YBP 1194

Last updated
YBP 1194
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Cancer
Right ascension 08h 51m 00.80527s [1]
Declination +11° 48′ 52.7956″ [1]
Apparent magnitude  (V)14.676 [2]
Characteristics
Spectral type G5V [3]
B−V color index 0.626 [3]
Astrometry
Radial velocity (Rv)+36.5 ± 0.9 [4]  km/s
Proper motion (μ)RA: -10.813  mas/yr [1]
Dec.: -2.732  mas/yr [1]
Parallax (π)1.1297 ± 0.0242  mas [1]
Distance 2,890 ± 60  ly
(890 ± 20  pc)
Details [3]
Mass 1.01±0.02  M☉
Radius 0.99±0.02  R☉
Surface gravity (log g)4.44±0.035  cgs
Temperature 5780±27  K
Metallicity [Fe/H]0.023±0.015  dex
Age 4.15±0.65 [5]   Gyr
Other designations
NGC 2682 YBP 1194, ES 4063, ES IV-63, FBC 2867, MMJ 5357, SAND 770, EPIC  211411531, TIC  437034946, 2MASS J08510080+1148527 [6]
Database references
SIMBAD data

YBP 1194 is a G-type main-sequence star, class G5V, in the open cluster Messier 67, about 2,890 light-years (890 parsecs ) from the Sun in the constellation Cancer. [6] [7] It is a solar twin, having the near exact same temperature and mass as the Sun. [8] YBP 1194 has a slightly higher metallicity than the Sun, and may be slightly younger at an age of 3.5-4.8 billion years. [3] In January 2014, this star was announced to have an exoplanet. [7] [3]

This system is packed in a small cluster, Messier 67, with a radius of 10 light-years, with over 500 other stars. [9] For comparison, the Sun has 9 star systems within 10 light-years and 94 star systems within 20 light-years. [10]

Planetary system

The exoplanet YBP 1194 b was discovered in January 2014 by researchers at the European Southern Observatory (ESO) as one of three new planets discovered in the M67 cluster, showing that open star clusters are more likely to have planets in them than previously thought. [7] [3] The exoplanet is about 100 times more massive than Earth, comparable in mass to Saturn. YBP 1194 b orbits its star with a 7-day period at a distance of 0.07 AU, closer than the planet Mercury is to the Sun. The combination of its large mass and close orbit makes this planet a hot Jupiter. The orbital eccentricity of YPB 1194 b is about 0.3, greater than Pluto's eccentricity of 0.25. [11]

The YBP 1194 planetary system [11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≥0.33±0.03  MJ 0.07166.960±0.0010.31±0.08——

Related Research Articles

<span class="mw-page-title-main">Messier 67</span> Old open cluster in the constellation Cancer

Messier 67 and sometimes called the King Cobra Cluster or the Golden Eye Cluster is an open cluster in the southern, equatorial half of Cancer. It was discovered by Johann Gottfried Koehler in 1779. Estimates of its age range between 3.2 and 5 billion years. Distance estimates are likewise varied, but typically are 800–900 parsecs (2,600–2,900 ly). Estimates of 855, 840, and 815 pc were established via binary star modelling and infrared color-magnitude diagram fitting.

HD 93083 is an orange-hued star in the southern constellation of Antlia. It has the proper name Macondo, after the mythical village of the novel One Hundred Years of Solitude. The name was selected by Colombia during the IAU's NameExoWorlds campaign. The star has an apparent visual magnitude of 8.30, which is too faint to be visible to the naked eye. It is located at a distance of 93 light years from the Sun based on parallax. HD 93083 is drifting further away with a radial velocity of +43.65 km/s, having come to within 43 light-years some 484,000 years ago.

<span class="mw-page-title-main">Solar analog</span> Star that is particularly similar to the Sun

Solar-type stars, solar analogs, and solar twins are stars that are particularly similar to the Sun. The stellar classification is a hierarchy with solar twin being most like the Sun followed by solar analog and then solar-type. Observations of these stars are important for understanding better the properties of the Sun in relation to other stars and the habitability of planets.

