AE Pictoris

AE Pictoris

A light curve for AE Pictoris, adapted from Pedersen et al. (2019)
Observation data
Epoch J2000      Equinox ICRS
Constellation Pictor
Right ascension 06h 31m 10.63900s
Declination −61° 52′ 46.3515″
Apparent magnitude (V) 6.14
Characteristics
Spectral type B3V
B−V color index −0.147±0.006
Variable type Eclipsing binary
Astrometry
Radial velocity (Rv)34.0±7.4 km/s
Proper motion (μ) RA: −9.142 mas/yr
Dec.: +12.087 mas/yr
Parallax (π)2.2770±0.0678 mas
Distance1,430 ± 40 ly
(440 ± 10 pc)
Absolute magnitude (MV)1.73
Orbit
Period (P)2.9723 d
Eccentricity (e)0.10
Periastron epoch (T)2,431,998.871 JD
Argument of periastron (ω)
(secondary)		39.0°
Semi-amplitude (K1)
(primary)		119.0 km/s
Details
AE Pic A
Mass7.1±0.1 M☉
Luminosity (bolometric)2,569 L☉
Temperature17,873 K
Metallicity [Fe/H]3.93 dex
Rotation1.490911 d
Rotational velocity (v sin i)70 km/s
Age27.7±1.4 Myr
AE Pic B
Temperature11,699 K
Metallicity [Fe/H]4.02 dex
Rotational velocity (v sin i)42 km/s
Other designations
AE Pic, CD−61°1394, HD 46792, HIP 31068, HR 2410, SAO 249572
Database references
SIMBADdata

AE Pictoris is an eclipsing binary star system in the southern constellation of Pictor. This dim, blue-white hued point of light is just barely visible to the naked eye; it has an apparent visual magnitude of 6.09, which drops to magnitude 6.14 during an eclipse. The system is located around 1,430 light years away from the Sun based on parallax, and it is receding with a radial velocity of 34 km/s.

This is a spectroscopic binary system with an orbital period of 2.97 days and an eccentricity of 0.10. The minimum value of the semimajor axis for the pair is 4.8 Gm (6.9 R☉). The secondary star was only recently (in 2023) detected, making it a double-lined spectroscopic binary. It is classed as a probable eclipsing binary variable (EB:), but with some uncertainty regarding the specific type. This is a candidate runaway star system, having a peculiar velocity of 24.9+4.9
−5.1 km/s relative to its neighbors. The visible component is a B-type main-sequence star with a stellar classification of B3V. it is 28 million years old with seven times the mass of the Sun. The star is radiating 2,569 times the luminosity of the Sun from its photosphere at an effective temperature of 18,700 K.

References

  1. ↑ Pedersen, May G.; Chowdhury, Sowgata; Johnston, Cole; Bowman, Dominic M.; Aerts, Conny; Handler, Gerald; De Cat, Peter; Neiner, Coralie; David-Uraz, Alexandre; Buzasi, Derek; Tkachenko, Andrew; Simón-Díaz, Sergio; Moravveji, Ehsan; Sikora, James; Mirouh, Giovanni M.; Lovekin, Catherine C.; Cantiello, Matteo; Daszyńska-Daszkiewicz, Jadwiga; Pigulski, Andrzej; Vanderspek, Roland K.; Ricker, George R. (February 2019). "Diverse Variability of O and B Stars Revealed from 2-minute Cadence Light Curves in Sectors 1 and 2 of the TESS Mission: Selection of an Asteroseismic Sample". The Astrophysical Journal Letters. 872 (1): L9. arXiv:1901.07576. Bibcode:2019ApJ...872L...9P. doi:10.3847/2041-8213/ab01e1.
  2. 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.
  3. ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H.
  4. 1 2 Hiltner, W. A.; et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal, 157: 313–326, Bibcode:1969ApJ...157..313H, doi:10.1086/150069.
  5. 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.
  6. 1 2 3 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  7. 1 2 Sahade, J.; Landi Dessy, J. (January 1950), "The Spectroscopic Binary CPD -61°669", Astrophysical Journal, 111: 191, Bibcode:1950ApJ...111..191S, doi:10.1086/145251.
  8. 1 2 3 4 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, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  9. 1 2 Hohle, M. M.; et al. (2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  10. 1 2 3 4 5 6 7 Kovalev, Mikhail; Straumit, Ilya (2023). "Application of the binary spectral model to high-resolution spectra. First estimation of the fundamental parameters for HD 20784". Monthly Notices of the Royal Astronomical Society. 523 (3): 3741–3748. arXiv:2210.00863. Bibcode:2023MNRAS.523.3741K. doi:10.1093/mnras/stad1667.
  11. ↑ Barraza, L. F.; Gomes, R. L.; Messias, Y. S.; Leão, I. C.; Almeida, L. A.; Janot-Pacheco, E.; Brito, A. C.; Brito, F. A. C.; Santana, J. V.; Gonçalves, N. S.; Das Chagas, M. L.; Teixeira, M. A.; De Medeiros, J. R.; Canto Martins, B. L. (2022). "Rotation Signature of TESS B-type Stars. A Comprehensive Analysis". The Astrophysical Journal. 924 (2): 117. arXiv:2202.01022. Bibcode:2022ApJ...924..117B. doi:10.3847/1538-4357/ac3335. S2CID 246030494.
  12. ↑ "AE Pic". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-03.
  13. ↑ Avvakumova, E. A.; et al. (October 2013), "Eclipsing variables: Catalogue and classification", Astronomische Nachrichten, 334 (8): 860, Bibcode:2013AN....334..860A, doi:10.1002/asna.201311942, hdl:10995/27061.
  14. ↑ Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Carnegie Institute Washington D.C. Publication, Bibcode:1953GCRV..C......0W.