72 Herculis

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72 Herculis
Observation data
Epoch J2000       Equinox J2000
Constellation Hercules
Right ascension 17h 20m 39.56754s [1]
Declination +32° 28′ 03.8773″ [1]
Apparent magnitude  (V)5.377±0.005 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type G0 V [3]
U−B color index +0.06 [4]
B−V color index +0.62 [4]
Variable type Suspected
Astrometry
Radial velocity (Rv)−78.608±0.0065 [5]  km/s
Proper motion (μ)RA: +135.731 [1]   mas/yr
Dec.: −1040.913 [1]   mas/yr
Parallax (π)68.7539 ± 0.0904  mas
Distance 47.44 ± 0.06  ly
(14.54 ± 0.02  pc)
Absolute magnitude  (MV)4.43±0.05 [2]
Details
Mass 0.91  M☉ [2] or
1.18 [6]   M☉
Radius 1.13+0.004
−0.007 [1]   R☉
Luminosity 1.331±0.003 [1]   L☉
Surface gravity (log g)4.26±0.10 [2]   cgs
Temperature 5,745±35 [7]   K
Metallicity [Fe/H]−0.31±0.11 [7]   dex
Rotational velocity (v sin i)1.0±1.0 [2]  km/s
Age 4.1–6.6 [8]   Gyr
Other designations
w Her, 72 Her, NSV  8553, BD+32°2896, FK5  1456, GJ  672, HD  157214, HIP  84862, HR  6458, SAO  65963, LHS  441, LTT  15148 [9]
Database references
SIMBAD data

72 Herculis is a single [10] star in the northern constellation of Hercules. The Flamsteed designation for this star comes from the publication Historia Coelestis Britannica by John Flamsteed. It is the 72nd star in Flamsteed's list of stars in Hercules. This star is faintly visible to the naked eye with an apparent visual magnitude of 5.4. [2] Parallax measurements show this star to be located at a distance of about 47 light years from the Sun. [1] It is drifting closer with a radial velocity of −78.6 km/s, [5] and is predicted to come to within 32.1 light-years in around 98,000 years. [6]

This is an ordinary G-type main-sequence star with a stellar classification of G0 V. It is similar in mass to the Sun, [2] with a 13% larger radius. [1] The star is radiating 1.3 [1] times the luminosity of the Sun from its photosphere at an effective temperature of 5,745 K. [7] The metallicity is much lower than in the Sun, with an [Fe/H] equal to −0.31±0.11. [7] The star is an estimated 4–7 [8]  billion years old with a projected rotational velocity of 1 km/s. [2] The level of chromospheric activity appears to be at or below that in the Sun. [11]

As of 2010, no planetary companion had been detected orbiting this star. [12] The Washington Visual Double Star Catalog for 1996 showed two visual companions of this star. The first is a visual magnitude 9.7 star located 289.1 arc seconds away. The second is only separated by 8.7 arc seconds, and is magnitude 12.9. [13] It is unknown whether these visual companions are gravitationally-bound to 72 Her.

Related Research Articles

107 Piscium is a single star in the constellation of Pisces. 107 Piscium is the star's Flamsteed designation. John Flamsteed numbered the stars of Pisces from 1 to 113, publishing his Catalogus Britannicus in 1725. He accidentally numbered 107 Piscium twice, as he also allocated it the designation of 2 Arietis. This star is faintly visible to the naked eye with an apparent visual magnitude that has been measured varying between 5.14 and 5.26. However, that finding of variation was not confirmed by subsequent observations and is most likely spurious data. It is located at a distance of about 24.8 light years away from the Sun. 107 Piscium is drifting closer to the Sun with a radial velocity of −33.6, and is predicted to come as close as 15.4 light-years in around 135,800 years.

37 Geminorum is a solitary Sun-like star located at the northwest part of the northern constellation of Gemini, about three degrees to the east of the bright star Epsilon Geminorum. The apparent visual magnitude of 37 Geminorum is 5.74, which is just bright enough to be visible to the naked eye on a dark night. It is located at a distance of 57 light years from the Sun based on parallax. This star is drifting closer with a radial velocity of −15 km/s, and is predicted to come as near as 13.8 light-years in approximately a million years. It is positioned close enough to the ecliptic to be subject to lunar occultations, such as happened on April 8, 1984.

