Astronomy:V539 Arae

From HandWiki
Short description: Triple star system in the constellation Ara
"Nu1 Arae" redirects here. For other star systems with this Bayer designation, see Nu Arae.
V539 Arae
The location of V539 Arae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ara[1]
Right ascension  17h 50m 28.393s[2]
Declination −53° 36′ 44.66″[2]
Apparent magnitude (V) 5.62[3]
Characteristics
Spectral type B2 V + B3 V + A1 V[3]
U−B color index −0.64[citation needed]
B−V color index −0.099±0.017[1]
Variable type Algol/SPB[4]
Astrometry
Radial velocity (Rv)−4.3±2.9[5] km/s
Proper motion (μ) RA: +2.517[2] mas/yr
Dec.: −12.105[2] mas/yr
Parallax (π)2.5208 ± 0.1096[2] mas
Distance1,290 ± 60 ly
(400 ± 20 pc)
Absolute magnitude (MV)−1.83/−1.11[6]
Orbit[7]
Period (P)3.1690854(12) d
Eccentricity (e)0.0548(15)
Inclination (i)85.2°
Argument of periastron (ω)
(secondary)		118.9(1.2)°
Details[8]
V539 Ara A
Mass6.239±0.066 M☉
Radius4.551±0.019 R☉
Luminosity2,000+240−210 L☉
Surface gravity (log g)3.9170±0.0029 cgs
Temperature18,100±500[6] K
Rotational velocity (v sin i)100[9] km/s
Age23.2±2.9[10] Myr
V539 Ara B
Mass5.313±0.060 M☉
Radius3.575±0.035 R☉
Luminosity980+130−110 L☉
Surface gravity (log g)4.0570±0.0084 cgs
Temperature17,100±500[6] K
Rotational velocity (v sin i)130[9] km/s
Other designations
Boss 4496, ν1 Arae, V539 Ara, CD−53°7423, GC 24187, HD 161783, HIP 87314, HR 6622, SAO 245065, PPM 346351, WDS J17505-5337A[11]
Database references
SIMBADAB
A

V539 Arae is a multiple star system in the southern constellation of Ara. It has the Bayer designation Nu1 Arae , which is Latinized from ν1 Arae and abbreviated Nu1 Ara or ν1 Ara. This is a variable star system, the brightness of which varies from magnitude 5.71 to 6.24, making it faintly visible to the naked eye under good observing conditions.[12] Based upon an annual parallax shift of 2.52 mas,[2] this system is at a distance of approximately 1,290 light-years (400 parsecs) from Earth. The system is drifting closer to the Sun with a radial velocity of −4 km/s.[5]

A visual band light curve for V539 Arae, adapted from Knipe (1971)[13]

In 1930, Ferdinand Johannes Neubauer found that the star (usually called Boss 4496 at the time) is a spectroscopic binary. He did not detect any brightness variability.[14] Eclipses were first reported by E. Schoeffel and U. Kohler in 1965. The period they reported is 1/2 the currently accepted value, because they did not realize that the light curve has a deep secondary minimum.[15][16] In 1996, the secondary component was found to be a slowly pulsating B-type star (SPB) with periods of periods of 1.36, 1.78 and possibly 1.08 days.[17]

The core members of this system, ν1 Ara AB, consist of a pair of B-type main-sequence stars in a detached orbit with a period of 3.169 days and an eccentricity of 0.055.[7] Their respective stellar classifications are B2 V and B3 V, and they have a combined visual magnitude of 5.65. Because the orbital plane lies close to the line of sight from the Earth, this pair form a detached eclipsing binary of the Algol type.[11] The eclipse of the primary causes a decrease of 0.52 in magnitude, while the secondary eclipse decreases the magnitude by 0.43.[18]

At an angular separation of 12.34 arcseconds, is a possible tertiary component of this system; a magnitude 9.40 A-type main-sequence star with a classification of A1 V.[3] A 2005 study of the orbit of the main pair demonstrated an apsidal motion, suggesting the influence of a third body. The initial estimate found an orbital period of 42.3±0.8 years and a mass of 1.63 M☉.[7] In 2022, a more refined study suggested the influence of two stellar objects with masses of 0.41 M☉ and 1.74 M☉.[19]

