52 Sagittarii

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52 Sagittarii
Sagittarius constellation map.svg
Red circle.svg
Location of 52 Sagittarii (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Sagittarius
Right ascension 19h 36m 42.43288s [1]
Declination −24° 53′ 01.0288″ [1]
Apparent magnitude  (V)4.59 [2] + 9.2
Characteristics
Evolutionary stage main sequence [3]
Spectral type B8/9V [4] + K2–4V
U−B color index −0.15 [5]
B−V color index −0.06 [5]
Astrometry
Radial velocity (Rv)−19.00 [6]  km/s
Proper motion (μ)RA: +68.30 [1]   mas/yr
Dec.: −21.51 [1]   mas/yr
Parallax (π)17.20 ± 0.23  mas [1]
Distance 190 ± 3  ly
(58.1 ± 0.8  pc)
Absolute magnitude  (MV)0.77 [2]
Details
52 Sgr A
Mass 3.0±0.1 [7]   M☉
Radius 2.1 [8]   R☉
Luminosity 60.5+1.9
−1.8 [3]   L☉
Surface gravity (log g)4.19 [9]   cgs
Temperature 10,592+74
−72 [3]   K
Metallicity [Fe/H]0.00 [10]   dex
Rotational velocity (v sin i)48 [3]  km/s
Age 57.3±11.7 [7]   Myr
Other designations
h2 Sgr, 52 Sgr, NSV  12191, CD−25°14184, GC  27089, HD  184707, HIP  96465, HR  7440, SAO  188337, CCDM J19367-2453AB, WDS J19367-2453AB, GSC  06893-02132 [11]
Database references
SIMBAD data

52 Sagittarii is a binary star [12] system in the southern constellation of Sagittarius. It has the Bayer designation h2 Sagittarii, while 52 Sagittarii is the Flamsteed designation. This system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.59. [2] It is located approximately 190 light years away based on parallax, [1] but is drifting closer with a radial velocity of −19 km/s. [6]

The primary component is a B-type main-sequence star with a stellar classification of B8/9V. [4] Garrison and Gray (1994) assigned it a class of kB8 hB9 HeA0 Va (Sr Fe II), [13] displaying the calcium K line of a B8 class star, the hydrogen lines of a B9 star, and the helium lines of an A0 star, along with overabundances of strontium and iron. It is around 57 [7] million years old with three [7] times the mass of the Sun and about 2.1 [8] times the Sun's radius. It is radiating 60.5 [3] times the luminosity of the Sun from its photosphere at an effective temperature of 10,592 K. [3] The star is spinning with a projected rotational velocity of 48 km/s. [3]

52 Sagittarii has one companion at an angular separation of 2.4″ . This object is magnitude 9.2 with a spectral class in the K2V-K4V range, and is believed to be the source of X-ray emissions from the system. [14] [15]

Related Research Articles

Rho<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Rho1 Sagittarii, Latinized from ρ1 Sagittarii, is a single, variable star in the southern constellation of Sagittarius. It has a white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 3.93. The distance to this star is approximately 127 light years based on parallax, and it is drifting further away with a radial velocity of +1.2 km/s. It is positioned near the ecliptic and so it can be occulted by the Moon.

Theta<sup>2</sup> Sagittarii A-type subgiant star in the constellation Sagittarius

Theta2 Sagittarii, Latinized from θ2 Sagittarii, is a solitary star in the zodiac constellation of Sagittarius. It is faintly visible to the naked eye with an apparent visual magnitude of +5.30. The star is progressing in the general direction of the Sun with a radial velocity of −17.60 km/s. Based upon an annual parallax shift of 20.62 mas as seen from Earth, it is located around 158 light years from the Sun. The star is drifting closer with a radial velocity of −17.6 km/s.

<span class="mw-page-title-main">Nu Tauri</span> Single A-type main sequence star in the constellation Taurus

ν Tauri, Latinized as Nu Tauri, is a single star in the zodiac constellation of Taurus. It is a white-hued star and is visible to the naked eye with an apparent visual magnitude of +3.91. This object is located 117 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −6 km/s. It is predicted to come to within roughly 18.4 ly of the Sun in around five million years.

<span class="mw-page-title-main">Iota Tauri</span> Double star in the constellation Taurus

Iota Tauri, Latinized from ι Tauri, is a white-hued star in the zodiac constellation Taurus and an outlying member of the Hyades star cluster. It is visible to the naked eye with an apparent visual magnitude of 4.62, and is located at an estimated distance of about 173 light years based upon parallax measurements. The star is moving away from the Sun with a radial velocity of +38 km/s.

<span class="mw-page-title-main">72 Ophiuchi</span> Star in the constellation Ophiuchus

72 Ophiuchi is a binary star system in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint, white-hued point of light with a combined apparent visual magnitude of 3.73. It is located approximately 86.9 light years away from the Sun based on parallax, but is moving closer with a heliocentric radial velocity of -23.9 km/s.

<span class="mw-page-title-main">Epsilon Hydri</span> Star in the constellation Hydrus

Epsilon Hydri, Latinized from ε Hydri, is a single, blue-white hued star in the southern constellation of Hydrus. It is a faint star with an apparent visual magnitude of 4.12, but it can be seen with the naked eye. Measurements made by the Hipparcos spacecraft showed an annual parallax shift of 21.48 mas, which provides a distance estimate of 152 light years. The star is moving away from the Sun with a radial velocity of +13.6 km/s. It is a member of the Tucana-Horologium moving group, an association of stars that share a common motion through space.

