HD 178322

Last updated
HD 178322
Corona Australis constellation map.svg
Red circle.svg
Location of HD 178322 (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Corona Australis
Right ascension 19h 09m 57.65200s [1]
Declination −41° 53′ 32.0836″ [1]
Apparent magnitude  (V)5.86±0.01 [2]
Characteristics
Spectral type B5 V + B6 V [3]
U−B color index −0.49 [4]
B−V color index −0.08 [4]
Variable type suspected [5]
Astrometry
Radial velocity (Rv)13.3±2 [6]  km/s
Proper motion (μ)RA: −0.360  mas/yr [1]
Dec.: −10.096  mas/yr [1]
Parallax (π)2.104 ± 0.1145  mas [1]
Distance 1,550 ± 80  ly
(480 ± 30  pc)
Absolute magnitude  (MV)−2.31 [7] (combined)
Orbit [8]
PrimaryA
CompanionB
Period (P)12.4700  d
Semi-major axis (a)0.235  AU [9]
Eccentricity (e)0.05
Inclination (i)71.19°
Periastron epoch (T)2,438,237.4500  JD
Argument of periastron (ω)
(secondary)		199.1 [10] °
Argument of periastron (ω)
(primary)		19.10 [10] °
Semi-amplitude (K1)
(primary)		79.70 km/s
Semi-amplitude (K2)
(secondary)		78.90 km/s
Details
Age 50.1±8.4 [11]   Myr
A
Mass 4.39 [10]   M☉
Radius 3.26 [9]   R☉
Luminosity 11,749 [12]   L☉
Temperature 15,488 [12]   K
Rotational velocity (v sin i)45 [9]  km/s
B
Mass 4.35 [10]   M☉
Radius 3.07 [9]   R☉
Luminosity513 [12]   L☉
Temperature 14,454 [12]   K
Rotational velocity (v sin i)45±7 [9]  km/s
Other designations
45 G. Coronae Australis [13] , CD−42°13933, CPD−42°8616, GC  26375, HD  178322, HIP  94157, HR  7257, SAO  229531 [14]
Database references
SIMBAD data

HD 178322, also known as HR 7257 or rarely 45 G. Coronae Australis, is a double-lined spectroscopic binary located in the southern constellation Corona Australis. It has a combined apparent magnitude of 5.86, [2] making it faintly visible to the naked eye under ideal conditions. The system is located relatively far at a distance of roughly 1,550 light-years based on Gaia DR3 parallax measurements, [1] and it is currently receding with a heliocentric radial velocity of 13.3  km/s . [6] At its current distance, HD 178322's brightness is diminished by an extinction of 0.28 magnitudes [15] and it has an absolute magnitude of −2.31. [7] The system has a high peculiar velocity of 28.9+4.1
−7.9  km/s , [11] indicating that it may be a runaway star system; it is said to be part of the Scorpius-Centaurus Association. [16]

The components of HD 178322 are both B-type main-sequence stars with stellar classifications of B5 V and B6 V respectively. [3] Both stars have roughly 4.4 times the mass of the Sun [10] and they spin moderately with projected rotational velocities of 45  km/s . [9] The primary has 3.26 times the radius of the Sun [9] and it radiates 11,749 times the luminosity of the Sun [12] from its photosphere at an effective temperature of 15,488  K . The companion has 3.07 times the Sun's girth [9] and it radiates 513 times the luminosity of the Sun [12] from its photosphere at an effective temperature of 14,454  K . [12] Both stars take roughly 12 days to complete a relatively circular orbit [8] at a separation of 0.235  AU . [9] The system is estimated to be 50 million years old. [11]

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Kappa<sup>2</sup> Coronae Australis Star in the constellation Corona Australis

Kappa2 Coronae Australis, Latinized from κ2 Coronae Australis, is the primary of a probable binary system located in the southern constellation Corona Australis. It is visible to the naked eye as a bluish-white hued star with an apparent visual magnitude of 5.59. The distance to this star is roughly 710 light years based on Gaia DR3 parallax measurements. The radial velocity is poorly constrained, but the star appears to be moving closer with a radial velocity of around −15 km/s. At its current distance, Kappa2 CrA's brightness is diminished by 0.45 magnitudes due to interstellar dust.

<span class="mw-page-title-main">N Scorpii</span> Star in the constellation of Scorpius

N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.

<span class="mw-page-title-main">HD 138289</span> Star in the constellation Apus

HD 138289, also known as HR 5757, is a probable spectroscopic binary located in the constellation Apus, the bird-of-paradise. It has an apparent magnitude of 6.18, placing it near the limit for naked eye. Gaia DR3 parallax measurements place the object 359 light years away and it is currently receding with a heliocentric radial velocity of 13.1 km/s. At its current distance, HD 138289's brightness is diminished by 0.25 magnitudes due to extinction from interstellar dust. It has an absolute magnitude of +1.21.