HD 70642 is a star with an exoplanetary companion in the southern constellation of Puppis. It has an apparent visual magnitude of +7.17, which is too dim to be readily visible to the naked eye. The system is located at a distance of 95.5 light-years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of +49.3 km/s. It came to within 55.3 ly of the Solar System some 329,000 years ago.

HD 132406 is a star in the northern constellation of Boötes. With an apparent visual magnitude of 8.45, it is invisible to the naked eye. The distance to this star is 230 light-years based on parallax, but it is drifting closer with a radial velocity of −37.8 km/s. The star has an absolute magnitude of 4.30. It has one confirmed exoplanet companion.

HD 117207 is a star in the southern constellation Centaurus. With an apparent visual magnitude of 7.24, it is too dim to be visible to the naked eye but can be seen with a small telescope. Based upon parallax measurements, it is located at a distance of 105.4 light-years from the Sun. The star is drifting closer with a radial velocity of −17.4 km/s. It has an absolute magnitude of 4.67.

HD 141937 is a star in the southern zodiac constellation of Libra, positioned a couple of degrees to the north of Lambda Librae. It is a yellow-hued star with an apparent visual magnitude of 7.25, which means it is too faint to be seen with the naked eye. This object is located at a distance of 108.9 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −2.2 km/s. It has an absolute magnitude of 4.71.

HD 190228 is a star with an orbiting substellar companion in the northern constellation of Vulpecula. Its apparent magnitude is 7.30 – too faint to be seen with the naked eye – and the absolute magnitude is 3.34. Based on parallax measurements, it is located at a distance of 205 light-years from the Sun. The system is drifting closer with a radial velocity of −50 km/s.

HD 162020 is a star in the southern constellation of Scorpius with a likely red dwarf companion. It has an apparent visual magnitude of 9.10, which is too faint to be visible to the naked eye. The distance to this system is 102 light-years based on stellar parallax. It is drifting closer to the Sun with a radial velocity of −27 km/s, and is predicted to come to within ~18 light-years in 1.1 million years.

<span class="mw-page-title-main">WASP-8</span> Star in the constellation of Sculptor

WASP-8 is a binary star system 294 light-years away. The star system is much younger than the Sun at 300 million to 1.2 billion years age, and is heavily enriched in heavy elements, having nearly twice the concentration of iron compared to the Sun.

XO-2 is a binary star system about 490 light-years away in the constellation Lynx. It consists of two components, XO-2N and XO-2S, both of which host planetary systems.

<span class="mw-page-title-main">HD 190007</span> Star in the constellation Aquila

HD 190007, also known as Gliese 775, is a star with a close orbiting exoplanet in the constellation of Aquila. Parallax measurements by Gaia put the star at a distance of 41.5 light-years away from the Sun. It is drifting closer with a radial velocity of −30.3 km/s, and is predicted to come within 11.8 light-years in 375,000 years. The star has an absolute magnitude of 6.91, but at its present distance the apparent visual magnitude is 7.46, which is too faint to be viewed with the naked eye.

Kepler-39 is an F-type main sequence star located in the constellation Cygnus. It is located about 3,500 light-years away. One known substellar companion orbits it, Kepler-39b.

Kepler-41 or KOI-196 is a star in the constellation Cygnus. It is a G-type main-sequence star, like the Sun, and it is located about 3,510 light-years away. It is fairly similar to the Sun, with 115% of its mass, a radius of 129% times that of the Sun, and a surface temperature of 5,750 K. Search for stellar companions to Kepler-41 in 2013-2014 has yielded inconclusive results, compatible with Kepler-41 being the single star.

HD 109271 is a wide binary star system in the constellation of Virgo. The brighter member of the binary has a pair of orbiting exoplanets. With an apparent visual magnitude of 8.05, it cannot be seen with the naked eye. Parallax measurements made by Gaia put the star at a distance of 181 light-years away from the Sun, but it is drifting closer with a radial velocity of −5 km/s. The system shows a high proper motion, traversing the celestial sphere at an angular rate of 0.232 arcsec yr−1.

