HR 6594

Last updated
HR 6594
Observation data
Epoch J2000       Equinox J2000
Constellation Hercules
Right ascension 17h 41m 58.632s [1]
Declination +15° 57′ 08.76″ [1]
Apparent magnitude  (V)5.54 [2]
Characteristics
Evolutionary stage Main sequence [3]
Spectral type F4 Vw [4]
U−B color index −0.05 [5]
B−V color index +0.387±0.012 [2]
Astrometry
Radial velocity (Rv)−43.7 [6]  km/s
Proper motion (μ)RA: −1.868  mas/yr [1]
Dec.: +101.120  mas/yr [1]
Parallax (π)28.5131 ± 0.0532  mas [1]
Distance 114.4 ± 0.2  ly
(35.07 ± 0.07  pc)
Absolute magnitude  (MV)2.74 [7]
Details
HR 6594 A
Mass 1.34 [8]   M☉
Radius 0.97 [9]   R☉
Luminosity 6.17 [2]   L☉
Surface gravity (log g)4.07 [3]   cgs
Temperature 6,615 [3]   K
Metallicity [Fe/H]−0.04 [10]   dex
Rotational velocity (v sin i)31.7 [3]  km/s
Age 1.2 [8]   Gyr
Other designations
BD−16° 3256, HD  160910, HIP  86623, HR  6594, SAO  103033 [11]
Database references
SIMBAD data

HR 6594 is the Bright Star Catalogue designation for a binary star [12] system in the northern constellation of Hercules. It is faintly visible to the naked eye with an apparent visual magnitude of 5.54; [2] according to the Bortle scale, it is sufficiently bright to be visible from dark suburban skies. The distance to this system, as determined using parallax measurements, [1] is about 114  light years. It is drifting closer with a heliocentric radial velocity of −43.7 km/s, [6] and is predicted to come as near as 47 light-years in 686,000 years. [2] On the celestial sphere it is located near the star Alpha Ophiuchi; their projected separation is just 3 light years, although their actual separation is much greater. [13]

The primary is an F-type main sequence star with a stellar classification of F4 Vw, where the w indicates relatively weak metallic features in the ultraviolet spectrum. [4] This star has 134% of the Sun's mass, [8] but only 97% of the solar radius. [9] It is spinning with a projected rotational velocity of 31.7 km/s, [3] and is around 1.2 billion years old. [8] The effective temperature of the outer atmosphere is 6,615 K, [3] giving it the yellow-white hue of an F-type star. [14] The abundance of elements other than hydrogen or helium, what astronomers term the metallicity, is similar to that in the Sun. [10]

It has a magnitude 9.38 companion star orbiting with a 144-year period, a semimajor axis spanning 1.04  arcseconds, and an eccentricity of 0.42. [12] There is a third, visual companion of magnitude 14.46 at an angular separation of 154.70 arcseconds along a position angle of 271°, as of 2001. [15]

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60 Herculis is a single star located 134 light years away from the Sun in the northern constellation of Hercules, and is positioned just seven degrees away from Rasalgethi. It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.871. This star is moving closer to the Earth with a heliocentric radial velocity of −4 km/s.

Iota Delphini Star in the constellation Delphinus

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57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.90 mas provides a distance estimate of about 193 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).

π2 Gruis, Latinised as Pi2 Gruis, is a binary star system in the southern constellation of Grus. It is faintly visible to the naked eye as a yellow-white hued star with an apparent visual magnitude of 5.622. Based upon an annual parallax shift of 25.1 mas as seen from the Earth, the system is located 130 light years from the Sun.

HD 126053 is the Henry Draper Catalogue designation for a star in the equatorial constellation of Virgo. It has an apparent magnitude of 6.25, which means it is faintly visible to the naked eye. According to the Bortle scale, it requires dark suburban or rural skies to view. Parallax measurements made by the Hipparcos spacecraft provide an estimated distance of 57 light years to this star. It is drifting closer with a heliocentric radial velocity of −19.2 km/s.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID   227254300. Gaia EDR3 record for this source at VizieR.
  2. 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, S2CID   119257644.
  3. 1 2 3 4 5 6 Schröder, C.; et al. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi: 10.1051/0004-6361:200810377 .
  4. 1 2 Barry, Don C. (1970), "Spectral Classification of A and F Stars", Astrophysical Journal Supplement, 19: 281, Bibcode:1970ApJS...19..281B, doi:10.1086/190209.
  5. ↑ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  6. 1 2 Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington D.C., Bibcode:1953GCRV..C......0W.
  7. ↑ Boesgaard, A. M.; Tripicco, M. J. (April 15, 1986), "Lithium in early F dwarfs", Astrophysical Journal, Part 1, 303: 724–739, Bibcode:1986ApJ...303..724B, doi:10.1086/164120.
  8. 1 2 3 4 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.
  9. 1 2 Pasinetti-Fracassini, L. E.; et al. (February 2001), "Catalogue of Stellar Diameters (CADARS)", Astronomy and Astrophysics, 367: 521–524, arXiv: astro-ph/0012289 , Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID   425754.
  10. 1 2 Casagrande, L.; et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy & Astrophysics, 530 (A138): 21, arXiv: 1103.4651 , Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID   56118016.
  11. ↑ "HR 6594". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2016-09-12.
  12. 1 2 Malkov, O. Yu.; et al. (October 2012), "Dynamical masses of a selected sample of orbital binaries", Astronomy & Astrophysics, 546: 5, Bibcode:2012A&A...546A..69M, doi: 10.1051/0004-6361/201219774 , A69.
  13. ↑ Redfield, Seth; et al. (June 2007), "Spitzer Limits on Dust Emission and Optical Gas Absorption Variability around Nearby Stars with Edge-on Circumstellar Disk Signatures", The Astrophysical Journal, 661 (2): 944–971, arXiv: astro-ph/0703089 , Bibcode:2007ApJ...661..944R, doi:10.1086/517516, S2CID   42241365.
  14. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
  15. ↑ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 , retrieved 2015-07-22.
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