BD Phoenicis

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BD Phoenicis
BDPheLightCurve.png
A blue band light curve for BD Phoenicis, adapted from Koen et al. (2003) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix
Right ascension 01h 50m 54.44s [2]
Declination −50° 12′ 22.09″ [2]
Apparent magnitude  (V)5.90 – 5.94 [3]
Characteristics
Spectral type A1Va λ Boo [4]
Variable type δ Scuti [3]
Astrometry
Radial velocity (Rv)3.0 [5]  km/s
Proper motion (μ)RA: -47.85 [2]   mas/yr
Dec.: -3.70 [2]   mas/yr
Parallax (π)12.7260 ± 0.0447  mas [2]
Distance 256.3 ± 0.9  ly
(78.6 ± 0.3  pc)
Absolute magnitude  (MV)1.5 ± 0.1 [1]
Details
Mass 2.02 ± 0.04 [1]   M☉
Luminosity 20.5 ± 0.34 [6]   L☉
Surface gravity (log g)3.91 ± 0.08 [1]   cgs
Temperature 7,818 ± 38 [6]   K
Rotational velocity (v sin i)120 ± 5 [1]  km/s
Age 813+38
−89 [1]   Myr
Other designations
BD Phe, CD−50°514, HD  11413, HIP  8593, HR  541, SAO  232542 [7]
Database references
SIMBAD data

BD Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 256 light-years (78 parsecs ) from Earth. [2] Its absolute magnitude is calculated at 1.5. [1]

Description

BD Phoenicis is a Lambda Boötis star, an uncommon type of peculiar stars that have very low abundances of iron-peak elements. In particular, BD Phoenicis has near-solar carbon and oxygen content, but its iron abundance is only 4% of the solar value. [1] BD Phoenicis is also a pulsating variable of Delta Scuti type, varying its apparent magnitude between 5.90 and 5.94. [3] A study of its light curve detected seven pulsation periods that range from 50 to 84 minutes, the strongest one having a period of 57 minutes and an amplitude of 9 milli-magnitudes. Pulsations are common among Lambda Boötis stars and seem to be more common than normal main sequence stars of the same spectral type. [1]

BD Phoenicis is an A-type main-sequence star with a spectral type of A1Va. [4] Stellar evolution models indicate it contains double the solar mass and an age of about 800 million years—having completed 83% of its main sequence lifetime. [1] It is radiating 21 times the Sun's luminosity from its photosphere at an effective temperature of 7800  K . [6] BD Phoenicis has a composite spectra that indicate it is a binary star, but nothing is known about its companion. [8] [6]

Observations by the Herschel Space Observatory have detected an infrared excess from BD Phoenicis, indicating that there is a debris disk in the system. By modeling the emission as a black body, it is estimated that the dust has a temperature of 55±2 K and is at a distance of 118±10  au from the star. The existence of debris disks is possibly related to the Lambda Boötis phenomenon. [6]

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<span class="mw-page-title-main">Psi Phoenicis</span>

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<span class="mw-page-title-main">AE Phoenicis</span> Star in the constellation Phoenix

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<span class="mw-page-title-main">BB Phoenicis</span> Star in the constellation Phoenix

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<span class="mw-page-title-main">AZ Phoenicis</span> A type variable star in the constellation Phoenix

AZ Phoenicis is a variable star in the constellation of Phoenix. It has an average visual apparent magnitude of 6.47, so it is at the limit of naked eye visibility. From parallax measurements by the Gaia spacecraft, it is located at a distance of 322 light-years from Earth. Its absolute magnitude is calculated at 1.65.

<span class="mw-page-title-main">Rho Phoenicis</span> Variable star in the constellation Phoenix

Rho Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 245 light-years from Earth.

<span class="mw-page-title-main">DY Pegasi</span> Star in the constellation Pegasus

DY Pegasi, abbreviated DY Peg, is a binary star system in the northern constellation of Pegasus. It is a well-studied SX Phoenicis variable star with a brightness that ranges from an apparent visual magnitude of 9.95 down to 10.62 with a period of 1.75 hours. This system is much too faint to be seen with the naked eye, but can be viewed with large binoculars or a telescope. Based on its high space motion and low abundances of heavier elements, it is a population II star system.

References

  1. 1 2 3 4 5 6 7 8 9 10 Koen, C.; Paunzen, E.; Van Wyk, F.; Marang, F.; Chernyshova, I. V.; Andrievsky, S. M. (2003). "The pulsational characteristics of the λ Bootis type star BD Phe (HD 11413)". Monthly Notices of the Royal Astronomical Society. 338 (4): 931. Bibcode:2003MNRAS.338..931K. doi: 10.1046/j.1365-8711.2003.06149.x .
  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. 1 2 3 Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  4. 1 2 Gray, R. O.; Garrison, R. F. (1987). "The Early A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation". The Astrophysical Journal Supplement Series. 65: 581. Bibcode:1987ApJS...65..581G. doi: 10.1086/191237 .
  5. ↑ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv: 1606.08053 , Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID   119231169.
  6. 1 2 3 4 5 Draper, Z. H.; Matthews, B. C.; Kennedy, G. M.; Wyatt, M. C.; Venn, K. A.; Sibthorpe, B. (2016). "IR excesses around nearby Lambda Boo stars are caused by debris discs rather than ISM bow waves". Monthly Notices of the Royal Astronomical Society. 456 (1): 459. arXiv: 1511.05919 . Bibcode:2016MNRAS.456..459D. doi: 10.1093/mnras/stv2696 . S2CID   118343020.
  7. ↑ "BD Phe". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 January 2019.
  8. ↑ Faraggiana, R.; Bonifacio, P.; Caffau, E.; Gerbaldi, M.; Nonino, M. (2004). "λ Bootis stars with composite spectra". Astronomy and Astrophysics. 425 (2): 615–626. arXiv: astro-ph/0406265 . Bibcode:2004A&A...425..615F. doi:10.1051/0004-6361:20040216. S2CID   117998682.
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