GJ 3512 is a nearby star in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye but can be observed using a telescope, having an apparent visual magnitude of +15.05. The star is located at a distance of 31 light-years from the Sun based on parallax. It has a high proper motion, traversing the celestial sphere at the rate of 1.311″ yr−1. The measurement of the star's radial velocity is poorly constrained, but it appears to be drifting further away at a rate of ~8 km/s.

<span class="mw-page-title-main">HD 131399</span> Star in the constellation Centaurus

HD 131399 is a star system in the constellation of Centaurus. Based on the system's electromagnetic spectrum, it is located around 350 light-years away. The total apparent magnitude is 7.07, but because of interstellar dust between it and the Earth, it appears 0.22 ± 0.09 magnitudes dimmer than it should be.

HD 1690 is a giant star with an orbiting exoplanet companion in the constellation of Cetus. It has an apparent visual magnitude of 9.19, which is too faint to be visible to the naked eye. The distance to this system is approximately 2,570 light years, and it is drifting further away with a radial velocity of +18.2 km/s. HD 1690 has no known companion star, making it a single star system.

<span class="mw-page-title-main">HD 189567</span> Star in the constellation Pavo

HD 189567 is a star with a pair of orbiting exoplanets, located in the southern constellation of Pavo. It is also known as Gliese 776, CD-67 2385, and HR 7644. The star has an apparent visual magnitude of 6.07, which is bright enough for it to be dimly visible to the naked eye. It lies at a distance of 58 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −10.5 km/s.

References

  1. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. ↑ Krone-Martins, A.; Soubiran, C.; Ducourant, C.; Teixeira, R.; Le Campion, J. F. (2010). "Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue". Astronomy and Astrophysics. 516: A3. arXiv: 1006.0096 . Bibcode:2010A&A...516A...3K. doi:10.1051/0004-6361/200913881. S2CID   119252831.
  3. 1 2 3 4 5 6 Brucalassi, A.; Pasquini, L.; Saglia, R.; et al. (2014). "Three planetary companions around M 67 stars". Astronomy & Astrophysics. 561: L9. arXiv: 1401.4905 . Bibcode:2014A&A...561L...9B. doi:10.1051/0004-6361/201322584. S2CID   36895080.
  4. ↑ Lee, Young Sun; Beers, Timothy C.; Sivarani, Thirupathi; Johnson, Jennifer A.; An, Deokkeun; Wilhelm, Ronald; Allende Prieto, Carlos; Koesterke, Lars; Fiorentin, Paola Re; Bailer-Jones, Coryn A. L.; Norris, John E.; Yanny, Brian; Rockosi, Constance; Newberg, Heidi J.; Cudworth, Kyle M.; Pan, Kaike (2008). "The Segue Stellar Parameter Pipeline. Ii. Validation with Galactic Globular and Open Clusters". The Astronomical Journal. 136 (5): 2050–2069. arXiv: 0710.5778 . Bibcode:2008AJ....136.2050L. doi:10.1088/0004-6256/136/5/2050. S2CID   119247147.
  5. ↑ "Confirmed Exoplanet Overview". exoplanetarchive. Retrieved 4 March 2016.
  6. 1 2 "Cl* NGC 2682 YBP 1194". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 4 March 2014.
  7. 1 2 3 David Dickinson (January 15, 2014). "New exoplanet discoveries in open star cluster". Postmedia News. Archived from the original on February 20, 2014. Retrieved March 4, 2014.
  8. ↑ A. Önehag; A. Korn; B. Gustafsson; E. Stempels; D. A. VandenBerg (2011). "M67-1194, an unusually Sun-like solar twin in M67". Astronomy and Astrophysics. 528: A85. arXiv: 1009.4579 . Bibcode:2011A&A...528A..85O. doi:10.1051/0004-6361/201015138. S2CID   119116626.
  9. ↑ M67 Cluster
  10. ↑ Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics . 650: A201. arXiv: 2104.14972 . Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID   233476431. Data available at https://gruze.org/10pc/
  11. 1 2 Brucalassi, A.; Koppenhoefer, J.; et al. (July 2017). "Search for giant planets in M 67. IV. Survey results". Astronomy & Astrophysics . 603: A85. arXiv: 1703.04296 . Bibcode:2017A&A...603A..85B. doi:10.1051/0004-6361/201527562.
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