Nu Puppis
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Puppis |
| Right ascension | 06h 37m 45.67135s[1] |
| Declination | −43° 11′ 45.3602″[1] |
| Apparent magnitude (V) | 3.173[2] |
| Characteristics | |
| Spectral type | B8 III[3] |
| U−B color index | −0.397[2] |
| B−V color index | −0.113[2] |
| Astrometry | |
| Radial velocity (Rv) | +30.9[4] km/s |
| Proper motion (μ) | RA: −0.44[1] mas/yr Dec.: −3.87[1] mas/yr |
| Parallax (π) | 8.78±0.26 mas[1] |
| Distance | 370 ± 10 ly (114 ± 3 pc) |
| Absolute magnitude (MV) | −2.11[5] |
| Details | |
| Mass | 2.84[6] M☉ |
| Radius | 6.8 (equatorial) 5.8 (polar)[7] R☉ |
| Luminosity | 800[7] L☉ |
| Surface gravity (log g) | 2.9 (equatorial) 3.4 (polar)[7] cgs |
| Temperature | 10,000 (equatorial) 13,060 (polar)[7] K |
| Rotational velocity (v sin i) | 225[8] km/s |
| Age | 234[9] Myr |
| Other designations | |
| ν Pup, CPD−43°946, HD 47670, HIP 31685, HR 2451, SAO 218071[10] | |
| Database references | |
| SIMBAD | data |
Nu Puppis (ν Puppis), also named Pipit,[11] is a solitary,[12] blue-hued star in the southern constellation of Puppis. It is the fifth-brightest star in Puppis, with an apparent visual magnitude of 3.17.[2] Based upon an annual parallax shift of 8.78 mas as seen from Earth,[1] it is located about 370 light years from the Sun. The system made its closest approach about 3.6 million years ago when it underwent perihelion passage at a distance of roughly 27 light years.[13]
The star has a stellar classification of B8 III,[3] matching a B-type giant. Absorption lines in the spectrum are displaying central quasi-emission peaks, indicating this is a Be shell star with a circumstellar disk of heated gas that is being seen edge-on.[14] ν Puppis is a candidate variable star showing an amplitude of 0.0117 magnitude with a frequency of 0.15292 per day.[15] It is spinning rapidly with a projected rotational velocity of 225 km/s. This rotation is giving the star an oblate shape, with the equator being 17% larger than the poles. Similarly, the effective temperature and surface gravity vary across latitudes. The star's equatorial radius, temperature and surface gravity are estimated at 6.8 R☉, 10,000 K and 2.9 cgs, while the polar radius, temperature and surface gravity are 5.8 R☉, 13,000 K and 3.4 cgs.[7]
Among the Kendayan people of West Kalimantan province, Indonesia, this star is known as Pipit. The IAU Working Group on Star Names approved the name Pipit for this star on 25 August 2024 and it is now so entered in the IAU Catalog of Star Names.[11]
References
[edit]- ^ a b c d e f 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.
- ^ a b c d Cousins, A. W. J. (1973), "Revised zero points and UBV photometry of stars in the Harvard E and F regions", Memoirs of the Royal Astronomical Society, 77: 223–236, Bibcode:1973MmRAS..77..223C.
- ^ a b Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 2, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
- ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
- ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ Khalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G.; Valentini, M.; Torralba Elipe, G.; Steinmetz, M.; Pantaleoni-González, M.; Malhotra, S.; Jiménez-Arranz, Ó.; Enke, H.; Casamiquela, L.; Ardèvol, J. (2024), "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost", Astronomy and Astrophysics, 691: A98, arXiv:2407.06963, Bibcode:2024A&A...691A..98K, doi:10.1051/0004-6361/202451427.
- ^ a b c d e Baade, D.; Pigulski, A.; Rivinius, Th; Wang, L.; Martayan, Ch; Handler, G.; Panoglou, D.; Carciofi, A. C.; Kuschnig, R.; Mehner, A.; Moffat, A. F. J.; Pablo, H.; Rucinski, S. M.; Wade, G. A.; Weiss, W. W. (2018-12-01), "Short-term variability and mass loss in Be stars - IV. Two groups of closely spaced, approximately equidistant frequencies in three decades of space photometry of ν Puppis (B7-8 IIIe)", Astronomy & Astrophysics, 620: A145, doi:10.1051/0004-6361/201834161, ISSN 0004-6361.
- ^ Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
- ^ Gontcharov, G. A. (2012), "Dependence of kinematics on the age of stars in the solar neighborhood", Astronomy Letters, 38 (12): 771, arXiv:1606.08814, Bibcode:2012AstL...38..771G, doi:10.1134/S1063773712120031.
- ^ "nu. Pup", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-07-19.
- ^ a b IAU Catalog of Star Names, retrieved 22 February 2025.
- ^ 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.
- ^ 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.
- ^ Rivinius, Th.; et al. (August 1999), "Central quasi-emission peaks in shell spectra and the rotation of disks of Be stars", Astronomy and Astrophysics, 348: 831–842, Bibcode:1999A&A...348..831R.
- ^ 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.
