B Persei

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b Persei
Perseus constellation map.svg
Red circle.svg
Location of b Persei (circled)
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Perseus
Right ascension 04h 18m 14.61690s [1]
Declination +50° 17′ 43.8058″ [1]
Apparent magnitude  (V)4.52 - 4.68 [2]
Characteristics
Spectral type A1III [3]
B−V color index +0.04 [4]
Variable type Ellipsoidal [2]
Astrometry
Radial velocity (Rv)19.8±0.9 [5] km/s
Proper motion (μ)RA: 45.42±0.40 [1] mas/yr
Dec.: −56.72±0.32 [1] mas/yr
Parallax (π)10.40±0.35  mas [1]
Distance 310 ± 10  ly
(96 ± 3  pc)
Absolute magnitude  (MV)0.3 [6]
Orbit [7]
PrimaryA or Aa
CompanionB or Ab
Period (P)1.52735997±0.00000036 days
Eccentricity (e)0.0
Inclination (i)22±3 or 55±3 [6] °
Periastron epoch (T)2450001.0931±0.003
Orbit [8]
PrimaryAB
CompanionC or Ac
Period (P)703.06±0.07 days
Semi-major axis (a)26.22±0.06 mas
Eccentricity (e)0.185±0.003
Inclination (i)90.5±0.1°
Longitude of the node (Ω)120.0±0.1°
Periastron epoch (T)2440080±3
Argument of periastron (ω)
(secondary)		212±1°
Details
A or Aa
Mass 2.25 [6]   M☉
Radius 3.2 [9]   R☉
Luminosity 59 [6]   L☉
Temperature 9,000 [6]   K
Rotational velocity (v sin i)81 [10]  km/s
B or Ab
Mass 0.56 [11]   M☉
Radius 0.25 [9]   R☉
Luminosity 4.5 - 5.9 [6]   L☉
Temperature 6,700 [6]   K
C or Ac
Mass 1.24 [11]   M☉
Luminosity2 [12]   L☉
Other designations
BD+49°1150, GC  5174, HD 26961, HR 1324, HIP 20070, SAO  24531
Database references
SIMBAD data
Light curves for b Persei. The top panel, plotted from TESS data, shows the variability of the inner binary pair. The lower panels, plotted from AAVSO data, show two eclipses. BPerLightCurve.png
Light curves for b Persei. The top panel, plotted from TESS data, shows the variability of the inner binary pair. The lower panels, plotted from AAVSO data, show two eclipses.

b Persei (also known as HD 26961) is a spectroscopic triple star in the constellation Perseus. Its apparent magnitude is 4.60, making it visible to the naked eye. [6] It is about 320 light years away. [1]

In addition to the primary, an A-type giant, there is a smaller and cooler companion in a 1.53 day orbit, probably an F-class star around absolute magnitude 3.0, and a more distant companion (star C or Ac) in an orbit calculated to be 702 days long. [6] The close binary pair forms a rotating ellipsoidal variable with a 1.53 day period. Star C forms an Algol-type variable system with the close binary, showing both primary eclipses (when star C passes in front of the inner pair) and secondary eclipses (when the inner pair passes in front of star C). [15] Timings of the eclipses show a 704.5-day period. [12]

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 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ↑ Abt, Helmut A. (2009). "MK Classifications of Spectroscopic Binaries". The Astrophysical Journal Supplement. 180 (1): 117–18. Bibcode:2009ApJS..180..117A. doi:10.1088/0067-0049/180/1/117.
  4. ↑ 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
  5. ↑ 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.
  6. 1 2 3 4 5 6 7 8 9 Hill, G.; Aikman, G. C. L.; Cowley, A. P.; Bolton, C. T.; Thomas, J. C. (1976). "The radio-flaring triple system B Per". The Astrophysical Journal. 208: 152. Bibcode:1976ApJ...208..152H. doi:10.1086/154590.
  7. ↑ Koubský, Pavel; Hadrava, Petr; Šarounová, Lenka (December 2004). Study of b Per: an attempt to find lines of other components in the SB1 system. Spectroscopically and Spatially Resolving the Components of the Close Binary Stars. Vol. 318. Astronomical Society of the Pacific. pp. 103–106. Bibcode: 2004ASPC..318..103K .
  8. ↑ Collins, Donald F.; Sanborn, Jason; Zavala, Robert T. (May 2014). Modern V Photometry of the Eclipsing Triple System b Persei. The Society for Astronomical Sciences 33rd Annual Symposium on Telescope Science. Society for Astronomical Sciences. pp. 205–211. Bibcode: 2014SASS...33..205C .
  9. 1 2 Duerbeck, H. W.; Schettler, A. (1979). "Photometric and spectroscopic study of the ellipsoidal variable b Persei". Acta Astronomica. 29: 225. Bibcode:1979AcA....29..225D.
  10. ↑ Royer, F. (2007). "Rotational velocities of A-type stars. III. Velocity distributions". Astronomy and Astrophysics. 463 (2): 671–682. arXiv: astro-ph/0610785 . Bibcode:2007A&A...463..671R. doi:10.1051/0004-6361:20065224. S2CID   18475298.
  11. 1 2 Tokovinin, Andrei (23 February 2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv: 1712.04750 . Bibcode:2018ApJS..235....6T. doi: 10.3847/1538-4365/aaa1a5 . eISSN   1538-4365.
  12. 1 2 "Alert Notice 791: Anticipated secondary eclipse of b Per centered on September 29 2022 UT". AAVSO . Retrieved 2022-09-15.
  13. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 14 September 2022.
  14. ↑ "Download Data". aavso.org. AAVSO. Retrieved 14 September 2022.
  15. ↑ "b Per". The International Variable Star Index. AAVSO. Retrieved 15 September 2022.
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