HR 7135

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HR 7135
Observation data
Epoch J2000       Equinox J2000
Constellation Aquila
Right ascension 18h 55m 27.46151s [1]
Declination +06° 36′ 55.1499″ [1]
Apparent magnitude  (V)5.57 [2]
Characteristics
Spectral type G9 III [3]
U−B color index +0.87 [2]
B−V color index +1.041±0.002 [4]
Astrometry
Radial velocity (Rv)23.31±0.09 [5]  km/s
Proper motion (μ)RA: +7.972 [1]   mas/yr
Dec.: –92.211 [1]   mas/yr
Parallax (π)11.5405 ± 0.1636 [1]   mas
Distance 283 ± 4  ly
(87 ± 1  pc)
Absolute magnitude  (MV)0.87 [4]
Orbit [5] [6]
PrimaryHR 7135 A
CompanionHR 7135 B
Period (P)2,994±29 d
Semi-major axis (a)26.6±3.4  mas
Eccentricity (e)0.243±0.026
Inclination (i)31.9±3.6°
Longitude of the node (Ω)12.6±7.7°
Periastron epoch (T)2444276.5±52  JD
Argument of periastron (ω)
(secondary)		35±7°
Semi-amplitude (K1)
(primary)		4.65±0.13 km/s
Details
HR 7135 A
Mass 1.54 [7]   M☉
Radius 10.69+0.17
−0.93 [1]   R☉
Luminosity 52.8±0.9 [1]   L☉
Surface gravity (log g)2.7 [8]   cgs
Temperature 4,666±51 [7]   K
Metallicity [Fe/H]–0.26 [8]   dex
Rotational velocity (v sin i)0.0 [8]  km/s
Age 3.21 [7]   Gyr
Other designations
62 Ser, BD+06°3978, FK5  3509, HD  175515, HIP  92872, HR  7135, SAO  124050 [9]
Database references
SIMBAD data

HR 7135 is a binary star system. Despite its Flamsteed designation of 62 Serpentis, the star can be found in the equatorial constellation of Aquila, [10] in front of a dark rift in the Milky Way near the constellation border. [5] It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57. [2] The system is located 283  light years distant from the Sun, based on parallax, [1] and is drifting further away with a radial velocity of 23 km/s. [5]

Discovery of the binary nature of this system is credited to Canadian astronomer H. H. Plaskett in 1922. It is a single-lined spectroscopic binary with an orbital period of 8.2 years and an eccentricity of 0.24. [5] [6] The visible component is an aging giant star with a stellar classification of G9 III, [3] having exhausted the supply of hydrogen at its core and expanded to 10.7 [1] times the Sun's radius. It is a red clump giant, indicating it is on the horizontal branch and is generating energy via core helium fusion. [11] The star is 3.2 [7]  billion years old with 1.54 [7] times the mass of the Sun. It is radiating 53 [1] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,666 K. [7] The star has a very low rate of spin, with the projected rotational velocity being too small to measure. [8]

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Phi Aquarii Star in the constellation Aquarius

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1 Aquarii Binary star in the constellation Aquarius

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31 Vulpeculae Star in the constellation Vulpecula

31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s.

HD 173780 is a single star in the northern constellation Lyra, near the southern constellation border with Hercules. It is an orange-hued star that is faintly visible to the naked eye with an apparent visual magnitude of +4.84. This object is located at a distance of approximately 237 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −17 km/s.

27 Hydrae is a member of a triple star system system in the equatorial constellation of Hydra, located 222 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with a combined apparent visual magnitude of 4.82. The system is moving further from the Earth with a heliocentric radial velocity of +25.6 km/s.

6 Persei is a binary star system in the northern constellation of Andromeda. It is faintly visible to the naked eye with an apparent visual magnitude of 5.29. The system is located 182 light years from Earth, as determined from its annual parallax shift of 17.9 mas. It is moving further away with a heliocentric radial velocity of +42 km/s. The system has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.386 arcsecond/year.

Theta Librae Star in the constellation Libra

θ Librae, Latinised as Theta Librae, is a single star in the southern zodiac constellation of Libra, near the constellation border with Scorpius. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.14. The distance to this star is approximately 168 light years, as determined by parallax, and it is drifting further away with a radial velocity of 5 km/s. The position of this star near the ecliptic means it is subject to lunar occultations.

