HD 158633

Last updated
HD 158633
Observation data
Epoch J2000       Equinox J2000
Constellation Draco
Right ascension 17h 25m 00.09827s [1]
Declination +67° 18′ 24.1501″ [1]
Apparent magnitude  (V)6.44 [2]
Characteristics
Spectral type K0 V [2]
U−B color index +0.29 [3]
B−V color index +0.76 [3]
Astrometry
Radial velocity (Rv)−38.71±0.08 [2]  km/s
Proper motion (μ)RA: −531.958 [1]   mas/yr
Dec.: +4.734 [1]   mas/yr
Parallax (π)78.1653 ± 0.51  mas [1]
Distance 41.7 ± 0.3  ly
(12.79 ± 0.08  pc)
Absolute magnitude  (MV)5.89 [4]
Details
Mass 0.729 [5]   M☉
Radius 0.7891±0.0144 [5]   R☉
Luminosity 0.4090±0.0040 [5]   L☉
Surface gravity (log g)4.80 [6]   cgs
Temperature 5,203±46 [5]   K
Metallicity [Fe/H]−0.43±0.08 [7]   dex
Rotational velocity (v sin i)3.4 [8]  km/s
Age 4.27 [7]   Gyr
Other designations
BD+67°1014, GJ  675, HD  158633, HIP  85235, HR  6518, SAO  17474, LHS  287, LTT  15185 [9]
Database references
SIMBAD data

HD 158633 is a main sequence star in the northern constellation of Draco. With an apparent visual magnitude of 6.43, this star is a challenge to view with the unaided eye but it can be seen clearly with a small telescope. Based upon parallax measurements, it is located at a distance of around 42 light years from the Sun. The star is drifting closer to the Sun with a radial velocity of −39 km/s, [2] and is predicted to come to within 26.5 ly (8.1 pc) in around 190,400 years. [10]

This is a K-type main sequence star with a spectral classification of K0 V. It has about 79% of the Sun's radius and 73% of the solar mass. [5] It is an estimated 4.3 billion years old and is spinning with a projected rotational velocity of 3.4 km/s. [8] The star is emitting an excess of infrared radiation at a wavelength of 70 μm, suggesting the presence of an orbiting debris disk. [7] It has a low metallicity, with only 37% of the Sun's abundance of elements more massive than helium, [7] and has a relatively high proper motion. [1] [9]

Related Research Articles

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3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

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HD 213240 is a possible binary star system in the constellation Grus. It has an apparent visual magnitude of 6.81, which lies below the limit of visibility for normal human sight. The system is located at a distance of 133.5 light years from the Sun based on parallax. The primary has an absolute magnitude of 3.77.

HR 5256 is a star located thirty-three light-years away from the Sun in the northern circumpolar constellation of Ursa Major. It has an orange hue and is a challenge to view with the naked eye, having an apparent visual magnitude of 6.52 The distance to this star is very nearly 10 parsecs, so the absolute magnitude of 6.51 is nearly the same as the star's apparent magnitude. HR 5256 is drifting nearer to the Sun with a radial velocity of −26.4 km/s, and will make its closest approach to the Sun in about 333,000±16,000 years, when it will be at a distance of 12.72 ± 0.65 light-years.

HD 179791 is suspected variable star in the equatorial constellation of Aquila. It is a challenge to see with the naked eye even under good viewing conditions, having an apparent visual magnitude of 6.48. The distance to HD 179791 can be estimated from its annual parallax shift of 5.3 mas, which yields a value of 616 light years. It is moving further from the Earth with a heliocentric radial velocity of +16 km/s. Astrometric measurements of the star show changes in motion that may indicate it is a member of a close binary system.

HD 9578 is a candidate wide binary star system located at a distance of approximately 183 light-years from the Sun in the southern constellation of Sculptor. The main star must be viewed with binoculars or a telescope, as its low apparent visual magnitude of 8.35 is too faint to be viewed with the naked eye. The system is drifting closer to the Sun with a radial velocity of −4 km/s.

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Gliese 221, also known as BD-06 1339, is a star with an exoplanetary companion in the equatorial constellation of Orion. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 9.70 and an absolute magnitude of 8.15. Using parallax measurements, the distance to this system can be estimated as 66.2 light-years. It is receding from the Sun with a radial velocity of +23 km/s. This is a high proper motion star, traversing the celestial sphere at an angular rate of 0.333″·yr−1.

7 Cephei is a single star located approximately 820 light years away, in the northern circumpolar constellation of Cepheus. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.42.