<span class="mw-page-title-main">Theta Indi</span> Star in the constellation Indus

Theta Indi is a binary star in the constellation Indus. Its apparent magnitude is 4.40 and it is approximately 98.8 light years away based on parallax. The smaller companion, B, has a spectral type of G0V and an apparent magnitude of 7.18 at a separation of 6.71". Recent observations suggest the primary is itself a binary with components Aa and Ab orbiting at 0.0617", estimated period about 1.3 years.

<span class="mw-page-title-main">Epsilon Microscopii</span> Star in the constellation Microscopium

Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 km/s.

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

Beta Octantis, Latinized from β Octantis, is a probable astrometric binary star system in the southern circumpolar constellation of Octans. It is faintly visible to the naked eye with an apparent visual magnitude of 4.13. Based upon an annual parallax shift of 21.85 mas as seen from Earth, it is located about 149 light years from the Sun. It is moving away from the Sun with a radial velocity of +19 km/s.

<span class="mw-page-title-main">32 Orionis</span> Triple star system in the constellation Orion

32 Orionis is a triple star system in the equatorial constellation of Orion. It has the Bayer designation A Orionis, while 32 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.20. It is located approximately 303 light-years away from the Sun based on parallax, and is drifting further away with a radial velocity of +18.6 km/s.

<span class="mw-page-title-main">Epsilon Pavonis</span> Single white-hued star in the constellation Pavo

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<span class="mw-page-title-main">58 Persei</span> Multiple-star system in the constellation of Perseus

58 Persei is a binary and possibly a triple star system in the northern constellation of Perseus. It has the Bayer designation e Persei, while 58 Persei is the Flamsteed designation. This system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.26. It is approximately 800 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s.

<span class="mw-page-title-main">34 Persei</span> Star in the constellation Perseus

34 Persei is a binary star system in the northern constellation of Perseus. It is visible to the naked eye as a faint, blue-white hued point of light with a combined apparent visual magnitude of 4.67. The system is located approximately 540 light years away from the Sun based on parallax, but it is drifting closer with a radial velocity of −3.5 km/s. It is a likely member of the Alpha Persei Cluster.

<span class="mw-page-title-main">40 Persei</span> Star in the constellation Perseus

40 Persei is a wide binary star system in the northern constellation of Perseus. It has the Bayer designation ο Persei, while 40 Persei is the Flamsteed designation. The system is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude of 4.97. It is located approximately 1060 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s. The system is a member of the Perseus OB2 association of co-moving stars.

<span class="mw-page-title-main">29 Persei</span> B-type main sequence star in the constellation Perseus

29 Persei is a single star in the northern constellation of Perseus, located approximately 640 light years away from the Sun based on parallax. It is visible to the naked eye as faint, blue-white hued star with an apparent visual magnitude of 5.16. This object is a member of the Alpha Persei Cluster.

<span class="mw-page-title-main">HD 167818</span> Star in the constellation Sagittarius

HD 167818 is a class K3II star in the constellation Sagittarius. Its apparent magnitude is 4.66 and it is approximately 760 light years away based on parallax.

<span class="mw-page-title-main">21 Sagittarii</span> Star in the constellation Sagittarius

21 Sagittarii is a binary star system in the southern zodiac constellation of Sagittarius. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.81. The system is located approximately 410 light years away from the Sun based on parallax. It is moving closer to the Earth with a heliocentric radial velocity of −11.80 km/s.

56 Sagittarii is a single star in the southern constellation of Sagittarius. It has the Bayer designation f Sagittarii, while 56 Sagittarii is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.87. It is located approximately 208 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.

<span class="mw-page-title-main">43 Persei</span> Spectroscopic binary star system in the constellation Perseus

43 Persei is a binary star system in the northern constellation Perseus. It is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.28. The system is located around 38.5 parsecs (125.4 ly) distant from the Sun, based on parallax.

<span class="mw-page-title-main">41 Leonis Minoris</span> Star in the constellation Leo Minor

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References

  1. 1 2 3 4 5 6 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600. Vizier catalog entry
  2. 1 2 3 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. Vizier catalog entry
  3. 1 2 3 4 5 6 7 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars". Astronomy & Astrophysics. 537: A120. arXiv: 1201.2052 . Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID   55586789. Vizier catalog entry
  4. 1 2 Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  5. 1 2 Mallama, A. (2014). "Sloan Magnitudes for the Brightest Stars". The Journal of the American Association of Variable Star Observers. 42 (2): 443. Bibcode:2014JAVSO..42..443M. Vizier catalog entry
  6. 1 2 Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. LCCN   54001336.
  7. 1 2 3 4 Tetzlaff, N.; et al. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID   118629873. Vizier catalog entry
  8. 1 2 Allende Prieto, C.; Lambert, D. L. (1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures". Astronomy and Astrophysics. 352: 555–562. arXiv: astro-ph/9911002 . Bibcode:1999A&A...352..555A. Vizier catalog entry
  9. ↑ David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID   33401607. Vizier catalog entry
  10. ↑ Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv: 1606.08814 . Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID   118345778. Vizier catalog entry
  11. ↑ "h02 Sgr". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-07-27.
  12. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  13. ↑ Garrison, R. F.; Gray, R. O. (1994). "The late B-type stars: Refined MK classification, confrontation with stromgren photometry, and the effects of rotation". The Astronomical Journal. 107: 1556. Bibcode:1994AJ....107.1556G. doi:10.1086/116967. Garrison has note: "Balmer shell cores?"
  14. ↑ Hubrig, S.; et al. (2007). "Establishing the nature of companion candidates to X-ray-emitting late B-type stars". Monthly Notices of the Royal Astronomical Society. 381 (4): 1569. arXiv: 0708.0860 . Bibcode:2007MNRAS.381.1569H. doi:10.1111/j.1365-2966.2007.12325.x. S2CID   15143368.
  15. ↑ Mason, Brian D.; et al. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 . Vizier catalog entry
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