HD 16760

Last updated
HD 16760
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Perseus
Right ascension 02h 42m 21.3071s [1]
Declination +38° 37′ 07.1392″ [1]
Apparent magnitude  (V)8.74[ citation needed ]
Characteristics
Spectral type G5V [2]
B−V color index 0.715 [2]
Astrometry
Proper motion (μ)RA: 78.493±0.760 [1]   mas/yr
Dec.: −100.691±0.717 [1]   mas/yr
Parallax (π)14.3851 ± 0.4554  mas [1]
Distance 227 ± 7  ly
(70 ± 2  pc)
Absolute magnitude  (MV)5.41 [2]
Orbit [3]
CompanionHD 16760 b
Period (P)466.048±0.057  d
Semi-major axis (a)1.161±0.097  AU
Eccentricity (e)0.0812±0.0018
Inclination (i)3.164+0.810
−0.762 [4] °
Periastron epoch (T)24513802.6±1.9
Argument of periastron (ω)
(secondary)		241.9±1.4°
Semi-amplitude (K1)
(primary)		407.16±0.71 km/s
Details
HD 16760 A
Mass 0.78 ± 0.05 [2]   M☉
Radius 0.81 ± 0.27 [2]   R☉
Luminosity (bolometric)0.72 ± 0.43 [2]   L☉
Surface gravity (log g)4.47 ± 0.06 [2]   cgs
Temperature 5629 ± 44 [2]   K
Metallicity [Fe/H]+0.067 ± 0.05 [2]   dex
Rotational velocity (v sin i)0.5 ± 0.5 [2]  km/s
Age 1.3 ± 0.9 [5]   Gyr
HD 16760 b
Mass 291.9+120.7
−69.4 [4]   MJup
Other designations
2MASS  J02422130+3837073, BD+37°604, GSC  02845-02243, HIP  12638, SAO  55798, TYC  2845-2243-1
Database references
SIMBAD data
Exoplanet Archive data
Extrasolar Planets
Encyclopaedia 		data

HD 16760 is a binary star system approximately 227 light-years away in the constellation Perseus. The primary star HD 16760 (HIP 12638) is a G-type main sequence star similar to the Sun. The secondary, HIP 12635 is 1.521 magnitudes fainter and located at a separation of 14.6 arcseconds from the primary, corresponding to a physical separation of at least 660 AU. Announced in July 2009, HD 16760 has been confirmed to have a red dwarf orbiting it, formerly thought to be a brown dwarf or exoplanet. [2] [6] [4]

Stellar companion

The companion object was discovered independently by the SOPHIE extrasolar planets program [6] and the N2K Consortium. [2] It has a mass exceeding the lower limit required for fusion of deuterium in its interior. This criterion is sometimes used to distinguish between brown dwarfs, which lie above the limit, and planets which lie below the limit. [7] However its orbit is nearly circular, indicating that it may have formed in the same way as planets do, from a circumstellar disc. [6] The formation of massive planets up to 20–25 Jupiter masses has been predicted in some models of the core accretion process. [8] The identity of this object as a brown dwarf or a massive planet was thus unclear.

However, data analysed from direct imaging of the companion object using ground-based telescopes fitted with adaptive optics has revealed that it is aligned in a much more face-on orbit than previously realised. Consequently, its mass has been revised upwards. It is now no longer believed to be a large gas giant or even a brown dwarf but with a new mass calculated at around one quarter that of the Sun, or nearly 300 Jupiter masses, it easily qualifies as a stellar object, probably a red dwarf. [9] This was confirmed by Gaia astrometry in 2020. [4]

Related Research Articles

HD 4208 is a star with an orbiting exoplanetary companion in the southern constellation of Sculptor. It has a yellow hue with an apparent visual magnitude of 7.78, making it too dim to be visible to the naked eye. But with binoculars or small telescope it should be an easy target. This object is located at a distance of 111.6 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +57 km/s.

