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Z Canis Majoris

Not to be confused with Zeta Canis Majoris.
Z Canis Majoris

A visual band light curve for Z Canis Majoris, plotted from All Sky Automated Survey data[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Canis Major
Right ascension 07h 03m 43.15994s[2]
Declination −11° 33′ 06.2091″[2]
Apparent magnitude (V) 7.8 - 11.2[3]
Characteristics
Spectral type B5/8eq+F5/7[4]
B−V color index 1.19[5]
Variable type INA[3]
Astrometry
Radial velocity (Rv)−27±10[5] km/s
Proper motion (μ) RA: −4.839[2] mas/yr
Dec.: +3.831[2] mas/yr
Parallax (π)2.0354 ± 0.6322 mas[2]
Distance640+291
−154[6][7] pc
Details
SE (FU Ori)
Mass3[8] M☉
Radius13[8] R☉
Luminosity1,300[8] L☉
Temperature10,000[8] K
Age0.3[8] Myr
NW (Herbig Ae/Be)
Mass9.43+1.66
−3.62[7] M☉
Radius22.88±8.76[7] R☉
Luminosity2,190+1,700
−1,660[7] L☉
Temperature8,250±183[7] K
Age0.06±0.03[7] Myr
Other designations
Z CMa, BD−11 1760, HD 53179, HIP 34042, PPM 218073, SAO 152302[5]
Database references
SIMBADdata

Z Canis Majoris (Z CMa) is a B-type star in the constellation of Canis Major.[5] It has an average apparent visual magnitude of approximately 10, though has brightened by 1-2 magnitudes in irregular outbursts in 1987, 2000, 2004 and 2008.[9]

The star is a complex binary system only 300,000 years old with two main components separated by an estimated 100 astronomical units (AU) or 0.1" as seen from Earth. The southeast component is an FU Orionis star (a type of pre-main-sequence star in a phase of very high mass accretion resulting in an accretion disk which dominates the optical spectrum) that is 1300 times as luminous as the Sun, has 3 times its mass and 13 times its diameter and a surface temperature of 10,000 K. The northwest component is a Herbig Ae/Be star that has been calculated to be 12 times as massive as the Sun with a dust shell photosphere 1,690±30 times its diameter and a blackbody temperature of 980 K,[10][8] the star shines with a luminosity 2,400 times greater than that of the sun,[8] though there is some uncertainty about its properties. It is enveloped in an irregular roughly spherical cocoon of dust that has an inner diameter of 20 and outer diameter of 50 AU. The cocoon has a hole in it through which light shines that covers an angle of 5 to 10 degrees of its circumference. Both stars are surrounded by a large envelope of in-falling material that left over from the original cloud that formed the system. Both stars are emitting jets of material, that of the Herbig Ae/Be star being much larger - up to 11.7 light-years (3.6 parsecs) long.[11]

It is unclear whether the most recent (and brightest) brightening in 2008 was due to the Herbig Ae/Be star increasing in luminosity or a hole appearing in the cocoon.[11]

References

  1. ^ "ASAS All Star Catalogue". The All Sky Automated Survey. Retrieved 8 December 2021.
  2. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b Z CMa, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars Archived 2017-06-20 at the Wayback Machine, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 9, 2009.
  4. ^ Covino, E.; Terranegra, L.; Vittone, A. A.; Russo, G. (1984). "Spectroscopic and photometric observations of the Herbig be star Z Canis Majoris". The Astronomical Journal. 89: 1868. Bibcode:1984AJ.....89.1868C. doi:10.1086/113697.
  5. ^ a b c d "V* Z CMa". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved November 9, 2009.
  6. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021). "Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. S2CID 228063812.
  7. ^ a b c d e f Guzmán-Díaz, J.; Mendigutía, I.; Montesinos, B.; Oudmaijer, R. D.; Vioque, M.; Rodrigo, C.; Solano, E.; Meeus, G.; Marcos-Arenal, P. (25 June 2021). "Homogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3". Astronomy & Astrophysics. 650: 43. arXiv:2104.11759. Bibcode:2021A&A...650A.182G. doi:10.1051/0004-6361/202039519. ISSN 0004-6361. S2CID 233393918.
  8. ^ a b c d e f g Szeifert, T.; Hubrig, S.; Schöller, M.; Schütz, O.; et al. (2010). "The Nature of the Recent Extreme Outburst of the Herbig Be/FU Orionis Binary Z Canis Majoris". Astronomy and Astrophysics. 509 (L7): 5 pp. arXiv:0912.3889. Bibcode:2010A&A...509L...7S. doi:10.1051/0004-6361/200913704. S2CID 14928968.
  9. ^ Whelan, E.T.; Dougados, C.; Perrin, M. D.; Bonnefoy, M.; et al. (2010). "The 2008 Outburst in the Young Stellar System Z CMa: The First Detection of Twin Jets". The Astrophysical Journal Letters. 720 (1): L119-24. arXiv:1008.0111. Bibcode:2010ApJ...720L.119W. doi:10.1088/2041-8205/720/1/L119. S2CID 119237775.
  10. ^ Thiébaut, E.; Bouvier, J.; Blazit, A.; Bonneau, D.; Foy, F. -C.; Foy, R. (18 April 1995). "The companion of Z Canis Majoris detected in the visible". Astronomy & Astrophysics. 303: 795. Bibcode:1995A&A...303..795T. ISSN 0004-6361.
  11. ^ a b Canovas, H.; Min, M.; Jeffers, S.V.; Rodenhuis, M.; et al. (2012). "Constraining the Circumbinary envelope of Z Canis Majoris via Imaging Polarimetry". Astronomy & Astrophysics. 543 (A70): 8 pp. arXiv:1205.3784. Bibcode:2012A&A...543A..70C. doi:10.1051/0004-6361/201117762. S2CID 53690653.
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