Astronomy:Sigma Puppis

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Short description: Star in the constellation Puppis
Sigma Puppis
Puppis IAU.svg
Red circle.svg
Location of σ Puppis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Puppis
Right ascension  07h 29m 13.83049s[1]
Declination −43° 18′ 05.1597″[1]
Apparent magnitude (V) 3.25[2]
Characteristics
Spectral type K5 III[3]
U−B color index +1.77[2]
B−V color index +1.52[2]
Astrometry
Radial velocity (Rv)+87.7[4] km/s
Proper motion (μ) RA: −59.55[1] mas/yr
Dec.: +188.31[1] mas/yr
Parallax (π)16.84 ± 0.15[1] mas
Distance194 ± 2 ly
(59.4 ± 0.5 pc)
Absolute magnitude (MV)−0.50[5]
Orbit[6]
Period (P)257.8 days
Eccentricity (e)0.17
Periastron epoch (T)20418.6
Argument of periastron (ω)
(secondary)		349.3°
Semi-amplitude (K1)
(primary)		18.6 km/s
Details
σ Pup A
Radius107[7] R☉
Luminosity392[5] L☉
Rotational velocity (v sin i)3.0[8] km/s
Other designations
σ Pup, Sigma Pup, CPD−43  1499, FK5 1194, GC 10040, HD 59717, HIP 36377, HR 2878, SAO 218755, WDS J07292-4318A[9]
Database references
SIMBADdata

Sigma Puppis, Latinized from σ Puppis, is a binary star system in the southern constellation of Puppis. It has an apparent visual magnitude of 3.25,[2] which is bright enough to be visible to the naked eye at night from the Southern Hemisphere. Through a telescope, it appears as a bright, orange-hued star with a nearby white companion.[10] Parallax measurements indicate this star is located at a distance of about 194 light-years (59 parsecs) from Earth.[1]

A light curve for Sigma Puppis, adapted from Otero (2007)[11]

This is a spectroscopic binary system,[9] consisting of an orbiting pair of stars that have not been individually resolved with a telescope. Their orbital period is 257.8 days and the eccentricity is 0.17.[6] The pair form an eclipsing binary of the Beta Lyrae type and a period of 130.5 days, or one half of their orbital period. The eclipse of the primary component causes a decline of 0.04 of a magnitude, while the secondary eclipse reduces the magnitude by 0.03.[11][12]

The combined stellar classification is K5 III,[3] which matches the spectrum of a giant star. The measured angular diameter of the primary star is 16.71 ± 2.84 mas.[13] At the estimated distance of this system, this yields a physical size of about 107 times the radius of the Sun.[7] The primary component shows the behavior of a slow irregular variable.[11][12]

In addition to its binary components, Sigma Puppis has a more distant companion that has a matching proper motion, suggesting that it may be gravitationally bound to the binary. This magnitude 8.5[10] star is at an angular separation of 22.4 arcseconds with a position angle of 74° from Sigma Puppis, which is equivalent to a projected separation of 1,200 astronomical unit|AU.[14] In 1970, American astronomer Olin J. Eggen suggested that Sigma Puppis belonged to a moving group of stars that share a similar motion through space, and thereby a common origin. It served as the eponym for this, the σ Puppis group.[15] The existence of this group was later brought into question.[16]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V 
  2. ↑ 2.0 2.1 2.2 2.3 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. ↑ 3.0 3.1 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, Ann Arbor: Dept. of Astronomy, University of Michigan: distributed by University Microfilms International, Bibcode: 1978mcts.book.....H 
  4. ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, 30, University of Toronto: International Astronomical Union, p. 57, Bibcode: 1967IAUS...30...57E 
  5. ↑ 5.0 5.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  6. ↑ 6.0 6.1 Batten, A. H.; Fletcher, J. M.; Mann, P. J. (1978), "Seventh catalogue of the orbital elements of spectroscopic binary systems", Publications of the Dominion Astrophysical Observatory Victoria 15: 121–295;150–151, Bibcode: 1978PDAO...15..121B 
  7. ↑ 7.0 7.1 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1, https://books.google.com/books?id=OvTjLcQ4MCQC&pg=PA41 . The radius (R*) is given by:
    [math]\displaystyle{ \begin{align} 2\cdot R_* & = \frac{(10^{-3}\cdot 59.4\cdot 16.71)\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 213.5\cdot R_{\bigodot} \end{align} }[/math]
  8. ↑ Costa, J. M. et al. (February 2002), "The tidal effects on the lithium abundance of binary systems with giant component", Astronomy and Astrophysics 382 (3): 1016–1020, doi:10.1051/0004-6361:20011676, Bibcode: 2002A&A...382.1016C 
  9. ↑ 9.0 9.1 "sig Pup -- Spectroscopic binary", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Sigma+Puppis, retrieved 2010-01-05 
  10. ↑ 10.0 10.1 Plotner, Tammy; Mann, Terry (2007), The Night Sky Companion: A Yearly Guide to Sky-Watching, Patrick Moore's Practical Astronomy Series, Springer, p. 156, ISBN 978-0-387-71608-4, https://books.google.com/books?id=f42fFDCTF0MC&pg=PA156, retrieved 2012-01-11 
  11. ↑ 11.0 11.1 11.2 Otero, Sebastián A. (October 2007), "New Elements for 54 Eclipsing Binaries", Open European Journal on Variable Stars 72 (1): 1–19, Bibcode: 2007OEJV...72....1O 
  12. ↑ 12.0 12.1 Samus, N. N.; Durlevich, O. V. (February 12, 2009), GCVS Variability Types and Distribution Statistics of Designated Variable Stars According to their Types of Variability, Sternberg Astronomical Institute, Moscow University, http://www.sai.msu.su/gcvs/gcvs/iii/vartype.txt, retrieved 2012-04-18 
  13. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics 431 (2): 773–777, doi:10.1051/0004-6361:20042039, Bibcode: 2005A&A...431..773R 
  14. ↑ Burnham, Robert (1978), Burnham's celestial handbook: an observer's guide to the universe beyond the solar system, Dover books explaining science, 3 (2nd ed.), Courier Dover Publications, p. 150, ISBN 0-486-23673-0, https://books.google.com/books?id=PJzIt3SIlkUC&pg=PA150, retrieved 2012-01-11 
  15. ↑ Eggen, O. J. (June 1971), "The ζ Herculis, σ Puppis, ∈ Indi, and η Cephei Groups of Old Disk Population Stars", Publications of the Astronomical Society of the Pacific 83 (493): 251, doi:10.1086/129119, Bibcode: 1971PASP...83..251E, https://scholar.archive.org/work/zqy7uehl7rg2xk4ne6nie7wahu/access/wayback/https://iopscience.iop.org/article/10.1086/129119/pdf 
  16. ↑ Taylor, B. J. (October 2000), "A statistical analysis of the metallicities of nine old superclusters and moving groups", Astronomy and Astrophysics 362: 563–579, Bibcode: 2000A&A...362..563T 

Coordinates: Sky map 07h 27m 13.83s, −43° 18′ 05.2″



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