HD 150706 is a 7th magnitude star in the constellation of Ursa Minor. It is a remarkably Sun-like yellow dwarf being only 6% less massive than the Sun.

HD 28185 is a yellow dwarf star similar to the Sun located 128 light-years away from Earth in the constellation Eridanus. The designation HD 28185 refers to its entry in the Henry Draper catalogue. The star is known to possess one long-period extrasolar planet.

HD 1237 is a binary star system approximately 57 light-years away in the constellation of Hydrus.

HD 125612 is a binary star system with three exoplanetary companions in the equatorial constellation of Virgo. It is too dim to be visible to the naked eye, having an apparent visual magnitude of 8.31. The system is located at a distance of 188 light years from the Sun based on parallax measurements, but it is drifting closer with a radial velocity of −18 km/s.

Gliese 86 is a K-type main-sequence star approximately 35 light-years away in the constellation of Eridanus. It has been confirmed that a white dwarf orbits the primary star. In 1998 the European Southern Observatory announced that an extrasolar planet was orbiting the star.

HD 231701 is a yellow-white hued star in the northern constellation of Sagitta, near the southern constellation border with Aquila. With an apparent visual magnitude of 8.97, it is too dim to be viewed with the naked eye, but can be seen with powerful binoculars or a small telescope. Parallax measurements provide a distance estimate of approximately 356 light years from the Sun, but it is drifting closer with a radial velocity of −63 km/s. It is predicted to come as close as 189.5 light-years in 1.345 million years.

HD 33283 is a star in the southern constellation Lepus with one planet and a co-moving stellar companion. With an apparent visual magnitude of 8.05, the star is too faint to be seen with the naked eye. It is located at a distance of 294 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +4.5.

HD 4113 is a dual star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88. The distance to this star, as estimated by parallax measurements, is 137 light years. It is receding away from the Sun with a radial velocity of +5 km/s.

HD 73256 is a variable star in the southern constellation of Pyxis. It has the variable star designation CS Pyxidis. With a baseline apparent visual magnitude of 8.08, it requires binoculars or a small telescope to view. The star is located at a distance of 120 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +30 km/s.

HD 190228 is a star with a substellar companion in the constellation 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 star is older than the Sun with an age over 5 billion years and it is metal-poor.

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.

HD 45652 is a star with an exoplanetary companion in the equatorial constellation of Monoceros. It was officially named Lusitânia on 17 December 2019, after the IAU100 press conference in Paris by the IAU. This star has an apparent visual magnitude of 8.10, making it an 8th magnitude star that is too dim to be visible to the naked eye. The system is located at a distance of 114 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.188 arcsec yr−1.

HD 148427, formally named Timir, is a 7th-magnitude K-type subgiant star approximately 193 light years away in the constellation Ophiuchus. Its mass is 45% greater than the Sun, and it is three times the size and six times more luminous, although its age is 2½ billion years.

HD 6718 is a solar twin star in the equatorial constellation of Cetus. It has a yellow hue but is too faint to be viewed with the naked eye, having an apparent visual magnitude of 8.45. The distance to this object, as determined from parallax measurements, is 168 light years. It is drifting away from the Sun with a radial velocity of +35 km/s.

HD 156279 is a type K0 star, located 36.1 parsecs (118 ly) away from Earth. It has various alternate designations, including HIP 84171 and BD+63 1335. It is presumed to be a single star, as in 2019 all imaging surveys have failed to find any stellar companions.

HD 113337 is the primary component of binary star system LDS 2662, about 118 light-years away from Earth. The primary main-sequence star belongs to the spectral class of F6. The star system is extremely young, and it is slightly enriched in heavy elements, with an abundance of such elements at about 115% that of the Sun.

