Xi Phoenicis

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Xi Phoenicis

A light curve for Xi Phoenicis plotted from TESS data[1]
Observation data
ICRS
)
Constellation Phoenix
Right ascension 00h 41m 46.30191s[2]
Declination −56° 30′ 05.2370″[2]
Apparent magnitude (V) 5.70[3] + 9.98[4]
Characteristics
Spectral type A3 Vp(SrCr v. st; K sn)[5]
B−V color index +0.19[3]
Variable type α2 CVn[6]
Distance
221.1 ± 0.5 ly
(67.8 ± 0.2 pc)
Details
ξ Phe A
Myr
ξ Phe B
Mass0.81[11] M☉
Radius0.76+0.04
−0.03[8] R☉
Luminosity0.328±0.001[8] L☉
Temperature4,999+116
−100[8] K
HR 183, SAO 232152, WDS J00418-5630A[12]
Database references
SIMBADdata

Xi Phoenicis,

light years from the Sun. The system is moving away from the Sun with a radial velocity of about +10 km/s.[7]

Primary star

The primary is a

Sun's luminosity from its photosphere at an effective temperature of 8,300 K.[4] Stellar evolution models indicate its properties are consistent with a mass of 1.91 times the solar mass and an age of 680 million years.[9]

Xi Phoenicis has a strong

kG, inclined by 88° in relation to the rotation axis of the star. The reconstruction of the stellar surface by Doppler imaging showed it is heterogenous with regions of different chemical abundances, which seem to be associated to the geometry of the magnetic field. For instance, lithium and oxygen have high abundances in the magnetic poles and low abundances in the magnetic equator, while elements like silicon and lanthanum are concentrated in a region between the magnetic equator and poles.[4] However, these results have been contested, and it is possible the abundance maps are spurious due to the strong magnetic field.[13]

An Alpha2 Canum Venaticorum variable, Xi Phoenicis's visual magnitude varies between 5.68 and 5.78 with a period of 3.9516 days,[6] which is the rotation period of the star and is also associated with changes in the spectrum and the magnetic field. The brightness variation is maximum in the v band, with an amplitude of 0.13 magnitudes. The light curve in this band is symmetrical and has two distinct minima separated by half a rotation period, while the two maxima are igual. In other bands the variability is smaller or even absent, and doesn't show a regular pattern like in v.[10] The star is similar in many aspects to rapidly oscillating Ap stars, but does not display the rapid pulsations typical of these stars.[14]

Secondary star

Xi Phoenicis is known as a

arcseconds and position angle of 252.5°, in relation to the primary. Considering the distance to the system, this corresponds to a projected separation of 875 AU between the stars. The mass of the secondary is estimated at 0.81 times the solar mass.[11]

This star is in the second catalogue of the Gaia spacecraft, which measured independently a distance equal to that of the primary, and estimated a radius of 0.76 R☉, luminosity of 0.33 L☉, and effective temperature of 5,000 K.[8]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^
    S2CID 18759600
    .
  3. ^
    Bibcode:1966RGOB..121....1C
    .
  4. ^
    S2CID 53700611
    , A151.
  5. ^
    doi:10.1086/192182
    .
  6. ^
    S2CID 125853869
    .
  7. ^
    S2CID 59451347
    , A61.
  8. ^
    doi:10.1051/0004-6361/201833051
    .
  9. ^
    S2CID 18596834
    .
  10. ^
    Bibcode:1980A&A....81..323M
    .
  11. ^
    S2CID 88503488
    .
  12. ^ "ksi Phe". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-20.
  13. doi:10.1093/mnras/stw2885
    .
  14. S2CID 19030373
    .
  15. ^
    doi:10.1086/323920
    .
  16. S2CID 14878976
    .
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