalactic exoplanet or an extroplanet, is a star-bound planet or rogue planet located outside of the Milky Way Galaxy. Due to the immense distances to such worlds, they would be very hard to detect directly. However, indirect evidences suggest that such planets exist. Nonetheless, the most distant confirmed planets are SWEEPS-11 and SWEEPS-04, located in Sagittarius, approximately 27,710 light-years from the Sun, while the Milky Way is about 87,400 light-years in diameter. This means that even galactic planets located further than that distance have not been detected.
NGC 4845 is a spiral galaxy located in the constellation Virgo around 65 million light years away. The galaxy was originally discovered by William Herschel in 1786. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster.
In astronomy, a disrupted planet is a planet or exoplanet or, perhaps on a somewhat smaller scale, a planetary-mass object, planetesimal, moon, exomoon or asteroid that has been disrupted or destroyed by a nearby or passing astronomical body or object such as a star. Necroplanetology is the related study of such a process.
NGC 4660 is an elliptical galaxy located about 63 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.
NGC 1271 is a compact elliptical or lenticular galaxy located about 250 million light-years away in the constellation Perseus. The galaxy was discovered by astronomer Guillaume Bigourdan on November 14, 1884. NGC 1271 is a member of the Perseus Cluster and has a nuclear dust disk in its center. It also has an edge-on, intermediate-scale disk and has a central bulge. Like NGC 1277, NGC 1271 is a candidate "relic galaxy".
The small planet radius gap is an observed scarcity of planets with radii between 1.5 and 2 times Earth's radius, likely due to photoevaporation-driven mass loss. A bimodality in the Kepler exoplanet population was first observed in 2011 and attributed to the absence of significant gas atmospheres on close-in, low-mass planets. This feature was noted as possibly confirming an emerging hypothesis that photoevaporation could drive atmospheric mass loss This would lead to a population of bare, rocky cores with smaller radii at small separations from their parent stars, and planets with thick hydrogen- and helium-dominated envelopes with larger radii at larger separations. The bimodality in the distribution was confirmed with higher-precision data in the California-Kepler Survey in 2017, which was shown to match the predictions of the photoevaporative mass-loss hypothesis later that year.
S62 is a star in the cluster surrounding Sagittarius A* (Sgr A*), the supermassive black hole in the center of the Milky Way. S62 was initially thought to orbit extremely close to Sgr A*, with a period of 9.9 years and a closest approach of only 16 astronomical units (2.4×109 km), less than the distance between Uranus and the Sun. This would have put it at just 215 times the Schwarzschild radius of Sgr A* (the Schwarzschild radius of Sgr A* is approximately 0.082 AU, or 12 million km).
Tau Ceti f is a potential super-Earth or mini-Neptune orbiting Tau Ceti that was discovered in 2012 by statistical analyses of the star's variations in radial velocity, based on data obtained using HIRES, AAPS, and HARPS. It is of interest because its orbit places it in Tau Ceti's extended habitable zone, but a 2015 study implies that there may not be a detectable biosignature because it has only been in the temperate zone for less than one billion years. In 2017, it was again recovered from radial-velocity data, along with Tau Ceti e. Despite this, it remains an unconfirmed candidate.
WASP-69, also named Wouri, is a K-type main-sequence star 164 light-years away from Earth. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.
Kepler-167 is a K-type main-sequence star located about 1,119 light-years (343 pc) away from the Solar System in the constellation of Cygnus. The star has about 78% the mass and 75% the radius of the Sun, and a temperature of 4,884 K. It hosts a system of four known exoplanets. There is also a companion red dwarf star at a separation of about 700 AU, with an estimated orbital period of over 15,000 years.
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.
Little red dots (LRDs) are a class of small, red-tinted galaxies discovered by the James Webb Space Telescope. Their discovery was published in March 2024, and they are currently poorly understood. They appear to have existed between 0.6 and 1.6 billion years after the Big Bang, from 13.2 to 12.2 billion years ago.
References
- ↑ Letzter, R. (6 August 2020). "Thousands of Earthlike 'blanets' might circle the Milky Way's central black hole". Space.com. Retrieved 2020-08-08.
- ↑ Wada, K.; Tsukamoto, Y.; Kokubo, E. (26 November 2019). "Planet Formation around Supermassive Black Holes in the Active Galactic Nuclei". The Astrophysical Journal. 886 (2): 107. arXiv: 1909.06748 . Bibcode:2019ApJ...886..107W. doi: 10.3847/1538-4357/ab4cf0 .
- 1 2 Wada, K.; Tsukamoto, Y.; Kokubo, E. (2021). "Formation of "Blanets" from Dust Grains around the Supermassive Black Holes in Galaxies". The Astrophysical Journal. 909 (1): 96. arXiv: 2007.15198 . Bibcode:2021ApJ...909...96W. doi: 10.3847/1538-4357/abd40a . S2CID 220870610.
- ↑ Starr, M. (3 August 2020). "We Have Ploonets. We Have Moonmoons. Now Hold Onto Your Hats For... Blanets". ScienceAlert. Retrieved 2020-08-08.
- ↑ Greene, T. (2020-08-04). "Scientists: What if black holes had a safe zone where little planets could live? Let's call them 'blanets'". The Next Web. Retrieved 2020-08-08.
- ↑ "Chandra Sees Evidence for Possible Planet in Another Galaxy - NASA" . Retrieved 2024-08-07.
- ↑ Martin, Pierre-Yves (2016). "Planet IGR J12580+0134 b". exoplanet.eu. Retrieved 2024-11-03.
- ↑ Lei, Wei-Hua; Yuan, Qiang; Zhang, Bing; Wang, Daniel (2016-01-01). "Igr J12580+0134: The First Tidal Disruption Event with an Off-Beam Relativistic Jet". The Astrophysical Journal. 816 (1): 20. arXiv: 1511.01206 . doi: 10.3847/0004-637X/816/1/20 . ISSN 0004-637X.
