Zeta Puppis

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Zeta Puppis
Zeta Puppis.png
Artistic depiction of Zeta Puppis (Naos).
Observation data
Epoch J2000      Equinox J2000
Constellation Puppis
Right ascension 08h 03m 35.1s[1]
Declination −40° 00′ 11.6″[1]
Apparent magnitude (V) 2.21
Characteristics
Spectral type O4If(n)p[2]
U−B color index −1
B−V color index −0.27
Astrometry
Proper motion (μ) RA: −30.82[1] mas/yr
Dec.: 16.77[1] mas/yr
Parallax (π) 3.00 ± 0.10 mas
Distance 1,090 ± 40 ly
(330 ± 10 pc)
Absolute magnitude (MV) -5.5
Details
Mass 22.5[3] M
Radius 14[3] R
Luminosity (bolometric) 550,000[3] L
Surface gravity (log g) 3.5[4] cgs
Temperature 42,000[3] K
Metallicity [Fe/H] 0.34[5] dex
Rotational velocity (v sin i) >220[5] km/s
Age 2+[3] Myr
Other designations
Naos, Suhail Hadar, ζ Puppis, ζ Pup, Zeta Pup, CPD−39  2011, CPD−39  2111, FK5 306, GC 10947, HD 66811, HIP 39429, HR 3165, PPM 312524, SAO 198752.
Database references
SIMBAD data

Zeta Puppis (Zeta Pup, ζ Puppis, ζ Pup) is a star in the constellation of Puppis. It is also known by the traditional names Naos (/ˈn.ɒs/, from the Greek ναύς "ship") and Suhail Hadar (سهيل هدار, possibly "roaring bright one") in Arabic.

Its spectral class is O4If, making it an exceptionally hot star, and it is one of the sky's few naked-eye class O-type stars as well as one of the closest to Earth.[3] It had been assumed to be part of the Vela complex near the Gum nebula over 400 parsecs from Earth, but the 2008 reduction of Hipparcos data gave a distance of 335 parsecs (1,093 ly) ± 4%.[6] Its surface temperature is 42,000 K . The current mass is calculated at 22.5 solar masses and the radius at 14 times the solar radius but these values are highly uncertain. Older derivations assumed the larger distance and were correspondingly larger, but some new calculations still give values up to twice these.[5]

Zeta Puppis is an extreme blue supergiant, one of the most luminous stars in the Milky Way. Visually, it is 12,500 times more powerful than the Sun, but being an extreme blue star, most of its radiation is in the ultraviolet and hence its bolometric luminosity is over 500,000 times that of the sun. It is also the 62nd brightest star in terms of apparent magnitude from Earth

Zeta Puppis, being typical of O-type stars, is also notable for its extremely strong stellar wind, and it has garnered increasing attention for this over the past decade. Its stellar wind velocity has been estimated at 2,500 km/s,[7] which sees the star shed more than a millionth of its mass each year,[7] or about 10 million times that shed by our own Sun over a comparable time period. This mass ejection is highly evident in non-visible wavelengths such as radio and X-ray.


Origin[edit]

It was long thought that Zeta Puppis was associated with the Vela star-forming region about 1400 light years distant. However the parallax obtained in 2008 from the revision of Hipparcos data (see above) shows that the star is closer. The new distance combined with the known radial velocity show that it encountered the Trumpler 10 OB association around 2 million years ago.[3] It appears not to have originated there since Trumpler 10 has a well established age in excess of 30 million years while Zeta Puppis is no more than a tenth that age. Others theories include the idea that Zeta Puppis was the companion of the star that went supernova and produced the Gum Nebula,[8] but evidence supporting this is sparse.[9] It also shows a common feature of runaways, an anomalously high rotational velocity of 220 km/s at the equator[7] as well as an apparent enrichment in helium and nitrogen on the surface.[5]

Helium[edit]

In 1896, Edward C. Pickering observed mysterious spectral lines from ζ Puppis, which fit the Rydberg formula if half-integers were used instead of whole integers. It was later found that these were due to ionized helium.[10]

Namesakes[edit]

USS Naos (AK-105) was a United States Navy Crater class cargo ship named after the star.

References[edit]

  1. ^ a b c d "SIMBAD Query Result". Results for NAOS. Retrieved 2012-08-05. 
  2. ^ Sota, A.; Maíz Apellániz, J.; Walborn, N. R.; Alfaro, E. J.; Barbá, R. H.; Morrell, N. I.; Gamen, R. C.; Arias, J. I. (2011). "The Galactic O-Star Spectroscopic Survey. I. Classification System and Bright Northern Stars in the Blue-Violet at R ∼ 2500". The Astrophysical Journal Supplement Series 193 (2): 24. arXiv:1101.4002. Bibcode:2011ApJS..193...24S. doi:10.1088/0067-0049/193/2/24.  edit
  3. ^ a b c d e f g Schilbach, E.; Röser, S. (2008). "On the origin of field O-type stars". Astronomy and Astrophysics 489: 105. arXiv:0806.0762. Bibcode:2008A&A...489..105S. doi:10.1051/0004-6361:200809936.  edit
  4. ^ Underhill, A. B. et al. (November 1979). "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars". Monthly Notices of the Royal Astronomical Society 189: 601–605. Bibcode:1979MNRAS.189..601U 
  5. ^ a b c d Dany Vanbeveren (2011). "Zeta Pup: The merger of at least two massive stars". arXiv:1109.6497v1 [astro-ph.GA].
  6. ^ Maíz Apellániz, J.; Alfaro; Sota; Alfaro, E. J.; Sota, A. (2008). Accurate distances to nearby massive stars with the new reduction of the Hipparcos raw data 0804. p. 2553. arXiv:0804.2553. Bibcode:2008arXiv0804.2553M. 
  7. ^ a b c Eversberg, T.; Lepine, S.; Moffat, A. F. J. (1998). "Outmoving Clumps in the Wind of the Hot O Supergiant ζ Puppis". The Astrophysical Journal 494 (2): 799. Bibcode:1998ApJ...494..799E. doi:10.1086/305218.  edit
  8. ^ Woermann, B.; Gaylard, M. J.; Otrupcek, R. (2001). "Kinematics of the Gum nebula region". Monthly Notices of the Royal Astronomical Society 325 (3): 1213. doi:10.1046/j.1365-8711.2001.04558.x.  edit
  9. ^ Choudhury, R.; Bhatt, H. C. (2009). "Kinematics of the young stellar objects associated with the cometary globules in the Gum Nebula". Monthly Notices of the Royal Astronomical Society 393 (3): 959. arXiv:0811.4389. Bibcode:2009MNRAS.393..959C. doi:10.1111/j.1365-2966.2008.14189.x.  edit
  10. ^ Bohr, N. (1913). "The Spectra of Helium and Hydrogen". Nature 92 (2295): 231. doi:10.1038/092231d0.  edit