Wikipedia

35 Leonis

35 Leonis (HIP 53019, HD 89010) is a spectroscopic binary star system[4] located in the constellation of Leo, next to the star Zeta Leonis.[1] It is located 96.5 ly (29.6 pc) from Earth based upon parallax measurements.[2] The system consists of a G-type star (yellow dwarf) and a red dwarf star.[4] With an apparent magnitude of 5.97, it can be naked-eye visible only from dark skies.[1]

35 Leonis
Approximate location of 35 Leonis (circled)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Leo[1][note 1]
Right ascension 10h 16m 32.289s[2]
Declination +23° 30′ 11.206″[2]
Apparent magnitude (V) 5.97[1]
Characteristics
35 Leonis A
Evolutionary stage Main-sequence star to subgiant
Spectral type G1.5IV–V[3]
Apparent magnitude (U) 6.8[3]
Apparent magnitude (B) 6.6[3]
Apparent magnitude (R) 5.6[3]
Apparent magnitude (G) 5.8[3]
Apparent magnitude (J) 4.8[3]
Apparent magnitude (H) 4.5[3]
Apparent magnitude (K) 4.3[3]
B
Evolutionary stage Red dwarf
Apparent magnitude (K) 8.4[4]
Astrometry
Radial velocity (Rv)−35.25±0.79[2] km/s
Proper motion (μ) RA: −200.342±0.259 mas/yr[2]
Dec.: 32.03±0.32 mas/yr[2]
Parallax (π)33.7721 ± 0.258 mas[2]
Distance96.6 ± 0.7 ly
(29.6 ± 0.2 pc)
Absolute magnitude (MV)+3.56[5]
Orbit[4]
PrimaryA
Period (P)1.471 years
(537 days)
Details
A
Mass1.34[4] M☉
Radius2.12±0.18[5] R☉
Luminosity4.37+0.76
−0.65[5] L☉
Surface gravity (log g)3.87±0.02[5] cgs
Temperature5480±10[4] K
Metallicity [Fe/H]0.02±0.01[5] dex
Rotational velocity (v sin i)2.68±0.97[5] km/s
Age5.25+0.64
−0.57[5] Gyr
B[4]
Mass0.15 M☉
Temperature3300+130
−140 K
Rotational velocity (v sin i)<10.1 km/s
Position (relative to A)[4]
ComponentB
Angular distance56.9±0.3 mas
Other designations
BD+24 2207, Gaia DR2 725469767850488064, Gaia DR3 725469767850488064, HD 89010, HIP 50319, HR 4030, SAO 81260, PPM 100216, WDS J10167+2325B, NLTT 23866, TYC 1969-1260-1, IRAS 10137+2345, 2MASS J10163231+2330111
Database references
SIMBADdata

Properties

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35 Leonis was discovered to be a binary system in 2024, after analysis from Daniel Echeverri et al. using vortex fiber nulling, which is a technique for detecting and characterizing faint stellar companions that are close to their parent star.[4] The team derived a visual separation of 56.9 milliarcseconds between both components using the CHARA array.[4] Both stars are completing one orbit around each other every 537 days (1.47 years).[4] The system classifies as a single-lined spectroscopic binary (SB1).[4]

35 Leonis the Flamsteed designation. Other designations for this system include HD 89010 from the Henry Draper Catalogue, HIP 53019 from the Hipparcos Catalogue and HR 4030 from the Bright Star Catalogue.[3]

35 Leonis A

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The main component, 35 Leonis A, is currently a main-sequence star that is evolving into a subgiant, based on its spectral class of G1.5V-IV.[3] It has 34% more mass than the Sun,[4] 2.12 times the radius of the Sun, and irradiates four times more luminosity than it.[5] The effective temperature of 35 Leonis A is 5480 K,[4] which gives it the typical hue of a G-type star.[6] The age of the star is around 5.25 billion years,[5] which is around 14% older than the Solar System.

35 Leonis B

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The secondary component, 35 Leonis B, is a red dwarf star. The mass of 35 Leonis B is estimated at 0.15 M☉, based on a mass of 1.34 M☉ for the primary and a mass ratio of 0.11.[4] An effective temperature of 3300+130
−140 K and an upper limit in the rotational velocity of 10.1 km/s are derived from the vortex fiber nulling's parameters.[4] Other characteristics, such as the radius and luminosity, are unknown.

Notes

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  1. ^ Obtained with a right ascension of 10h 16m 32.289s and a declination of +23° 30′ 11.206″[2] on this website.

References

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  1. ^ a b c d e "35 Leonis - Star in Leo | TheSkyLive.com". theskylive.com. Retrieved 2024-03-29.
  2. ^ a b c d e f g 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. ^ a b c d e f g h i j "35 Leo". SIMBAD. Centre de données astronomiques de Strasbourg.
  4. ^ a b c d e f g h i j k l m n o p Echeverri, Daniel; Xuan, Jerry W.; Monnier, John D.; Delorme, Jacques-Robert; Wang, Jason J.; Jovanovic, Nemanja; Horstman, Katelyn; Ruane, Garreth; Mennesson, Bertrand; Serabyn, Eugene; Mawet, Dimitri; Wallace, J. Kent; Hillman, Sofia; Baker, Ashley; Bartos, Randall (April 2024). "Vortex Fiber Nulling for Exoplanet Observations: First Direct Detection of M Dwarf Companions around HIP 21543, HIP 94666, and HIP 50319". The Astrophysical Journal. 965 (2): L15. arXiv:2403.17295. Bibcode:2024ApJ...965L..15E. doi:10.3847/2041-8213/ad3619. ISSN 2041-8205.
  5. ^ a b c d e f g h i Deka-Szymankiewicz, B.; Niedzielski, A.; Adamczyk, M.; Adamów, M.; Nowak, G.; Wolszczan, A. (2018-07-01). "The Penn State - Toruń Centre for Astronomy Planet Search stars. IV. Dwarfs and the complete sample". Astronomy and Astrophysics. 615: A31. arXiv:1801.02899. Bibcode:2018A&A...615A..31D. doi:10.1051/0004-6361/201731696. ISSN 0004-6361. 35 Leo's database entry at VizieR.
  6. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16
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