Xi Piscium Binary star system in the constellation Pisces

Xi Piscium (ξ Piscium) is an orange-hued binary star system in the zodiac constellation of Pisces. In 1690, the astronomer Johannes Hevelius in his Firmamentum Sobiescianum regarded the constellation Pisces as being composed of four subdivisions. Xi Piscium was considered to be part of the Linum Austrinum, the South Cord. The star is visible to the naked eye, having an apparent visual magnitude of 4.60. Based upon an annual parallax shift of 11.67 mas as seen from Earth, it is located about 280 light years from the Sun. It is moving away from the Sun, having a radial velocity of +26 km/s.

HD 106760 is a single-lined spectroscopic binary star system in the northern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.99. The system is located around 38 light years away, as determined from its annual parallax shift of 10.2417 mas. It is moving closer with a heliocentric radial velocity of −40 km/s, and is expected to come as close as 259 ly in about 772,000 years.

Chi Geminorum is a binary star system in the constellation Gemini, near the western border with Cancer. It can be viewed with the naked eye on a dark night, having an apparent visual magnitude of 4.98. Based upon an annual parallax shift of 12.73 mas, it is located roughly 260 light years from the Sun.

Phi3 Hydrae is a binary star in the equatorial constellation of Hydra. It originally received the Flamsteed designation of 2 Crateris before being placed in the Hydra constellation. Based upon an annual parallax shift of 15.49 mas as seen from Earth, it is located around 211 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.90. It forms a triangle with the fainter φ1 Hydrae and φ2 Hydrae, between μ Hydrae and ν Hydrae.

41 Ophiuchi Star in the constellation Ophiuchus

41 Ophiuchi is a binary star system in the zodiac constellation of Ophiuchus, and is positioned less than half a degree to the south of the celestial equator. It is visible to the naked eye as a faint, orange-hued point of light with a combined apparent visual magnitude of 4.72. The distance to this system is approximately 202 light years based on parallax.

70 Pegasi is a binary star system in the northern constellation Pegasus. It is a faint star, visible to the naked eye under good seeing conditions, with an apparent visual magnitude of 4.56. The measured annual parallax shift measured from Earth's orbit is 18.65 mas, yielding a distance estimate of around 175 light years. The visual magnitude of the star is diminished by an extinction of 0.07±0.02 due to interstellar dust. It is moving closer to the Sun with a radial velocity of −17 km/s.

33 Piscium Star in the constellation Pisces

33 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.61. The distance to this system, as determined from an annual parallax shift of 25.32±0.53 mas, is about 129 light years. It is moving closer to the Sun with a heliocentric radial velocity of −6.6 km/s.

RR Ursae Minoris, abbreviated RR UMi, is a binary star system in the northern circumpolar constellation of Ursa Minor. It can be viewed with the naked eye, typically having an apparent visual magnitude of around 4.710. Based upon an annual parallax shift of 10.0 mas as seen from Earth's orbit, it is located 330 light years away. The system is moving further from the Sun with a heliocentric radial velocity of +6 km/s.

16 Serpentis is a binary star system in the Serpens Caput portion of the equatorial constellation of Serpens, located 228 light years from the Sun. It is visible to the naked eye as a fain, orange-hued star with an apparent visual magnitude of 5.261. The system is moving further from the Earth with a heliocentric radial velocity of +3 km/s.

6 Serpentis is a binary star system in the constellation Serpens. It has a combined apparent visual magnitude of 5.382, which is bright enough to be faintly visible to the naked eye. The distance to this system, based upon an annual parallax shift of 13.63±0.73 mas, is about 240 light years. It is moving further from the Sun with a heliocentric radial velocity of +10 km/s.

References

  1. 1 2 3 4 5 6 7 8 9 10 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 Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. 1 2 McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances", Astrophysical Journal Supplement Series, 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527
  4. 1 2 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.
  5. 1 2 3 4 5 Griffin, R. F. (1981), "Spectroscopic binary orbits from photoelectric radial velocities. Paper 41: HR 7135", The Observatory, 101: 208–211, Bibcode:1981Obs...101..208G.
  6. 1 2 Jancart, S.; et al. (2005), "Astrometric orbits of SB9 stars", Astronomy and Astrophysics, 442 (1): 365–380, arXiv: astro-ph/0507695 , Bibcode:2005A&A...442..365J, doi:10.1051/0004-6361:20053003, S2CID   15123997.
  7. 1 2 3 4 5 6 Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv: 1507.01466 , Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID   118505114.
  8. 1 2 3 4 Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi: 10.1088/0004-6256/135/1/209 .
  9. ↑ "HD 175515". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-08-04.
  10. ↑ Kaler, James B. (1996), The ever-changing sky: a guide to the celestial sphere, Cambridge University Press, p. 119, ISBN   0-521-38053-7.
  11. ↑ Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv: astro-ph/0003329 , Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID   16673121.
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