69 Herculis

Last updated
69 Herculis
Observation data
Epoch J2000       Equinox J2000
Constellation Hercules
Right ascension 17h 17m 40.25427s [1]
Declination +37° 17′ 29.3995″ [1]
Apparent magnitude  (V)4.63 (4.66 + 8.68) [2]
Characteristics
Evolutionary stage main sequence
Spectral type A2V [3]
B−V color index 0.043±0.003 [4]
Astrometry
Radial velocity (Rv)−9.90±1.78 [5]  km/s
Proper motion (μ)RA: −43.05 [1]   mas/yr
Dec.: +64.36 [1]   mas/yr
Parallax (π)18.59 ± 0.33 [1]   mas
Distance 175 ± 3  ly
(53.8 ± 1.0  pc)
Absolute magnitude  (MV)0.99 [4]
Details
69 Her A
Mass 2.12 [6]   M☉
Radius 2.2 [7]   R☉
Luminosity 36.64 [4]   L☉
Surface gravity (log g)4.02 [8]   cgs
Temperature 9,141 [8]   K
Metallicity [Fe/H]0.29 [8]   dex
Rotational velocity (v sin i)141 [8]  km/s
Age 155 [9]   Myr
Other designations
e Her, 69 Her, BD+37°2864, HD  156729, HIP  84606, HR  6436, SAO  65921 [10]
Database references
SIMBAD data

69 Herculis is a binary star [2] system in the northern constellation Hercules. It has the Bayer designation e Herculis, while 69 Herculis is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.63. [2] The distance to this system can be estimated from parallax measurements, which yields a range of 175  light years. It is moving closer to the Earth with a heliocentric radial velocity of −10 km/s. [5]

The magnitude 4.66 [2] primary, designated component A, is an A-type main-sequence star with a stellar classification of A2V. [3] It is 155 [9]  million years old with 2.12 [6] times the mass of the Sun. The star is spinning with a projected rotational velocity of 155 km/s, which is creating an equatorial bulge that is 5% larger than the star's polar radius. [9] It is about 2.2 [7] times the size of the Sun and is radiating 37 [4] times the Sun's luminosity from its photosphere at an effective temperature of 9,141 K. [8]

The secondary, component B, is magnitude 8.68 star with an angular separation of 0.840″ from the primary, as of 2008. [2] X-ray emission has been detected from this system. As A-type stars are not expected to be X-ray sources, this emission is most likely coming from the companion. [11]

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Gamma Trianguli Australis Star in the constellation Triangulum Australe

Gamma Trianguli Australis is a single, white-hued star in the southern constellation of Triangulum Australe. Along with Alpha and Beta Trianguli Australis it forms a prominent triangular asterism that gives the constellation its name. It is the third-brightest member of this constellation with an apparent visual magnitude of +2.87. based upon parallax measurements, Gamma Trianguli Australis is located at a distance of about 184 light-years from Earth.

Tau Virginis

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Chi Boötis, Latinized as χ Boötis, is a single, white-hued star in the northern constellation Boötes, near the eastern constellation border with Corona Borealis. It is faintly visible to the naked eye with an apparent visual magnitude of +5.3. Based upon an annual parallax shift of 13.0 mas as seen from the Earth, it is located about 251 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −16 km/s.

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Pi Cassiopeiae Variable star in the constellation Cassiopeia

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun.

π2 Columbae, Latinized as Pi2 Columbae, is a binary star system in the southern constellation of Columba, near the southern constellation border with Pictor. It is white-hued and dimly visible to the naked eye with a combined apparent visual magnitude of 5.50. Based upon an annual parallax shift of 12.8 mas as seen from Earth, this system is located about 254 light years from the Sun. They are receding with a heliocentric radial velocity of +31 km/s.

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Tau Herculis Variable star in the constellation Hercules

Tau Herculis, a name Latinized from τ Herculis, is a variable star in the northern constellation of Hercules. It has a blue-white hue and is visible to the naked eye at night with an apparent visual magnitude that fluctuates around 3.91. The star is located at a distance of approximately 307 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −16 km/s.

Gamma Crateris Star in the constellation Crater

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Rho Piscium Star in the constellation Pisces

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74 Cygni is a visual binary star system in the northern constellation Cygnus, located around 249 light years distant from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.04. The pair orbit each other with a period of 1.57 years and an eccentricity of 0.5. The system is a source of X-ray emission, which is most likely coming from the secondary component.

Sigma1 Gruis, a Latinization of σ1 Gruis, is a star in the constellation Grus. It is a dim, white-hued star near the lower limit for visibility to the naked eye with an apparent visual magnitude of 6.26. This object is located 229 light-years (70.1 pc) distant from the Sun based on parallax. The radial velocity of this star is poorly constrained, but it appears to be drifting further away at the rate of +7 km/s.

μ Fornacis is the Bayer designation for a star in the southern constellation of Fornax. With an apparent visual magnitude of 5.27, it is visible to the naked eye. The distance to this star, as determined by its annual parallax shift of 10.18 mas, is around 320 light years.

References

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  6. 1 2 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv: 1501.03154 , Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID   33401607.
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  8. 1 2 3 4 5 Erspamer, D.; North, P. (February 2003), "Automated spectroscopic abundances of A and F-type stars using echelle spectrographs. II. Abundances of 140 A-F stars from ELODIE", Astronomy and Astrophysics, 398 (3): 1121–1135, arXiv: astro-ph/0210065 , Bibcode:2003A&A...398.1121E, doi:10.1051/0004-6361:20021711, S2CID   1109164.
  9. 1 2 3 van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv: 1204.2572 , Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID   119273474.
  10. ↑ "69 Her". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-06-15.
  11. ↑ Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars", Astronomy and Astrophysics, 475 (2): 677−684, Bibcode:2007A&A...475..677S, doi: 10.1051/0004-6361:20077429 .
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