Omicron Puppis

Omicron Puppis
Location of ο Puppis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Puppis
Right ascension 07h 48m 05.16839s[1]
Declination −25° 56′ 13.8123″[1]
Apparent magnitude (V) +4.48[2]
Characteristics
Spectral type B1 IVnne[3]
U−B color index −1.02[2]
B−V color index −0.09[2]
Variable type LERI
Astrometry
Radial velocity (Rv)+15.0[4] km/s
Proper motion (μ) RA: −10.09[1] mas/yr
Dec.: +4.26[1] mas/yr
Parallax (π)2.30 ± 0.23 mas[1]
Distance1,400 ± 100 ly
(430 ± 40 pc)
Absolute magnitude (MV)−3.77[5]
Orbit[6]
Period (P)28.903±0.004 d
Eccentricity (e)0
Periastron epoch (T)2456012.93 ± 0.04
Semi-amplitude (K2)
(secondary)		159.7±11.7 km/s
Details
Mass15.5±0.8[7] M☉
Luminosity (bolometric)59,279[8] L☉
Temperature24,200[8] K
Rotational velocity (v sin i)315[9] km/s
Age11.1±0.5[7] Myr
Other designations
ο Pup, CPD−25° 2882, HD 63462, HIP 38070, HR 3045, SAO 174558, WDS J07481-2556A[10]
Database references
SIMBADdata

Omicron Puppis (ο Puppis) is candidate binary star[6] system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48.[2] Based upon an annual parallax shift of 2.30 mas as seen from Earth,[1] it is located roughly 1,400 light years from the Sun.

This is a suspected close spectroscopic binary system. The spectrum varies with a periodicity of 28.9 days, and a helium emission component shows a radial velocity variation that matches the period. The properties indicate it may be a φ Per-like system with a Be star primary and a hot subdwarf companion of type sdO. If this is the case, then the pair have a circular orbit with a period that matches the variability. The close-orbiting pair may have undergone interaction in the past, leaving the subdwarf stripped down and the primary star spinning rapidly.[6]

A light curve for Omicron Puppis, plotted from TESS data.[11] The 2.0651 day period[12] is shown in red.

ο Puppis is slightly variable. The General Catalogue of Variable Stars lists it as a possible Be star with a magnitude range of 4.43 - 4.46.[13] The International Variable Star Index classifies it as a Lambda Eridani variable.[12]

  1. ^ a b c d e f Cite error: The named reference vanLeeuwen2007 was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference Feinstein1979 was invoked but never defined (see the help page).
  3. ^ Cite error: The named reference Hiltner1969 was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference Kharchenko2007 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Anderson2012 was invoked but never defined (see the help page).
  6. ^ a b c Cite error: The named reference Koubsky2012 was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Tetzlaff2011 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference hohle2010 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Abt2002 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference MAST was invoked but never defined (see the help page).
  12. ^ a b Cite error: The named reference vsx was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference gcvs2009 was invoked but never defined (see the help page).