83 Leonis

Last updated
83 Leonis
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Leo
83 Leonis A
Right ascension 11h 26m 45.32173s [1]
Declination +03° 00′ 47.1566″ [1]
Apparent magnitude  (V)6.49
83 Leonis B
Right ascension 11h 26m 46.27833s [2]
Declination +03° 00′ 22.7567″ [2]
Apparent magnitude  (V)7.58 [3]
Characteristics
Spectral type G9IV-V [4] / K2V [5]
U−B color index 1.024 (83 Leonis B) [6]
B−V color index 0.913 (83 Leonis B) [6]
Variable type None
Astrometry
83 Leonis A
Radial velocity (Rv)4.18±0.13 [1]  km/s
Proper motion (μ)RA: −725.963(29)  mas/yr [1]
Dec.: 180.980(30)  mas/yr [1]
Parallax (π)55.0090 ± 0.0240  mas [1]
Distance 59.29 ± 0.03  ly
(18.179 ± 0.008  pc)
83 Leonis B
Radial velocity (Rv)3.63±0.13 [2]  km/s
Proper motion (μ)RA: −728.131(34)  mas/yr [2]
Dec.: 188.554(27)  mas/yr [2]
Parallax (π)55.0618 ± 0.0304  mas [2]
Distance 59.23 ± 0.03  ly
(18.16 ± 0.01  pc)
Details
83 Leonis A
Mass 0.95 ± 0.06 [7]   M☉
Radius 0.96+0.04
−0.02 [8]   R☉
Luminosity 0.74 [7]   L☉
Surface gravity (log g)4.42 [7]   cgs
Temperature 5509 ± 8.6 [9]   K
Metallicity 0.30 [7]
Age 8.09 ± 6.75 [7]   Gyr
83 Leonis B
Mass 0.85±0.02 [3]   M☉
Radius 0.78±0.02 [3]   R☉
Luminosity (bolometric)0.418 ± 0.057 [5]   L☉
Surface gravity (log g)4.57±0.06 [3]   cgs
Temperature 4929±44 [3]   K
Metallicity 0.3±0.03 [3]
Rotation 40-45 days [10]
Rotational velocity (v sin i)0.41±0.5 [3]  km/s
Age 4.8±4.1 [3]   Gyr
Other designations
BD+03° 2502/3, GJ  429, HD  99491/99492, HIP  55846, HR  4414, Wolf  393 [11]
Database references
SIMBAD HD 99491
HD 99492

83 Leonis, abbreviated 83 Leo, is a binary star system approximately 59 light-years away in the constellation of Leo (the Lion). The primary star of the system is a cool orange subgiant star, while the secondary star is an orange dwarf star. The two stars are separated by at least 515 astronomical units from each other. Both stars are presumed to be cooler than the Sun.

Contents

The primary star is also known as HD 99491 and the secondary star as HD 99492. In 2005, an exoplanet was confirmed to be orbiting the secondary star within the system. [12]

Stellar system

The primary component, 83 Leonis A, is a 6th magnitude star. It is not visible to the unaided eye, but easily visible with small binoculars. The star is classified as a subgiant, meaning that it has ceased fusing hydrogen in its core and started to evolve towards red gianthood.

The secondary component, 83 Leonis B, is an 8th magnitude orange dwarf, somewhat less massive (0.88 MSun), smaller and cooler than the Sun. [13] It is visible only with binoculars or better equipment. Components A and B share common proper motion, which confirms them as a physical pair. The projected separation between the stars is 515 AU, but the true separation may be much higher. [14]

There is yet another, magnitude 14.4 component listed in the Washington Double Star Catalog. However, this star is moving into a different direction and is therefore not a true member of the 83 Leonis system.

Planetary system

Planet 83 Leonis Bb was discovered in Jan 2005 by the California and Carnegie Planet Search team, who use the radial velocity method to detect planets. The planet's minimum mass is less than half of the mass of Saturn. It orbits very close to the star, completing one orbit in about 17 days. [12]

In 2010, a second planet, 83 Leonis Bc, was claimed, [5] but was found to be a false positive in 2016. [3] However, in 2023 a different second planet was discovered, also given the designation "c". [10]

The 83 Leonis B planetary system [3] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b ≥25.5±0.6  M🜨 0.123±0.00117.0503±0.00160.034+0.025
−0.021		——
c≥17.9±1.3  M🜨 —95.233+0.098
−0.096		0.063+0.060
−0.040		——

See also

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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 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.
  3. 1 2 3 4 5 6 7 8 9 10 Kane, Stephen R.; Thirumalachari, Badrinath; Henry, Gregory W.; Hinkel, Natalie R.; Jensen, Eric L. N.; Boyajian, Tabetha S.; Fischer, Debra A.; Howard, Andrew W.; Isaacson, Howard T.; Wright, Jason T. (2016). "Stellar Activity and Exclusion of the Outer Planet in the Hd 99492 System". The Astrophysical Journal. 820 (1): L5. arXiv: 1603.00487 . Bibcode:2016ApJ...820L...5K. doi: 10.3847/2041-8205/820/1/L5 . S2CID   16443458.
  4. ↑ Abt, H. A. (1986). "The Ages and Dimensions of Trapezium Systems". Astrophysical Journal. 304: 688. Bibcode:1986ApJ...304..688A. doi:10.1086/164207.
  5. 1 2 3 Meschiari, Stefano; et al. (2011). "The Lick-Carnegie Survey: Four New Exoplanet Candidates". The Astrophysical Journal. 727 (2). 117. arXiv: 1011.4068 . Bibcode:2011ApJ...727..117M. doi:10.1088/0004-637X/727/2/117. S2CID   59065004.
  6. 1 2 Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (2010). "UBV(RI)C JHK observations of Hipparcos-selected nearby stars". Monthly Notices of the Royal Astronomical Society. 403 (4): 1949–1968. Bibcode:2010MNRAS.403.1949K. doi: 10.1111/j.1365-2966.2009.16182.x .
  7. 1 2 3 4 5 Luck, R. Earle (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 . 21.
  8. ↑ 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.
  9. ↑ Kovtyukh, V. V.; et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics. 411 (3): 559–564. arXiv: astro-ph/0308429 . Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID   18478960.
  10. 1 2 3 Stalport, M.; Cretignier, M.; et al. (August 2023). "A review of planetary systems around HD 99492, HD 147379 and HD 190007 with HARPS-N". Astronomy & Astrophysics . 678: A90. arXiv: 2308.05669 . Bibcode:2023A&A...678A..90S. doi:10.1051/0004-6361/202346887. S2CID   260775534.
  11. ↑ "83 Leo". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 15 February 2018.
  12. 1 2 Marcy, Geoffrey W.; et al. (2005). "Five New Extrasolar Planets" (PDF). The Astrophysical Journal. 619 (1): 570–584. Bibcode:2005ApJ...619..570M. doi:10.1086/426384. S2CID   5803173.
  13. ↑ "The Planet Around HD 99492". California & Carnegie Planet Search. Archived from the original on 2005-12-16. Retrieved 2006-05-09.
  14. ↑ Raghavan, Deepak; et al. (2006). "Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems". The Astrophysical Journal. 646 (1): 523–542. arXiv: astro-ph/0603836 . Bibcode:2006ApJ...646..523R. doi:10.1086/504823. S2CID   5669768.
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