<span class="mw-page-title-main">HD 72922</span> Star in the constellation Chamaleon

HD 72922, also known as HR 3393, is a suspected astrometric binary located in the southern circumpolar constellation Chamaeleon. A 1993 paper by Olin J. Eggen lists it as a member of the Milky Way's old disk population.

<span class="mw-page-title-main">HD 57197</span> Star in the constellation Puppis

HD 57197, also known as M Puppis or HR 2789, is a suspected astrometric binary located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 5.84, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, the system is estimated to be 629 light years away from the Solar System. The value is poorly constrained, but it appears to be receding with a heliocentric radial velocity of 13 km/s. At its current distance, HD 57197's brightness is diminished by 0.3 magnitudes due to interstellar dust. It has an absolute magnitude of -0.43.

HD 72337, also known as HR 3370, is a solitary, bluish-white hued star located in the southern constellation Volans. With an apparent magnitude of 5.51, it is faintly visible to the unaided eye but only under ideal conditions.

HD 23277 is a spectroscopic binary located in the northern circumpolar constellation Camelopardalis. With a combined apparent magnitude of 5.39, it is faintly visible to the naked eye under ideal conditions. This star is located at a distance of 372 light years, but is drifting away at a rate of 17 km/s.

<span class="mw-page-title-main">14 Trianguli</span> Star in the constellation Triangulum

14 Trianguli, also known as HD 15656, is a spectroscopic binary located in the northern constellation Triangulum. It has an apparent magnitude of 5.14, making it faintly visible to the naked eye in ideal conditions. Gaia DR3 parallax measurements place the system 433 light years away, and it is currently approaching the Solar System with a heliocentric radial velocity of −37 km/s. At its current distance, 14 Tri's brightness is diminished by 0.21 magnitude due to interstellar dust. It has an absolute magnitude of −0.46.

HD 170069 is a solitary star in the southern constellation Telescopium. It has an apparent magnitude of 5.68, allowing it to be faintly seen with the naked eye. The star is located at a distance of 590 light years but is approaching closer with a heliocentric radial velocity of −18 km/s. HD 170069 was designated as Tau Telescopii before Benjamin Apthorp Gould dropped the title.

HD 10800, also known as HR 512 or Gliese 67.1, is a triple star located in the southern circumpolar constellation Octans. It has a combined apparent magnitude of 5.87, allowing it to be faintly seen with the naked eye. The system is relatively close at a distance of 88.1 light years but is drifting closer with a heliocentric radial velocity −1.1 km/s.

<span class="mw-page-title-main">AF Columbae</span> Star in the constellation of Columba

AF Columbae, also known as HD 42682, is a solitary, red hued variable star located in the southern constellation Columba, the dove. It has an apparent magnitude that fluctuates between 5.6 and 5.71. Nevertheless, it is faintly visible to the naked eye. Parallax measurements from the Gaia spacecraft place the star relatively far at a distance of 820 light years. However, it is approaching the Solar System with a poorly constrained radial velocity of −19 km/s.

HD 183552, also known as HR 7411, is a probable spectroscopic binary located in the southern constellation Telescopium. The system has a combined apparent magnitude of 5.74, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, it is estimated to be 337 light years distant. The value is horribly constrained, but it appears to receding with a radial velocity of 14 km/s.

HD 34255, also known HR 1720, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.60, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of about 1.65 kly but is approaching the Solar System with a heliocentric radial velocity of −7.7 km/s.

HD 43899, also designated as HR 2263, is a solitary, orange hued star located in the southern constellation Columba, the dove. It has an apparent magnitude of 5.53, allowing it to be faintly visible to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be 284 light years distant. It appears to be rapidly receding with a heliocentric radial velocity of 66.5 km/s. Eggen (1993) lists HD 43899 as an old disk star and its kinematics match with that of the ζ Herculis moving group.

<span class="mw-page-title-main">HD 26755</span> Binary star system in Camelopardalis

HD 26755, also known as HR 1313, is a spectroscopic binary located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.72, making it faintly visible to the naked eye under ideal conditions. Gaia DR3 parallax measurements place the system at a distance of 271 light years and is currently drifitng closer with a heliocentric radial velocity of −38 km/s. At its current distance, HD 26755's brightness is diminished by 0.19 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 22764</span> Double star; Camelopardalis

HD 22764, also known as HR 1112, is an orange hued star located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.78, allowing it to be faintly visible to the naked eye. The object is located relatively far at a distance of approximately 1,770 light years based on Gaia DR3 parallax measurements but is approaching the Solar System with a heliocentric radial velocity of −12.5 km/s. At its current distance, HD 22764's brightness is diminished by 0.66 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 197630</span> Star in the constellation of Microscopium

HD 197630, also known as HR 7933 or rarely 23 G. Microscopii, is a probable astrometric binary located in the southern constellation Microscopium. The visible component is a bluish-white hued star that is faintly visible to the naked eye with an apparent magnitude of 5.47. Based on parallax measurements from the Gaia satellite, the system is estimated to be 328 light years away. However, it is drifting closer with a heliocentric radial velocity of −30 km/s. At its current distance, HD 197630's brightness is diminished by 0.11 magnitudes due to interstellar dust. A 2012 multiplicity survey failed to confirm the velocity variations.

