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]

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<span class="mw-page-title-main">Theta Boötis</span> Star in the northern constellation of Boötes

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Lambda<sup>2</sup> Fornacis Binary star system in the constellation Fornax

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HIP 12961 is a star with an exoplanetary companion in the equatorial constellation of Eridanus. It is too faint to be visible to the naked eye, with an apparent visual magnitude of 10.24. The distance to this system can be estimated from its parallax measurements, which yield a separation of 76.4 light-years from the Sun. It is receding with a radial velocity of +33 km/s and has a high proper motion, traversing the celestial sphere at an angular rate of 0.300″ yr−1.

HD 93385 is a star in the southern constellation of Vela. At an apparent visual magnitude of 7.5, it is too faint to be seen with the unaided eye. Parallax measurements made using the Gaia spacecraft show an annual shift of 23.15 mas. This is equivalent to a physical separation of around 141 light years from the Sun. It is drifting further away with a radial velocity of +47.8 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.

c Ursae Majoris is the Bayer designation for a double-lined spectroscopic binary star system in the northern constellation of Ursa Major. It has an apparent visual magnitude of 5.18, which indicates that is visible to the naked eye. Parallax measurements yield an estimated distance of 66 light years from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of −14 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).

<span class="mw-page-title-main">HD 111395</span> Star in the constellation Coma Berenices

HD 111395 is a single, variable star in the northern constellation of Coma Berenices. It has the variable star designation LW Com, short for LW Comae Berenices; HD 111395 is the Henry Draper Catalogue designation. The star has a yellow hue and is just bright enough to be barely visible to the naked eye with an apparent visual magnitude that fluctuates around 6.29. Based upon parallax measurements, it is located at a distance of 55.8 light years from the Sun. The star is drifting closer with a radial velocity of −8.9 km/s. It is a member of the Eta Chamaeleontis stellar kinematic group.

HAT-P-15 is a G-type main-sequence star about 630 light-years away. The star is older than Sun yet has a concentration of heavy elements roughly 190% of solar abundance. The star has no noticeable starspot activity.

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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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