HD 165185

Last updated
HD 165185
Observation data
Epoch J2000       Equinox J2000
Constellation Sagittarius
Right ascension 18h 06m 23.720s [1]
Declination –36° 01′ 11.23″ [1]
Apparent magnitude  (V)5.94 [2]
Characteristics
Spectral type G1 V [2]
U−B color index 0.07 [3]
B−V color index 0.61 [3]
Astrometry
Radial velocity (Rv)+15.4 [2]  km/s
Proper motion (μ)RA: +106.020  mas/yr [1]
Dec.: +8.812  mas/yr [1]
Parallax (π)58.4296 ± 0.0404  mas [1]
Distance 55.82 ± 0.04  ly
(17.11 ± 0.01  pc)
Absolute magnitude  (MV)+4.59 [4]
Details
Mass 1.13 [5]   M☉
Radius 0.94 [6]   R☉
Luminosity (bolometric)1.15 [7]   L☉
Surface gravity (log g)4.46±0.06 [8]   cgs
Temperature 5,940±18 [8]   K
Metallicity [Fe/H]−0.05±0.03 [8]   dex
Rotation 5.90 [6]  days
Rotational velocity (v sin i)7.53 [8]  km/s
Age 437±186 [5]   Myr
Other designations
29 G. Sgr [9] , CD−36°12214, GJ  702.1, HD  165185, HIP  88694, HR  6748, SAO  209710, WDS J18064-3601A [10]
Database references
SIMBAD data
ARICNS data

HD 165185 is the Henry Draper Catalogue designation for a star in the southern zodiac constellation of Sagittarius. It has an apparent visual magnitude of 5.94, [2] which indicates it is a sixth magnitude star that is faintly visible to the naked eye. (According to the Bortle scale, it can be viewed from dark suburban skies.) Parallax measurements give an estimated distance of 55.8  light years from the Sun. [1] It is drifting further away with a heliocentric radial velocity of +15.4 km/s. [2]

This star is a pre-main-sequence [11] solar analog [12] with a stellar classification of G1 V. [2] It is spinning with a projected rotational velocity of 7.53 km/s [8] and a rotation period of 5.9 days. [6] Measurements of magnetic activity in the chromosphere show variations over time, much like the sunspot cycle. This activity showed a distinct peak in 2009. [13] Stellar models give an estimated mass equal to 1.13 [5] times the mass of the Sun, but only 94% [6] of the Sun's radius. The total, or bolometric luminosity of the star is 15% higher than the Sun, [7] while the abundance of elements other than hydrogen and helium—what astronomer's term the metallicity—is nearly the same as in the Sun. [8] The stellar atmosphere has an effective temperature of 5,940 [8]  K, giving it the yellow-hued glow of a G-type star. [14]

HD 165185 completed its perihelion passage some 851,000 years ago when it came within 29 ly (8.9 pc) of the Sun, [15] and it is now moving away with a radial velocity component of 15.4 km/s. [2] Based upon the motion of this star through space, its age, and properties, this star is a probable member of the Ursa Major Moving Group; a stellar kinematic group that formed in the same region of space. [11] It has a suspected common proper motion companion at an angular separation of 12″, corresponding to a projected separation of 220  AU. This is a red dwarf star with a stellar classification of M0 and an infrared K band magnitude of 8.11. [16]

Related Research Articles

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<span class="mw-page-title-main">Tau Virginis</span> Single star in the constellation Virgo

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<span class="mw-page-title-main">53 Aquarii</span> Binary star in the constellation Aquarius

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94 Ceti is a trinary star system approximately 73 light-years away in the constellation Cetus.

Xi2 Capricorni (ξ2 Capricorni) is a yellow-white hued star in the southern constellation of Capricornus. It is dimly visible to the naked eye on a dark night, having an apparent visual magnitude of +5.83. Based upon an annual parallax shift of 36.10 mas as seen from Earth, this system is located 90 light years from the Sun.

20 Leonis Minoris is a binary star system in the northern constellation of Leo Minor. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.4. Based upon an annual parallax shift of 66.46 mas, it is located 49 light years from the Sun. The star has a relatively high proper motion and is moving away from the Sun with a radial velocity of +56 km/s. The system made its closest approach about 150,000 years ago when it came within 32.2 ly (9.86 pc).

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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.

GJ 3379 is the nearest star in the Orion constellation, located at a distance of 17 light years from the Sun based on parallax. It is a single star with an apparent visual magnitude of +11.31 and an absolute magnitude of +12.71, therefore, the star is not visible with the naked eye. It is positioned in the upper left part of the Orion constellation, to the SSE of Betelgeuse. This star is drifting further away with a radial velocity of +30.0 kilometers per second. In the past, this star had a relatively close encounter with the Solar System. Some 161,000±6,000 years ago, it achieved a minimum distance of 4.08 ± 0.20 ly (1.25 ± 0.06 pc).

Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.

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> G-type star in the constellation Cetus

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HD 189245 is the Henry Draper catalogue designation for a solitary star in the southern constellation of Sagittarius. It has an apparent visual magnitude of 5.66, which means it is faintly visible to the naked eye. Parallax measurements from the Hipparcos satellite indicate a distance of 72 light years from the Sun. It is drifting closer with a heliocentric radial velocity of −13 km/s.

HD 168009 is a star in the northern constellation of Lyra. It has an apparent visual magnitude of 6.3, placing it just above to below the normal limit of stars visible to the naked eye under good viewing conditions of 6-6.5. An annual parallax shift of 42.93 mas provides a distance estimate of 76 light years. It is moving closer to the Sun with a heliocentric radial velocity of −65 km/s. In about 328,000 years from now, the star will make its closest approach at a distance of around 17 ly (5.1 pc).

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

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. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 Torres, C. A. O.; et al. (December 2006). "Search for associations containing young stars (SACY). I. Sample and searching method". Astronomy and Astrophysics . 460 (3): 695–708. arXiv: astro-ph/0609258 . Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. S2CID   16080025.
  3. 1 2 Stobie, R. S. (1970), "Photometry of bright southern cepheids", Monthly Notices of the Royal Astronomical Society, 148: 1–15, Bibcode:1970MNRAS.148....1S, doi: 10.1093/mnras/148.1.1 .
  4. ↑ Eggen, Olin J. (August 1998), "The Sirius Supercluster and Missing Mass near the Sun", The Astronomical Journal, 116 (2): 782–788, Bibcode:1998AJ....116..782E, doi: 10.1086/300465 .
  5. 1 2 3 Plavchan, Peter; et al. (June 2009), "New Debris Disks Around Young, Low-Mass Stars Discovered with the Spitzer Space Telescope", The Astrophysical Journal, 698 (2): 1068–1094, arXiv: 0904.0819 , Bibcode:2009ApJ...698.1068P, doi:10.1088/0004-637X/698/2/1068, S2CID   51417657.
  6. 1 2 3 4 Linsky, Jeffrey L.; et al. (July 2012), "Ultraviolet Spectroscopy of Rapidly Rotating Solar-Mass Stars: Emission-line Redshifts as a Test of the Solar-Stellar Connection", The Astrophysical Journal, 754 (1): 14, arXiv: 1205.6498 , Bibcode:2012ApJ...754...69L, doi:10.1088/0004-637X/754/1/69, S2CID   119205513, 69.
  7. 1 2 Léger, Alain; et al. (August 2015), "Impact of ηEarth on the Capabilities of Affordable Space Missions to Detect Biosignatures on Extrasolar Planets", The Astrophysical Journal, 808 (2): 19, arXiv: 1504.08232 , Bibcode:2015ApJ...808..194L, doi:10.1088/0004-637X/808/2/194, S2CID   55000780, 194.
  8. 1 2 3 4 5 6 7 Tsantaki, M.; et al. (October 2014), "Spectroscopic parameters for solar-type stars with moderate-to-high rotation. New parameters for ten planet hosts", Astronomy & Astrophysics, 570: 14, arXiv: 1407.6765 , Bibcode:2014A&A...570A..80T, doi:10.1051/0004-6361/201424257, S2CID   118833879, A80.
  9. ↑ B. A., Gould (1879), Resultados del Observatorio Nacional Argentino en Cordoba, vol. 1, retrieved 2016-04-05.
  10. ↑ "HD 165185 -- Pre-main sequence Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg.
  11. 1 2 Nakajima, Tadashi; Morino, Jun-Ichi (January 2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal, 143 (1): 2, Bibcode:2012AJ....143....2N, doi: 10.1088/0004-6256/143/1/2 .
  12. ↑ Gaidos, Eric J.; Gonzalez, Guillermo (July 2002), "Stellar atmospheres of nearby young solar analogs", New Astronomy, 7 (5): 211–226, arXiv: astro-ph/0203518 , Bibcode:2002NewA....7..211G, doi:10.1016/S1384-1076(02)00108-2, S2CID   40662059.
  13. ↑ Metcalfe, T. S.; et al. (September 2009), "Activity Cycles of Southern Asteroseismic Targets", Proceedings of the "Solar Analogs II" workshop, arXiv: 0909.5464 , Bibcode:2009arXiv0909.5464M.
  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. ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv: 1412.3648 , Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID   59039482, A35.
  16. ↑ Chini, R.; et al. (January 2014), "New visual companions of solar-type stars within 25 pc", Monthly Notices of the Royal Astronomical Society, 437 (1): 879–886, arXiv: 1310.2684 , Bibcode:2014MNRAS.437..879C, doi:10.1093/mnras/stt1953, S2CID   118717758.
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