Lambda1 Tucanae is the Bayer designation for one member of a pair of stars sharing a common proper motion through space, which lie within the southern constellation of Tucana. As of 2013, the pair had an angular separation of 20.0 arc seconds along a position angle of 82°. Together, they are barely visible to the naked eye with a combined apparent visual magnitude of 6.21. Based upon an annual parallax shift for both stars of approximately 16.5 mas as seen from Earth, this system is located roughly 198 light years from the Sun.

60 Aquarii is a star located 375 light years away from the Sun in the equatorial constellation of Aquarius. 60 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.89. The star is moving closer to the Earth with a heliocentric radial velocity of –8 km/s.

11 Aquilae is a single star in the equatorial constellation of Aquila. 11 Aquilae is the Flamsteed designation. It has an apparent visual magnitude of 5.2, which means it is faintly visible to the naked eye. Based upon an annual parallax shift of 20.9 mas, the distance to this star is approximately 156 light-years. The brightness of this star is diminished by 0.33 in magnitude because of extinction from interstellar gas and dust.

<span class="mw-page-title-main">14 Aurigae</span> Quadruple star system in the constellation Auriga

14 Aurigae is a quadruple star system located 269 light years away from the Sun in the zodiac constellation of Auriga. It has the variable star designation KW Aurigae, whereas 14 Aurigae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.01. The system is moving closer to the Sun with a heliocentric radial velocity of −9 km/s.

HD 4308 is a single star with an orbiting exoplanet in the southern constellation of Tucana. It has a yellow hue and is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of 6.54. This object is located at a distance of 72 light years, as determined from parallax measurements. It is a population II star and is considered to be a member of the thick disk. The star is receding from the Sun with a radial velocity of +95 km/s.

<span class="mw-page-title-main">Nu Phoenicis</span> Star in the constellation Phoenix

Nu Phoenicis is a F-type main-sequence star in the southern constellation of Phoenix. It is visible to the naked eye with an apparent visual magnitude of 4.95. This is a solar analogue, meaning its observed properties appear similar to the Sun, although it is somewhat more massive. At an estimated distance of around 49.5 light years, this star is located relatively near the Sun.

HR 4458 is a binary star system in the equatorial constellation of Hydra. It has the Gould designation 289 G. Hydrae; HR 4458 is the Bright Star Catalogue designation. At a distance of 31.13 light years, it is the closest star system to the Solar System within this constellation. This object is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.97. It is moving closer to the Earth with a heliocentric radial velocity of −22 km/s.

<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.

<span class="mw-page-title-main">45 Herculis</span> Star in the constellation Hercules

45 Herculis is a solitary variable star in the northern constellation Hercules. It has the Bayer designation l Herculis and the variable star designation V776 Herculis. The Flamsteed designation for this star comes from the publication Historia Coelestis Britannica by John Flamsteed. It is the 45th star in Flamsteed list of stars in the constellation Hercules, and is visible to the naked eye with a baseline apparent visual magnitude of 5.22. Parallax measurements show this star to be about 400 light-years away from the Solar System. It is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.

HD 24496 is a binary star system in the equatorial constellation of Taurus. The combined apparent visual magnitude of the pair is 6.81, which is too faint to be readily visible to the normal human eye. The system is located at a distance of 66.8 light-years from the Sun, based on parallax, and is drifting further away with a radial velocity of +19 km/s. It is traversing the celestial sphere with a proper motion of 0.276″ per year.

ADS 48 is a multiple star system in the constellation of Andromeda consisting of 7 stars. The components, in order from A to G, have apparent visual magnitudes of 8.826, 8.995, 13.30, 12.53, 11.68, 9.949, and 13.00.

<span class="mw-page-title-main">HD 190007</span> Star in the constellation Aquila

HD 190007, also known as Gliese 775, is a star with a close orbiting exoplanet in the constellation of Aquila. Parallax measurements by Gaia put the star at a distance of 41.5 light-years away from the Sun. It is drifting closer with a radial velocity of −30.3 km/s, and is predicted to come within 11.8 light-years in 375,000 years. The star has an absolute magnitude of 6.91, but at its present distance the apparent visual magnitude is 7.46, which is too faint to be viewed with the naked eye.

20 Camelopardalis is a solitary star in the circumpolar constellation Camelopardalis. It has an apparent magnitude of 7.45, making it readily visible in binoculars but not to the naked eye. Located about 880 light years away, it is approaching the Solar System with a radial velocity of −50.3 km/s. Due to its faintness, 20 Cam is one of the 220 Flamsteed stars without Bright Star Catalog designations.

