Tau Puppis

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Template:Short description

Tau Puppis
Template:Location mark
Location of τ Puppis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) +2.95[2]
Characteristics
Spectral type K1 III[3]
U−B Template:Engvar +1.195[2]
B−V Template:Engvar +1.20[2]
Astrometry
Radial velocity (Rv)+36.4[4] km/s
Proper motion (μ) RA: +34.36[1] mas/yr
Dec.: −69.11[1] mas/yr
Parallax (π)18.7577±0.3475 mas[5]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−0.80[6]
Orbit[7][8]
Period (P)Script error: No such module "val".
Semi-major axis (a)Script error: No such module "val".
Eccentricity (e)Script error: No such module "val".
Inclination (i)80.20 ± 6.10°
Longitude of the node (Ω)2.90 ± 6.20°
Periastron epoch (T)Script error: No such module "val".
Argument of periastron (ω)
(secondary)		64.00°
Details
Mass3.19[9] Template:Solar mass
Radius27[10] Template:Solar radius
TemperatureScript error: No such module "val".[9] K
Rotational velocity (v sin i)2.2[11] km/s
Age540[9] Myr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist[12]
Database references
SIMBADdata

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Tau Puppis, Latinized from τ Puppis, is a star in the southern constellation of Puppis, near the southern constellation boundary with Carina. It is visible to the naked with an apparent visual magnitude of +2.95[2] and is located at a distance of about Script error: No such module "convert". from Earth.[1] The variable radial velocity of this system was detected by H. D. Curtis and H. K. Palmer in 1908, based on observations made at the D. O. Mills Observatory.[8] It is a spectroscopic binary star system, with the presence of the secondary component being revealed by the shifts of absorption lines in the spectrum resulting from the Doppler effect. The two components orbit each other with a period of Script error: No such module "convert". and a low eccentricity of 0.090.[7]

The primary component of this system has a stellar classification of K1 III.[3] A luminosity class 'III' indicates this has expanded into a giant star after exhausting the supply of hydrogen at its core and evolving away from the main sequence of stars like the Sun. The interferometry-measured angular diameter of this star, after correcting for limb darkening, is 4.49 ± 0.07 mas,[13] which, at its estimated distance, equates to a physical radius of about 27 times the radius of the Sun.[10] It appears to be rotating slowly, with a projected rotational velocity of 2.2 km s−1.[11] This gives a lower bound on the azimuthal velocity of rotation along the star's equator. Tau Puppis is radiating energy from its outer envelope at an effective temperature of around Script error: No such module "val".,[14] giving it the orange hue of a cool, K-type star.[15]

References

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  1. ↑ a b c d e Script error: No such module "citation/CS1".
  2. ↑ a b c d Script error: No such module "citation/CS1".
  3. ↑ a b Script error: No such module "citation/CS1".
  4. ↑ Script error: No such module "Citation/CS1".
  5. ↑ Template:Cite Gaia EDR3
  6. ↑ Script error: No such module "citation/CS1".
  7. ↑ a b Script error: No such module "citation/CS1".
  8. ↑ a b Script error: No such module "citation/CS1".
  9. ↑ a b c Script error: No such module "citation/CS1".
  10. ↑ a b Script error: No such module "citation/CS1".. The radius (R*) is given by:
    2⋅R*=(10−3⋅56⋅4.49) AU0.0046491 AU/R⨀≈54⋅R⨀
  11. ↑ a b Script error: No such module "citation/CS1".
  12. ↑ Template:Cite simbad
  13. ↑ Script error: No such module "citation/CS1".
  14. ↑ Script error: No such module "citation/CS1".
  15. ↑ Script error: No such module "citation/CS1".

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External links

Template:Stars of Puppis

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