The system is sometimes referred as Upsilon1 Arae (υ1 Arae), and more generally unlettered.[20]

References

  1. ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  4. ↑ Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, GCVS 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S, http://www.sai.msu.su/gcvs/gcvs/index.htm, retrieved 2025-04-30. 
  5. ↑ 5.0 5.1 Gontcharov, G. A. (2006), "Pulkovo compilation of radial velocities for 35495 stars in a common system", Astronomy Letters 32 (11): 759–771, doi:10.1134/S1063773706110065, Bibcode: 2006AstL...32..759G. 
  6. ↑ 6.0 6.1 6.2 Torres, G. et al. (February 2010), "Accurate masses and radii of normal stars: modern results and applications", The Astronomy and Astrophysics Review 18 (1–2): 67–126, doi:10.1007/s00159-009-0025-1, Bibcode: 2010A&ARv..18...67T. 
  7. ↑ 7.0 7.1 7.2 Wolf, M.; Zejda, M. (July 2005), "Apsidal motion in southern eccentric eclipsing binaries: V539 Ara, GG Lup, V526 Sgr and AO Vel", Astronomy and Astrophysics 437 (2): 545–551, doi:10.1051/0004-6361:20041868, Bibcode: 2005A&A...437..545W. 
  8. ↑ Southworth, John; Bowman, Dominic M. (July 2022), "High-mass pulsators in eclipsing binaries observed using TESS", Monthly Notices of the Royal Astronomical Society 513 (3): 3191–3209, doi:10.1093/mnras/stac875, Bibcode: 2022MNRAS.513.3191S. 
  9. ↑ 9.0 9.1 Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institution of Washington), Bibcode: 1953GCRV..C......0W. 
  10. ↑ Tetzlaff, N. et al. (January 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, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  11. ↑ 11.0 11.1 "V* V539 Ara". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+V539+Ara. 
  12. ↑ Samus, N. N. et al., V539 Ara, Lomonosov Moscow State University, http://www.sai.msu.su/gcvs/cgi-bin/search2.cgi?search=V539+Ara, retrieved 25 November 2024. 
  13. ↑ Knipe, G. F. G. (September 1971), "The light curve and orbital elements of V539 Arae", Astronomy & Astrophysics 14: 70–77, Bibcode: 1971A&A....14...70K. 
  14. ↑ Neubauer, F. J. (August 1930), "Forty-two Spectroscopic Binary Stars", Publications of the Astronomical Society of the Pacific 42 (248): 235–236, doi:10.1086/124043, Bibcode: 1930PASP...42..235N. 
  15. ↑ Schoeffel, E.; Kohler, U. (January 1965), "Photometric Light-Curves of Bright Southern BV-Stars Eclipsing Binaries", Information Bulletin on Variable Stars 77: 1, Bibcode: 1965IBVS...77....1S. 
  16. ↑ Thackeray, A. D.; Knipe, G. F. G. (1965), "The Eclipsing Variable HD 161783 (BV 420)", Monthly Notes of the Astronomical Society of Southern Africa 24: 109, Bibcode: 1965MNSSA..24..109T. 
  17. ↑ Clausen, J. V. (April 1996), "V539 Arae: first accurate dimensions of a slowly pulsating B star", Astronomy and Astrophysics 308: 151–169, Bibcode: 1996A&A...308..151C. 
  18. ↑ Malkov, O. Yu. et al. (February 2006), "A catalogue of eclipsing variables", Astronomy and Astrophysics 446 (2): 785–789, doi:10.1051/0004-6361:20053137, Bibcode: 2006A&A...446..785M. 
  19. ↑ Wolf, M. et al. (April 2022), "The two eccentric eclipsing binaries in multiple systems: V539 Arae and V335 Serpentis", New Astronomy 92: id. 101708, doi:10.1016/j.newast.2021.101708, Bibcode: 2022NewA...9201708W. 
  20. ↑ Hoffleit, D.; Warren, Jr., W. H. (1991), "Note for HR 6622", The Bright Star Catalogue, http://vizier.u-strasbg.fr/viz-bin/VizieR?-6N&-out.form=H0&//*&-source%3DV/50/notes&HR%3D6622, retrieved 2025-04-30. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:V539_Arae&oldid=3928993"