HD 114837 is a suspected binary star system in the southern constellation of Centaurus. The brighter star is faintly visible to the naked eye with an apparent visual magnitude of 4.90. It has a magnitude 10.2 candidate common proper motion companion at an angular separation of 4.2″, as of 2014. The distance to this system, based on an annual parallax shift of 55.0143″ as seen from Earth's orbit, is 59.3 light years. It is moving closer with a heliocentric radial velocity of −64 km/s, and will approach to within 21.8 ly in around 240,600 years.

49 Librae is the Flamsteed designation for a binary star system in the Zodiac constellation of Libra. It has an apparent visual magnitude of 5.47, making it faintly visible to the naked eye from dark suburban skies as a dim, yellow-white hued star. The system is located 95 light years away from the Sun, based on parallax, but is drifting closer with a radial velocity of −20 km/s.

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.

<span class="mw-page-title-main">9 Ceti</span> Star in the constellation Cetus

9 Ceti is a star in the equatorial constellation of Cetus. It has the variable star designation BE Ceti, while 9 Ceti is the Flamsteed designation. It has an apparent visual magnitude of 6.4, which is below the limit that can be seen with the naked eye by a typical observer. Based upon parallax measurements, this star is 69.6 light years away from the Sun.

<span class="mw-page-title-main">15 Leonis Minoris</span> Star in the constellation Ursa Major

15 Leonis Minoris is the Flamsteed designation for a single star in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of 5.08, making it a fifth magnitude star that is visible to the naked eye. Based on parallax measurements, it is located at a distance of 61.7 light years from the Sun. The star has been examined for an infrared excess, but none was detected.

References

  1. 1 2 3 4 5 6 7 8 9 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.
  2. 1 2 3 4 5 6 7 8 Fuhrmann, Klaus (February 2008). "Nearby stars of the Galactic disc and halo - IV". Monthly Notices of the Royal Astronomical Society . 384 (1): 173–224. Bibcode:2008MNRAS.384..173F. doi: 10.1111/j.1365-2966.2007.12671.x .
  3. ↑ Cenarro, A. J.; et al. (July 2009). "Mg and TiO spectral features at the near-IR: spectrophotometric index definitions and empirical calibrations". Monthly Notices of the Royal Astronomical Society. 396 (4): 1895–1914. arXiv: 0903.4835 . Bibcode:2009MNRAS.396.1895C. doi: 10.1111/j.1365-2966.2009.14839.x . S2CID   15729759.
  4. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. SIMBAD. Bibcode:1986EgUBV........0M.
  5. 1 2 Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv: 1804.09370 . Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID   52952408.
  6. 1 2 Bailer-Jones, C.A.L.; et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv: 1805.07581 . Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID   56269929.
  7. 1 2 3 4 Stonkutė, E.; et al. (2020). "High-resolution Spectroscopic Study of Dwarf Stars in the Northern Sky: Lithium, Carbon, and Oxygen Abundances". The Astronomical Journal. 159 (3): 90. arXiv: 2002.05555 . Bibcode:2020AJ....159...90S. doi: 10.3847/1538-3881/ab6a19 . S2CID   211096705.
  8. 1 2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv: 0807.1686 . Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID   27151456.
  9. ↑ "72 Her". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 January 2018.
  10. ↑ Fuhrmann, K.; et al. (February 2017). "Multiplicity among Solar-type Stars". The Astrophysical Journal. 836 (1): 23. Bibcode:2017ApJ...836..139F. doi: 10.3847/1538-4357/836/1/139 . 139.
  11. ↑ Hall, Jeffrey C.; et al. (July 2009). "The Activity and Variability of the Sun and Sun-Like Stars. II. Contemporaneous Photometry and Spectroscopy of Bright Solar Analogs". The Astronomical Journal. 138 (1): 312–322. Bibcode:2009AJ....138..312H. doi: 10.1088/0004-6256/138/1/312 . S2CID   12332945.
  12. ↑ Lubin, Dan; et al. (June 2010). "Lithium Abundance in Solar-type Stars with Low Chromospheric Activity: Application to the Search for Maunder Minimum Analogs". The Astrophysical Journal. 716 (1): 766–775. Bibcode:2010ApJ...716..766L. doi: 10.1088/0004-637X/716/1/766 .
  13. ↑ 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 .
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