HD 167257 is a solitary star in the southern constellation Telescopium. It has an apparent magnitude of 6.05, making it faintly visible to the naked eye. Parallax measurements place the star at a distance of 420 light years and has a radial velocity of −5.1 km/s, which is poorly constrained. This indicates that it is drifting towards the Solar System.

HD 219623 is a solitary star in the northern circumpolar constellation of Cassiopeia. HD 219623 is its Henry Draper Catalogue designation. It has an apparent visual magnitude of 5.59, which lies in the brightness range that is visible to the naked eye. According to the Bortle scale, it can be observed from dark suburban skies. Parallax measurements place it at an estimated distance of around 67.2 light years. It has a relatively high proper motion, advancing 262 mas per year across the celestial sphere.

<span class="mw-page-title-main">HD 42936</span> Star in the constellation Mensa

HD 42936 (DMPP-3) is a star located in the southern circumpolar constellation Mensa. With an apparent magnitude of 9.1, it is too faint to be detected with the naked eye but can be seen with a telescope. The star is relatively close at a distance of about 153 light years but is receding with a heliocentric radial velocity of 34.4 km/s.

HD 64484 is a solitary star in the southern circumpolar constellation Volans. With an apparent magnitude of 5.76, it is faintly visible to the naked eye under dark skies. Parallax measurements place it at a distance of 458 light years but is receding with a heliocentric radial velocity of 11 km/s.

<span class="mw-page-title-main">Eta Octantis</span> Star in the constellation of Octans

Eta Octantis, Latinized from η Octantis, is a solitary star located in the southern circumpolar constellation Octans. It has an apparent magnitude of 6.19, making it faintly visible to the naked eye. The object is situated at a distance of 358 light years but is approaching the Solar System with a heliocentric radial velocity of −1.7 km/s.

13 Delphini is a binary star in the equatorial constellation Delphinus, with a combined apparent magnitude of 5.64. The system is located at a distance of 471 light years but is approaching the Solar System with a heliocentric radial velocity of about −7 km/s.

15 Delphini is a star in the equatorial constellation Delphinus. It has an apparent magnitude of 5.99, allowing it to be faintly seen with the naked eye. The star is relatively close at a distance of 99 light years but is receding with a heliocentric radial velocity of 4.1 km/s.

<span class="mw-page-title-main">HD 31134</span> A-type dwarf; Camelopardalis

HD 31134, also designated as HR 1561, is a solitary star located in the northern circumpolar constellation Camelopardalis, the giraffe. It is faintly visible to the naked eye as a white-hued star with an apparent magnitude of 5.74. Gaia DR3 parallax measurements place it 473 light years away. It appears to be approaching the Solar System with a heliocentric radial velocity of −15.1 km/s. At its current distance, HD 31134's brightness is diminished by 0.35 magnitudes due to interstellar dust. It has an absolute magnitude of +0.19.

References

  1. 1 2 3 4 5 6 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 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 Hauck, B.; Mermilliod, M. (1998). "uvbyβ photoelectric photometric catalogue". Astronomy and Astrophysics Supplement Series. 129 (3): 431–433. Bibcode:1998A&AS..129..431H. doi: 10.1051/aas:1998195 .
  4. ↑ Kovtyukh, V. V.; et al. (2004). "A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence". Astronomy and Astrophysics. 427 (3): 933–936. arXiv: astro-ph/0409753 . Bibcode:2004A&A...427..933K. doi:10.1051/0004-6361:20041449. S2CID   204935981.
  5. 1 2 3 4 5 Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv: 1306.2974 , Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID   14911430, 40. See Table 3.
  6. ↑ Luck, R. Earle; Heiter, Ulrike (2006). "Dwarfs in the Local Region". The Astronomical Journal. 131 (6): 3069–3092. Bibcode:2006AJ....131.3069L. doi: 10.1086/504080 .
  7. 1 2 3 4 Beichman, C. A.; et al. (2006). "New Debris Disks Around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets". The Astrophysical Journal. 652 (2): 1674–1693. arXiv: astro-ph/0611682 . Bibcode:2006ApJ...652.1674B. doi:10.1086/508449. S2CID   14207148.
  8. 1 2 Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv: 1611.02897 , Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, S2CID   119511744, 21.
  9. 1 2 "LHS 3287". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-14.
  10. ↑ Bailer-Jones, C. A. L. (January 2018), "The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release", Astronomy & Astrophysics, 609: 16, arXiv: 1708.08595 , Bibcode:2018A&A...609A...8B, doi:10.1051/0004-6361/201731453, S2CID   119462489, A8
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