Pi Canis Majoris

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]

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

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]

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

See also

References
  1. 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. 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. 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. 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. 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. 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. 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. 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. 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.
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