43 Sagittarii

Last updated
43 Sagittarii
Sagittarius constellation map.svg
Red circle.svg
Location of 43 Sagittarii (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Sagittarius
Right ascension 19h 17m 38.07906s [1]
Declination −18° 57′ 10.4626″ [1]
Apparent magnitude  (V)4.88 [2]
Characteristics
Spectral type G8II-III [3]
U−B color index +0.81 [4]
B−V color index +1.02 [4]
Astrometry
Radial velocity (Rv)+15.20 [5]  km/s
Proper motion (μ)RA: −10.341 [1]   mas/yr
Dec.: −10.892 [1]   mas/yr
Parallax (π)6.9681 ± 0.1875 [1]   mas
Distance 470 ± 10  ly
(144 ± 4  pc)
Absolute magnitude  (MV)-0.96 [2]
Details [6]
Mass 3.30  M☉
Radius 23.99  R☉
Luminosity 277  L☉
Surface gravity (log g)2.22  cgs
Temperature 4,813  K
Metallicity [Fe/H]−0.18  dex
Rotational velocity (v sin i)4.2 [7]  km/s
Age 350±100 [8]   Myr
Other designations
d Sgr, 43 Sgr, BD−19°5379, GC  26589, HD  180540, HIP  94820, HR  7304, SAO  162413, GSC  06304-00334 [9]
Database references
SIMBAD data

43 Sagittarii is a single [10] star in the southern constellation of Sagittarius. It has the Bayer designation d Sagittarii, while 43 Sagittarii is the Flamsteed designation. [9] This object is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.88. [2] From parallax measurements, it is estimated to lie around 470  light years away from the Sun. [1] The star is drifting further from the Earth with a heliocentric radial velocity of +15.2 km/s. [5] It is located near the ecliptic and thus is subject to lunar occultations. [11]

This is an aging giant/bright giant star with a stellar classification of G8II-III, [3] and is most likely (97% chance) on the horizontal branch. [8] It is around 350 [8]  million years old with 3.3 [6] times the mass of the Sun. Having exhausted the supply of hydrogen at its core, the star has expanded to 24 [6] times the Sun's radius and is now generating energy through core helium fusion. It is radiating 277 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,813 K. [6]

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.

Iota Sculptoris

ι Sculptoris, Latinized as Iota Sculptoris and abbreviated iot Scl, is a solitary star in the southern constellation of Sculptor. It is visible to the naked eye as a dim, orange-hued point of light with an apparent visual magnitude of 5.18. The star is located approximately 336 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +21 km/s.

Mu Sculptoris Star in the constellation Sculptor

μ Sculptoris, Latinized as Mu Sculptoris, is a solitary, orange-hued star in the southern constellation of Sculptor. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.30. This star is located approximately 291 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +16 km/s.

4 Sagittarii

4 Sagittarii is a suspected astrometric binary star system in the zodiac constellation of Sagittarius, located approximately 390 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.74, The system is moving closer to the Earth with a heliocentric radial velocity of −18 km/s.

HR 6801 Star in the constellation Sagittarius

HR 6801 is a single star in the southern zodiac constellation of Sagittarius. It was designated as 1 Sagittarii by Flamsteed, but is now often referred to as 11 Sagittarii. Flamsteed's 11 Sgr actually refers to a different, much fainter star. The object is orange in hue and is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.96. The distance to this star is approximately 258 light years based on stellar parallax, and it is drifting further away with a radial velocity of +6 km/s.

10 Leonis Minoris

10 Leonis Minoris is a single, variable star in the northern constellation Leo Minor, located approximately 180 light years away based on parallax. It has the variable star designation SU Leonis Minoris; 10 Leonis Minoris is the Flamsteed designation. This body is visible to the naked eye as a faint, orange-hued star with a baseline apparent visual magnitude of 4.54. It is moving closer to the Earth with a heliocentric radial velocity of −12 km/s.

18 Monocerotis

18 Monocerotis is a binary star system located about half way from Orion's Belt to Procyon, in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.47, and is positioned around 370 light years away from the Sun based on parallax. The system is receding from the Earth with a heliocentric radial velocity of +11 km/s.

28 Monocerotis is a single star in the equatorial constellation of Monoceros. It has an orange-hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.69. The distance to this star is approximately 450 light years based on parallax, and it has an absolute magnitude of −1.00. The star is drifting further away from the Sun with a radial velocity of +26.7 km/s.

17 Monocerotis

17 Monocerotis is a single star located around 490 light years away from the Sun in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.77. The star is moving away from the Earth with a heliocentric radial velocity of +46 km/s.

