HD 87883

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HD 87883
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Leo Minor
Right ascension 10h 08m 43.14059s [1]
Declination +34° 14′ 32.1466″ [1]
Apparent magnitude  (V)7.56 [2]
Characteristics
Spectral type K0V [3]
Apparent magnitude  (B)8.525 [2]
Apparent magnitude  (J)5.839±0.020 [2]
Apparent magnitude  (H)5.441±0.046 [2]
Apparent magnitude  (K)5.314±0.020 [2]
B−V color index 0.965±0.013 [2]
Astrometry
Radial velocity (Rv)+9.320±0.003 [4]  km/s
Proper motion (μ)RA: −64.293±0.027  mas/yr [1]
Dec.: −61.438±0.025  mas/yr [1]
Parallax (π)54.6678 ± 0.0295  mas [1]
Distance 59.66 ± 0.03  ly
(18.292 ± 0.010  pc)
Absolute magnitude  (MV)6.27 [5]
Details
Mass 0.80±0.02 [6]   M☉
Radius 0.76±0.03 [5]   R☉
Luminosity 0.338±0.008 [6]   L☉
Surface gravity (log g)4.56 [3]   cgs
Temperature 4,980±44 [5]   K
Metallicity [Fe/H]0.093±0.04 [5]   dex
Rotation 38.6 days [5]
Rotational velocity (v sin i)2.17±0.50 [5]  km/s
Age 7.6+2.8
−1.8 [6]   Gyr
Other designations
BD+34°2089, HD  87883, HIP  49699, SAO  61890, PPM  75021 [7]
Database references
SIMBAD data
Exoplanet Archive data
ARICNS data
Extrasolar Planets
Encyclopaedia 		data

HD 87883 is star in the northern constellation of Leo Minor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.56. [2] The star is located at a distance of 59.7  light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +9.3 km/s. [4] It has an absolute magnitude of 6.27. [5]

This is an ordinary K-type main-sequence star with a stellar classification of K0V. [3] It has a modest level of chromospheric activity, [5] and is rotating with a period of 38.6 days. [5] The star is smaller than the Sun, with 82% of the mass of the Sun and 76% of the Sun's radius. The age of this star is 9.8 billion years, compared with 4.6 billion years for the Sun. It is radiating 32% of the luminosity of the Sun from its photosphere at an effective temperature of 4,980 K. [5]

In August 2009, this star was found to have a planet via the radial velocity method. The orbital solution shows it to be a Super-Jupiter body in an elliptical orbit with a period of 7.54 yr and a typical separation of 3.6  AU . A relatively high deviation on the model fit suggests there may be an additional planetary companion in a close, perturbing orbit of the star. [5] The orbital parameters of the known planet do not preclude the existence of an Earth-mass planet with a dynamically-stable orbit in the habitable zone. [8] Since its orbit is relatively face-on, its true mass deviates significantly from its minimum mass, at 6.31+0.31
−0.32  MJ . [6] [9]

The HD 87883 planetary system [6]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b 6.31+0.31
−0.32  MJ 		3.77+0.12
−0.094		8.23+0.32
−0.34		0.720+0.038
−0.027		16.8+1.7
−1.4 ° 		—

See also

Related Research Articles

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HD 40979 is a triple star system in the northern constellation of Auriga. The combined brightness of this group lies below the typical limit of visibility to the naked eye at an apparent visual magnitude of 6.74. It is located at a distance of approximately 108 light years from the Sun based on parallax. The system is receding with a radial velocity of +32 km/s. It has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.182″ per year.

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.

HD 81040 is a star in the equatorial constellation of Leo. With an apparent visual magnitude of +7.73 it is too dim to be visible to the naked eye but can be viewed with a small telescope. The star is located at a distance of 112 light years from the Sun based on parallax. It is drifting further away with a radial velocity of +49 km/s, having come to within 48 light-years some 527,000 years ago.

<span class="mw-page-title-main">HD 81040 b</span>

HD 81040 b is a massive gas giant exoplanet that orbits the star HD 81040, discovered in 2005 by radial velocity. Its orbital period is just over 1000 days. It has a semimajor axis of about 1.95 AU, and its orbit is quite eccentric, at a little over 0.5.

<span class="mw-page-title-main">HD 136118</span> Star in the constellation Serpens

HD 136118 is a star in the Serpens Caput section of the Serpens constellation. The star is too dim to be readily visible to the naked eye, having an apparent visual magnitude of 6.93. It is located at a distance of 165 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −3 km/s.

HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51. The distance to this object is 167 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7.5 km/s. It has an absolute magnitude of 3.94.

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 72659 is a star in the equatorial constellation of Hydra. With an apparent visual magnitude of 7.46, his yellow-hued star is too faint to be viewed with the naked eye. Parallax measurements provide a distance estimate of 169.4 light years from the Sun, and it has an absolute magnitude of 3.98. The star is drifting closer with a radial velocity of −18.3 km/s.

HD 118203 is a star located in the northern circumpolar constellation of Ursa Major. It has the proper name Liesma, which means flame, and it is the name of a character from the Latvian poem Staburags un Liesma. The name was selected in the NameExoWorlds campaign by Latvia, during the 100th anniversary of the IAU.

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 30562 is a star in the equatorial constellation of Eridanus. It has a golden hue and can be viewed with the naked eye under good seeing conditions, having an apparent visual magnitude of 5.77. The distance to this star is 85 light years based on parallax. It is drifting further away with a high radial velocity of +77 km/s, having come to within 46.8 light-years some 236,000 years ago.

HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

Gliese 179 is a small red dwarf star with an exoplanetary companion in the equatorial constellation of Orion. It is much too faint to be visible to the naked eye with an apparent visual magnitude of 11.94. The system is located at a distance of 40.5 light-years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of –9 km/s. It is a high proper motion star, traversing the celestial sphere at an angular rate of 0.370″·yr−1.

HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.

HD 98649 is a G-type yellow dwarf star, classified as a G4V, that has approximately the same mass and diameter as the Sun, but has only 86% of its luminosity. It is considered a solar analog. HD 98649 is about 138 light-years from earth. HD 98649 is found in the Crater constellation.

HD 106515 is a binary star in the constellation of Virgo.

HD 222155 is a star in the northern constellation of Andromeda. It is a yellow star that can be viewed with binoculars or a small telescope, but is too faint to be seen with the naked eye at an apparent visual magnitude of 7.1. The imaging survey in 2017 did not detect any stellar companions to HD 222155.

HD 217786 is a binary star system in the equatorial constellation of Pisces. With an apparent visual magnitude of 7.78, it requires binoculars or a small telescope to view. The system is located at a distance of 181 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s. Kinematically, the star system belongs to the thin disk population of the Milky Way.

HD 221420 is a likely binary star system in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.81, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of 102 light years but is receding with a heliocentric radial velocity of 26.5 km/s.

References

  1. 1 2 3 4 5 6 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. 1 2 3 4 5 6 7 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  3. 1 2 3 Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv: 1611.02897 . Bibcode:2017AJ....153...21L. doi: 10.3847/1538-3881/153/1/21 . S2CID   119511744. 21.
  4. 1 2 Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv: 1804.09370 . Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID   52952408.
  5. 1 2 3 4 5 6 7 8 9 10 11 Fischer, Debra; et al. (2009). "Five planets and an independent confirmation of HD 196885 Ab from Lick Observatory". The Astrophysical Journal. 703 (2): 1545–1556. arXiv: 0908.1596 . Bibcode:2009ApJ...703.1545F. doi:10.1088/0004-637X/703/2/1545. S2CID   15524804.
  6. 1 2 3 4 5 Li, Yiting; Brandt, Timothy D.; Brandt, G. Mirek; Dupuy, Trent J.; Michalik, Daniel; Jensen-Clem, Rebecca; Zeng, Yunlin; Faherty, Jacqueline; Mitra, Elena L. (2021). "Precise Masses and Orbits for Nine Radial-velocity Exoplanets". The Astronomical Journal. 162 (6): 266. arXiv: 2109.10422 . Bibcode:2021AJ....162..266L. doi: 10.3847/1538-3881/ac27ab . S2CID   237592581.
  7. ↑ "HD 87883". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-06-25.{{cite web}}: CS1 maint: postscript (link)
  8. ↑ Agnew, Matthew T.; et al. (November 2017). "Stable habitable zones of single Jovian planet systems". Monthly Notices of the Royal Astronomical Society. 471 (4): 4494−4507. arXiv: 1706.05805 . Bibcode:2017MNRAS.471.4494A. doi:10.1093/mnras/stx1449. S2CID   119227856.
  9. ↑ Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series . 262 (21): 21. arXiv: 2208.12720 . Bibcode:2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57 . S2CID   251864022.
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