Beta Sextantis

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Template:Short description

β Sextantis
File:BetSexLightCurve.png
A light curve for Beta Sextantis, plotted from TESS data,[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Sextans
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 5.07[3]
Characteristics
Evolutionary stage Main sequence[4]
Spectral type B6 V[5] or B5 IV/V[6]
U−B Template:Engvar −0.51[3]
B−V Template:Engvar −0.14[3]
Variable type α2 CVn[7]
Astrometry
Radial velocity (Rv)Script error: No such module "val".[8] km/s
Proper motion (μ) RA: −39.290 mas/yr[2]
Dec.: −23.582 mas/yr[2]
Parallax (π)8.8899±0.1477 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−0.38[9]
Details
MassScript error: No such module "val".[4] Template:Solar mass
Radius3.00[10] Template:Solar radius
Luminosity330[4] Template:Solar luminosity
Surface gravity (log g)4.21[11] cgs
Temperature13,870[4] K
Metallicity [Fe/H]0.19[11] dex
Rotational velocity (v sin i)Script error: No such module "val".[11] km/s
Age216[12] Myr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist[13]
Database references
SIMBADdata

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Beta Sextantis, Latinized from β Sextantis, is a variable star in the equatorial constellation of Sextans. With an apparent visual magnitude of 5.07,[3] it is faintly visible to the naked eye on a dark night. According to the Bortle scale, it can be viewed from brighter lit suburban skies. The distance to this star, based upon an annual parallax shift of 8.89 mas,[2] is around 367 light years.

This star served as a primary standard in the MK spectral classification system with a stellar classification of B6 V,[5] indicating that it is a B-type main sequence star. However, Houk and Swift (1999) list a classification of B5 IV/V, suggesting it may be transitioning into a subgiant star.[6] Stellar evolution models support this is a main sequence star.[4] It has served as a uvby photometric standard, but is also categorized as an Alpha2 Canum Venaticorum variable[7] with a suspected period of 15.4 days. This lengthy a period conflicts with a relatively high projected rotational velocity of 85 km/s, leaving the explanation for the variance unresolved.[11][5]

References

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  6. ↑ a b Script error: No such module "Citation/CS1".
  7. ↑ a b Script error: No such module "Citation/CS1".
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  9. ↑ Template:Cite XHIP
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  11. ↑ a b c d Script error: No such module "Citation/CS1".
  12. ↑ Script error: No such module "Citation/CS1".
  13. ↑ Template:Cite simbad

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Template:Stars of Sextans Template:Sky

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