Tau Puppis

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Tau Puppis
Diagram showing star positions and boundaries of the Puppis constellation and its surroundings
Cercle rouge 100%.svg

Location of τ Puppis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension 06h 49m 56.16846s[1]
Declination –50° 36′ 52.4437″[1]
Apparent magnitude (V) +2.95[2]
Characteristics
Spectral type K1 III[3]
U−B color index +1.195[2]
B−V color index +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) 17.92 ± 0.40[1] mas
Distance 182 ± 4 ly
(56 ± 1 pc)
Orbit[5]
Period (P) 1,066.0 days
Semi-major axis (a) 7.15 ± 0.25 mas
Eccentricity (e) 0.090
Inclination (i) 80.20 ± 6.10°
Longitude of the node (Ω) 2.90 ± 6.20°
Periastron epoch (T) 2420992.8 HJD
Argument of periastron (ω)
(secondary)
64.00°
Details
Radius 27[6] R
Temperature 4,500[7] K
Rotational velocity (v sin i) 2.2[8] km/s
Other designations
τ Puppis, τ Pup, Tau Pup, CPD−50  1070, FK5 263, HD 50310, HIP 32768; HR 2553, PPM 335509, SAO 234735.[9]

Tau Puppis (Tau Pup, τ Puppis, τ Pup) is a star in the southern constellation of Puppis. It has an apparent visual magnitude of +2.95[2] and is located at a distance of about 182 light-years (56 parsecs) from Earth.[1] This 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 1,066.0 days (2.9 years) and a low eccentricity of 0.090.[5]

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,[10] which, at its estimated distance, equates to a physical radius of about 27 times the radius of the Sun.[6] It appears to be rotating slowly, with a projected rotational velocity of 2.2 km s–1.[8] 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 4,500,[7] giving it the orange hue of a cool, K-type star.[11]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (November 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 
  2. ^ a b c d Cousins, A. W. J. (1972), "UBV Photometry of Some Very Bright Stars", Monthly Notes of the Astronomical Society, Southern Africa 31: 69, Bibcode:1972MNSSA..31...69C 
  3. ^ a b Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars 2, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H 
  4. ^ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Carnegie Institution of Washington. Bibcode:1953QB901.W495..... 
  5. ^ a b Jancart, S. et al. (October 2005), "Astrometric orbits of SB^9 stars", Astronomy and Astrophysics 442 (1): 365–380, arXiv:astro-ph/0507695, Bibcode:2005A&A...442..365J, doi:10.1051/0004-6361:20053003 
  6. ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library 1 (3 ed.), Birkhäuser, ISBN 3-540-29692-1 . The radius (R*) is given by:
    \begin{align} 2\cdot R_*
 & = \frac{(10^{-3}\cdot 56\cdot 4.49)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\
 & \approx 54\cdot R_{\bigodot}
\end{align}
  7. ^ a b Pérez Martínez, M. Isabel; Schröder, K.-P.; Cuntz, M. (June 2011), "The basal chromospheric Mg II h+k flux of evolved stars: probing the energy dissipation of giant chromospheres", Monthly Notices of the Royal Astronomical Society 414 (1): 418–427, arXiv:1102.4832, Bibcode:2011MNRAS.414..418P, doi:10.1111/j.1365-2966.2011.18421.x 
  8. ^ a b Costa, J. M. et al. (February 2002), "The tidal effects on the lithium abundance of binary systems with giant component", Astronomy and Astrophysics 382: 1016–1020, arXiv:astro-ph/0111539, Bibcode:2002A&A...382.1016C, doi:10.1051/0004-6361:20011676 
  9. ^ "tau Pup -- Spectroscopic binary", SIMBAD (Centre de Données astronomiques de Strasbourg), retrieved 2012-01-25 
  10. ^ Richichi; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431: 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039 
  11. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16 

External links[edit]