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Pi Canis Majoris

Pi Canis Majoris
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Canis Major
Right ascension 06h 55m 37.43099s[1]
Declination −20° 08′ 11.3902″[1]
Apparent magnitude (V) +4.69[2]
Characteristics
Spectral type F1.5 V[3]
U−B color index +0.06[2]
B−V color index +0.36[2]
Astrometry
Radial velocity (Rv)−37.9±5.5[4] km/s
Proper motion (μ) RA: +51.50[1] mas/yr
Dec.: +39.58[1] mas/yr
Parallax (π)33.80 ± 0.24 mas[1]
Distance96.5 ± 0.7 ly
(29.6 ± 0.2 pc)
Absolute magnitude (MV)+2.06[5]
Details
π CMa A
Mass1.32[6] M☉
Luminosity9[7] L☉
Surface gravity (log g)3.91[6] cgs
Temperature6,863±233[6] K
Metallicity [Fe/H]−0.18[3] dex
Rotational velocity (v sin i)91.7±4.6[5] km/s
Age763[6] Myr
Other designations
π CMa, 19 Canis Majoris, BD−19°1610, HD 51199, HIP 33302, HR 2590, SAO 172579, ADS 5602, CCDM 06556-2008[8]
Database references
SIMBADdata

Pi Canis Majoris (π Canis Majoris; Latin for 'Greater Dog') is a binary star[9] system in the southern constellation of Canis Major. It is visible to the naked eye, having an apparent visual magnitude of +4.69.[2] Based upon an annual parallax shift of 33.80 mas as seen from Earth,[1] this system is located 96.5 light years from the Sun. The star is moving in the general direction of the Sun with a radial velocity of −37.9 km/s. It will make its closest approach in around 733,000 years when it comes within 23 ly (7 pc).[4]

The brighter primary, component A, is an F-type main-sequence star with a stellar classification of F1.5 V.[3] It is a periodic variable star with a frequency of 11.09569 cycles per day (2.16 hours per cycle) and an amplitude of 0.0025 in magnitude.[10] The star has an estimated 1.32[6] times the mass of the Sun and is radiating nine[7] times the Sun's luminosity from its photosphere at an effective temperature of around 6,863 K.[6] It displays a strong infrared excess at a wavelength of 24 μm and a weaker excess at 70 μm, indicating the presence of a circumstellar disk of dust with a temperature of 188 K, orbiting at 6.7 AU from the host star.[11]

The magnitude 9.6 companion, component B, lies at an angular separation of 11.6 arc seconds from the primary as of 2008.[9] Their projected separation is about 339 AU.[11]

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This star is the origin of the alien crystal, and the destination of starship Salvare, on Netflix show Another Life.

See also

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References

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  1. ^ a b c d e f van Leeuwen, F. (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, S2CID 18759600.
  2. ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. ^ a b c Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ a b Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
  5. ^ a b Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911, S2CID 8642707
  6. ^ a b c d e f David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  7. ^ a b McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  8. ^ "pi. CMa". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-03.{{cite web}}: CS1 maint: postscript (link)
  9. ^ a b Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  10. ^ Koen, Chris; Eyer, Laurent (2002), "New periodic variables from the Hipparcos epoch photometry", Monthly Notices of the Royal Astronomical Society, 331 (1): 45–59, arXiv:astro-ph/0112194, Bibcode:2002MNRAS.331...45K, doi:10.1046/j.1365-8711.2002.05150.x, S2CID 10505995.
  11. ^ a b Trilling, D. E.; et al. (April 2007), "Debris disks in main-sequence binary systems", The Astrophysical Journal, 658 (2): 1264–1288, arXiv:astro-ph/0612029, Bibcode:2007ApJ...658.1289T, doi:10.1086/511668, S2CID 14867168.