HD 22781, is a single star about 106 light-years away. It is a K-type main-sequence star. The star’s age is poorly constrained at 4.14±3.63 billion years, but is likely similar to that of the Sun. HD 22781 is heavily depleted in heavy elements, having just 45% of Sun's concentration of iron, yet is comparatively rich in carbon, having 90% of Sun`s abundance.

HD 35759 is a star with an orbiting exoplanet located in the circumpolar constellation Camelopardalis. With an apparent magnitude of 7.74, it's impossible to see with the unaided eye, but can be seen with binoculars. The distance to this system is 232 light years based on parallax measurements, and it is drifting closer with a heliocentric radial velocity of −12.6 km/s.

HD 203473 is a star in the equatorial constellation Equuleus. With an apparent magnitude of 8.23, it’s only visible by using an amateur telescope. The star is located at a distance of 237 light years based on its parallax shift but is drifting closer at a high rate of 61.7 km/s. As of 2014, no stellar companions have been detected around the star.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 Bunei Sato; Debra A. Fischer; Shigeru Ida; Hiroki Harakawa; Masashi Omiya; John A. Johnson; Geoffrey W. Marcy; Eri Toyota; Yasunori Hori; Howard Isaacson; Andrew W. Howard; Kathryn M.G. Peek (2009). "A Substellar Companion in a 1.3 yr Nearly-circular Orbit of HD 16760". The Astrophysical Journal. 703 (1): 671–674. arXiv: 0907.5080 . Bibcode:2009ApJ...703..671S. doi:10.1088/0004-637X/703/1/671. S2CID   5435270.
  3. ↑ Ment, Kristo; et al. (2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv: 1809.01228 . Bibcode:2018AJ....156..213M. doi: 10.3847/1538-3881/aae1f5 . S2CID   119243619.
  4. 1 2 3 4 Kiefer, Flavien; Hébrard, Guillaume; Lecavelier, Alain; Martioli, Eder; Dalal, Shweta; Vidal-Madjar, Alfred (2021). "Determining the true mass of radial-velocity exoplanets with Gaia 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets". Astronomy & Astrophysics. A7: 645. arXiv: 2009.14164 . Bibcode:2021A&A...645A...7K. doi:10.1051/0004-6361/202039168. S2CID   221995447.
  5. ↑ Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv: 1411.4302 . Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID   54555839.
  6. 1 2 3 Bouchy, François; Hébrard, Guillaume; Udry, Stéphane; Delfosse, Xavier; Boisse, Isabelle; Desort, Morgan; Bonfils, Xavier; Eggenberger, Anne; Ehrenreich, David; Forveille, Thierry; Le Coroller, Hervé; Lagrange, Anne-Marie; Lovis, Christophe; Moutou, Claire; Pepe, Francesco; Perrier, Christian; Pont, Frédéric; Queloz, Didier; Santos, Nuno C.; Ségransan, Damien; Vidal-Madjar, Alfred (2009). "The SOPHIE northern extrasolar planets. I. A companion close to the planet/brown-dwarf transition around HD16760". Astronomy and Astrophysics. 505 (2): 853–858. Bibcode:2009A&A...505..853B. doi: 10.1051/0004-6361/200912427 .
  7. ↑ "Definition of a "Planet"". Working Group on Extrasolar Planets (WGESP) of the International Astronomical Union.
  8. ↑ Christoph Mordasini; Yann Alibert; Willy Benz; Dominique Naef (2007). "Giant Planet Formation by Core Accretion". arXiv: 0710.5667 [astro-ph].
  9. ↑ Evans T.M.; Ireland M.J.; Kraus A.L.; Martinache F.; Stewart P.; Tuthill P.G.; Lacour S.; Carpenter, J.M.; Hillenbrand L.A. (2011). "Mapping The Shores Of The Brown Dwarf Desert III: Young Moving Groups". The Astrophysical Journal. 744 (2): 120. arXiv: 1109.5900 . Bibcode:2012ApJ...744..120E. doi:10.1088/0004-637X/744/2/120. S2CID   118650120.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.