<span class="mw-page-title-main">V686 Coronae Australis</span> Alpha2 CVn variable; Corona Australis

V686 Coronae Australis is a solitary, bluish-white-hued variable star located in the southern constellation Corona Australis. It has an apparent magnitude that ranges between 5.25 and 5.41, which makes it faintly visible to the naked eye. Gaia DR3 parallax measurements imply a distance of 480 light years and it is slowly receding with a heliocentric radial velocity of 1.3 km/s. At its current distance V686 CrA's average brightness is diminished by 0.35 magnitudes due to extinction from interstellar dust and it has an absolute visual magnitude of −0.24.

<span class="mw-page-title-main">HD 170521</span> Distant K-type giant; Corona Australis

HD 170521, also known as HR 6937 or rarely 12 G. Coronae Australis, is a solitary star located in the southern constellation Corona Australis. It is faintly visible to the naked eye as an orange-hued point of light with an apparent magnitude of 5.69. The object is located relatively far at a distance of approximately 1,500 light years based on Gaia DR3 parallax measurements, and it is receding with a heliocentric radial velocity of 7.2 km/s. At its current distance, HD 170521's brightness is heavily diminished by 0.46 magnitudes due to extinction from interstellar dust and it has an absolute magnitude of −1.90.

References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27 –L30. Bibcode:2000A&A...355L..27H. ISSN   0004-6361. S2CID   17128864.
  3. 1 2 Levato, H. (January 1975). "Rotational velocities and spectral types for a sample of binary systems". Astronomy and Astrophysics Supplement Series. 19: 91–99. Bibcode:1975A&AS...19...91L. ISSN   0365-0138. S2CID   118523421.
  4. 1 2 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968). "A Photometric Investigation of the SCORPlO-CENTAURUS Association". The Astrophysical Journal Supplement Series. 15: 459. Bibcode:1968ApJS...15..459G. doi: 10.1086/190168 . eISSN   1538-4365. ISSN   0067-0049. S2CID   123957668.
  5. ↑ Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. eISSN   1562-6881. ISSN   1063-7729. S2CID   125853869.
  6. 1 2 Evans, David S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E, doi:10.1017/S007418090010662X (inactive 31 December 2024), S2CID   122899856 {{citation}}: CS1 maint: DOI inactive as of December 2024 (link)
  7. 1 2 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN   1562-6873. ISSN   1063-7737. S2CID   119257644.
  8. 1 2 Thackeray, A. D.; Hutchings, J. B. (1 February 1965). "Orbits of Two Double-lined Binaries HD 140008 and 178322". Monthly Notices of the Royal Astronomical Society. 129 (2): 191–197. Bibcode:1965MNRAS.129..191T. doi: 10.1093/mnras/129.2.191 . eISSN   1365-2966. ISSN   0035-8711. S2CID   125267464.
  9. 1 2 3 4 5 6 7 8 9 Howe, K. S.; Clarke, C. J. (1 January 2009). "An analysis of v sin (i) correlations in early-type binaries". Monthly Notices of the Royal Astronomical Society. 392 (1): 448–454. Bibcode:2009MNRAS.392..448H. doi: 10.1111/j.1365-2966.2008.14073.x . eISSN   1365-2966. ISSN   0035-8711. S2CID   120183969.
  10. 1 2 3 4 5 Kraicheva, Z.; Popova, E.; Tutukov, A.; Yungelson, L. (July 1980). "Catalogue of physical parameters of spectroscopic binary stars". Bull. Inf. Centre Données Stellaires. 19: 71. Bibcode:1980BICDS..19...71K. S2CID   118298938.
  11. 1 2 3 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (October 12, 2010). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1). Oxford University Press (OUP): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi: 10.1111/j.1365-2966.2010.17434.x . ISSN   0035-8711. S2CID   118629873.
  12. 1 2 3 4 5 6 7 Vansina, F.; De Grève, J. P. (October 1982). "Close binary systems before and after mass transfer". Astrophysics and Space Science. 87 (1–2): 377–401. Bibcode:1982Ap&SS..87..377V. doi:10.1007/BF00648931. eISSN   1572-946X. ISSN   0004-640X. S2CID   123986012.
  13. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  14. ↑ "HD 178322". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved May 30, 2023.
  15. ↑ Schmidt-Kaler, Th. (October 1982). "Automated spectral classification. A survey". Bulletin d'Information du Centre de Donnees Stellaires. 23: 2. Bibcode:1982BICDS..23....2S. ISSN   1169-8837. S2CID   230958433.
  16. ↑ Buscombe, W.; Morris, P. M. (1 September 1960). "The Scorpio-Centaurus Association: I. Radial Velocities of 120 Bright Stars". Monthly Notices of the Royal Astronomical Society. 121 (3): 263–278. Bibcode:1960MNRAS.121..263B. doi: 10.1093/mnras/121.3.263 . eISSN   1365-2966. ISSN   0035-8711. S2CID   121858509.
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