113 Herculis

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113 Herculis
Hercules constellation map.svg
Red circle.svg
Location of 113 Herculis (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Hercules [1]
Right ascension 18h 54m 44.88499s [2]
Declination +22° 38′ 42.2715″ [2]
Apparent magnitude  (V)4.57 [1]
Characteristics
Giant
Evolutionary stage Red clump [3]
Spectral type G8III+ [1]
Main sequence
Evolutionary stage Main Sequence [3]
Spectral type A0.5 [1]
Astrometry
Radial velocity (Rv)−21.94±1.84 [2] km/s
Proper motion (μ)RA: +6.571 mas/yr [2]
Dec.: +1.305 mas/yr [2]
Parallax (π)7.5501±0.2067  mas [2]
Distance 430 ± 10  ly
(132 ± 4  pc)
Absolute magnitude  (MV)−1.23 [1]
Orbit [4] [3]
Period (P)245.325±0.006 days
Semi-major axis (a)0.0101±0.0001″
Eccentricity (e)0.101±0.005
Inclination (i)40.2±0.6°
Longitude of the node (Ω)70.1±1.2°
Periastron epoch (T)2447784.1±0.8  JD
Argument of periastron (ω)
(secondary)		186.7±2.0°
Semi-amplitude (K1)
(primary)		15.48±0.09 km/s
Semi-amplitude (K2)
(secondary)		22.58±0.30 km/s
Details [3]
A
Mass 3.045  M☉
Radius 22.2  R☉
Temperature 5047  K
Age 390.9  Myr
B
Mass 2.087  M☉
Radius 2.05  R☉
Temperature 9506  K
Age 390.9  Myr
Other designations
113 Her, BD+22 3524, GC 25954, HD 175492, HD 175493, HIP 92818, HR 7133, SAO 86567, PPM 108046, ADS 11820, TYC 2109-2837-1, IRAS 18526+2234 [5]
Database references
SIMBAD data

113 Herculis is a binary star system located about 430 light-years (130 parsecs ) away in the constellation Hercules. With an apparent magnitude of 4.6, it is faintly visible to the naked eye. [6]

This star was first discovered to be a spectroscopic binary in 1900 by W. W. Campbell and W. H. Wright. [7] The two stars orbit with a period of 245.3 days. [4]

Charecterstics

113 Herculis is a spectroscopic double-line binary with an orbital period of 245.33 days and an eccentricity of 0.10. The system is estimated to be 391 million years old. It contains an evolved primary star, designated 113 Herculis Aa, and generally classified as a G-type yellow giant. It is a red clump star , meaning that it generates its energy by the fusion of helium in its core. It is estimated to be 3.15 times more massive than the Sun and its radius is nearly 24 times larger than the Sun's radius. Its surface temperature is 4,775  K . The Secondary component, 113 Herculis Ab, is a white main-sequence star of type A0 to A8. It is 2.18 times more massive than the Sun and its radius is 2.1 times larger than the solar radius. Its surface temperature is 9,183 K. [3] [8]

Double and multiple star catalogs list two visual companions of magnitude 11.1 near 113 Herculis. Designated B and C, they were located at 34.4 and 36.9  arcseconds respectively from 113 Herculis A in 2001. [9] Eggleton & Tokovinin (2008) proposed that these two stars are physically bound to the system, [10] but measurements of their annual parallaxes of components B and C by the Gaia satellite show that they are much more distant, at distances of about 590 parsecs (1,900 ly) [11] and about 4 kiloparsecs (13 kly) [12] respectively.

References

  1. 1 2 3 4 5 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. XHIP record for this object 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 Eggleton, Peter P.; Yakut, Kadri (July 2017). "Models for 60 double-lined binaries containing giants". Monthly Notices of the Royal Astronomical Society . 468 (3): 3533–3556. arXiv: 1611.05041 . Bibcode:2017MNRAS.468.3533E. doi: 10.1093/mnras/stx598 .
  4. 1 2 Hummel, C. A.; Armstrong, J. T.; et al. (July 1995). "Orbits of Small Angular Scale Binaries Resolved with the Mark III Interferometer". Astronomical Journal . 110: 376. Bibcode:1995AJ....110..376H. doi:10.1086/117528.
  5. ↑ "* 113 Her". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2 August 2025.
  6. ↑ Ford, Dominic. "113-Her (Star)". In-The-Sky.org. Retrieved 2025-10-31.
  7. ↑ Campbell, W. W.; Wright, W. H. (November 1900). "A list of nine stars whose velocities in the line of sight are variable". Astrophysical Journal . 12: 254–257. Bibcode:1900ApJ....12..254C. doi:10.1086/140765.
  8. ↑ Skiff, B. A. (October 2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009- )". VizieR Online Data Catalog. 1: B/mk. Bibcode:2014yCat....1.2023S.
  9. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  10. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008-09-11). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x .
  11. ↑ 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.
  12. ↑ 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.
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