3 Monocerotis

3 Monocerotis is a binary star system in the equatorial constellation of Monoceros, located approximately 780 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.92. The system is moving further from the Earth with a heliocentric radial velocity of +39 km/s.

27 Monocerotis is a single star located about 318 light years away from the Sun star in the equatorial constellation of Monoceros. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.93. The star is advancing toward the Earth with a heliocentric radial velocity of −28 km/s.

71 Ophiuchi star in the constellation of Ophiuchus

71 Ophiuchi is a single star in the equatorial constellation of Ophiuchus. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.64. The star is located approximately 273 light years away from the Sun based on parallax, and is moving closer with a radial velocity of −3 km/s.

24 Scorpii

24 Scorpii is a star that was originally placed by John Flamsteed within the constellation of Scorpius but in now placed within the southeastern constellation of Ophiuchus. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.91. Based on the trigonometric parallax published in Gaia Data Release 2, the star lies approximately 121 parsecs or 390 light years away. It is positioned near the ecliptic and thus is subject to lunar occultations.

31 Orionis

31 Orionis is a binary star system in the equatorial constellation of Orion, located near the bright star Mintaka. It is visible to the naked eye as a faint, orange-hued point of light with a baseline apparent visual magnitude of 4.71. The distance to this system is approximately 490 light years away based on parallax, and it is drifting further away with a mean radial velocity of +6 km/s.

51 Orionis Star in the constellation of Orion

51 Orionis is a single star in the equatorial constellation of Orion. It has the Bayer designation b Orionis, while 51 Orionis is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.90. It is located approximately 299 light years away from the Sun based on parallax, and is drifting further away with a radial velocity of +88 km/s.

Pi Pavonis

π Pavonis, Latinized as Pi Pavonis, is a candidate astrometric binary star system in the constellation Pavo. It is a white-hued star that is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.33. The distance to this object is 130 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −15.6 km/s.

Xi Pavonis

ξ Pavonis, Latinized as Xi Pavonis, is a triple star system in the southern constellation of Pavo. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 4.35 The system is located approximately 440 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s.

54 Persei Star in the constellation Perseus

54 Persei is a single star in the northern constellation of Perseus. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.93. The star is located approximately 220 light years away based on parallax, but is drifting closer with a radial velocity of −27 km/s.

24 Persei

24 Persei is a star in the northern constellation of Perseus, located around 337 light years from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.94. The object is moving closer to the Earth with a heliocentric radial velocity of −37 km/s.

Lambda Octantis

λ Octantis, Latinized as Lambda Octantis, is a binary star system in the southern circumpolar constellation of Octans. It is visible to the naked eye as a dim point of light with a combined apparent visual magnitude of 5.27. The distance to this system is approximately 398–409 light years, based on parallax, but it is moving closer with a radial velocity of −10 km/s.

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 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 Hoffleit, D.; Warren, W. H. (1995). "Bright Star Catalogue". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H (5th Revised ed.). 5050. Bibcode:1995yCat.5050....0H.
  4. 1 2 Mermilliod, J. C. (2006). "Homogeneous Means in the UBV System (Mermilliod 1991)". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie. 2168. Bibcode:2006yCat.2168....0M. Vizier catalog entry
  5. 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. ISBN   9780598216885. LCCN   54001336.
  6. 1 2 3 4 Reffert, Sabine; et al. (2015). "Precise radial velocities of giant stars". Astronomy & Astrophysics. 574: A116. arXiv: 1412.4634 . Bibcode:2015A&A...574A.116R. doi:10.1051/0004-6361/201322360. hdl:10722/215277. S2CID   59334290. Vizier catalog entry
  7. ↑ De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (2014). "A catalog of rotational and radial velocities for evolved stars". Astronomy & Astrophysics. 561: A126. arXiv: 1312.3474 . Bibcode:2014A&A...561A.126D. doi:10.1051/0004-6361/201220762. S2CID   54046583. Vizier catalog entry
  8. 1 2 3 Stock, Stephan; et al. (August 2018), "Precise radial velocities of giant stars. X. Bayesian stellar parameters and evolutionary stages for 372 giant stars from the Lick planet search", Astronomy & Astrophysics, 616: 15, arXiv: 1805.04094 , Bibcode:2018A&A...616A..33S, doi:10.1051/0004-6361/201833111, S2CID   119361866, A33.
  9. 1 2 "d Sgr". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-07-22.
  10. ↑ 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.
  11. ↑ Richichi, A.; et al. (May 1996). "New binary stars discovered by lunar occultations. II". Astronomy and Astrophysics. 309: 163–170. Bibcode:1996A&A...309..163R.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.