171 G. Puppis
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Puppis |
| Right ascension | 07h 45m 35.02168s[1] |
| Declination | –34° 10′ 20.5143″[1] |
| Apparent magnitude (V) | 5.38[2] |
| Characteristics | |
| Spectral type | F9 V[3] |
| U−B color index | −0.085[2] |
| B−V color index | +0.56[2] |
| Astrometry | |
| Radial velocity (Rv) | +102.6[4] km/s |
| Proper motion (μ) | RA: +10.32[1] mas/yr Dec.: −124.46[1] mas/yr |
| Parallax (π) | 65.75 ± 0.51[1] mas |
| Distance | 49.6 ± 0.4 ly (15.2 ± 0.1 pc) |
| Details | |
| 171 Puppis A | |
| Mass | 0.81[5] M☉ |
| Surface gravity (log g) | 4.24[5] cgs |
| Temperature | 5,852[5] K |
| Metallicity [Fe/H] | −0.81[5] dex |
| Rotational velocity (v sin i) | 4.4[6] km/s |
| Other designations | |
171 Puppis (171 Pup) is a triple[8] star system in the constellation of Puppis – the stern of Argo Navis – of apparent magnitude +5.38. Lacking a Bayer designation, it is instead known by its Gould designation. Based upon parallax measurements, the system is 49.6 light years away from the Solar System.
The inner pair form a spectroscopic binary with an orbital period of around 10 years. In 2011, they had an angular separation of 309.8±1.6 mas along a position angle of 72.1°.[9] There is a common proper motion companion, Van Biesbroeck 3 or WD 0743-340, at an angular separation of 869.65″ along a position angle of 2.81° from the inner pair. This is a white dwarf star with a classification of DC11.0 and a temperature of 4,600 K, making it one of the coolest white dwarfs known.[10]
References
- 1 2 3 4 5 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. - 1 2 3 Mermilliod, J.-C. (1986), Compilation of Eggen's UBV data, transformed to UBV (unpublished), SIMBAD, Bibcode:1986EgUBV........0M.
- ↑ Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637.
- ↑ 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.
- 1 2 3 4 Bensby, T.; et al. (2014), "Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood", Astronomy & Astrophysics, 562 (A71): 28, arXiv:1309.2631, Bibcode:2014A&A...562A..71B, doi:10.1051/0004-6361/201322631.
- ↑ Ammler-von Eiff, M.; Reiners, A. (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, A116.
- ↑ "171 Pup -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-08-11.
- ↑ Tokovinin, Andrei; et al. (July 2012), "Revealing Companions to Nearby Stars with Astrometric Acceleration", The Astronomical Journal, 144 (1): 10, arXiv:1204.4206, Bibcode:2012AJ....144....7T, doi:10.1088/0004-6256/144/1/7, 7.
- ↑ Tokovinin, Andrei (August 2012), "Speckle Interferometry and Orbits of "Fast" Visual Binaries", The Astronomical Journal, 144 (2): 11, arXiv:1206.1882, Bibcode:2012AJ....144...56T, doi:10.1088/0004-6256/144/2/56, 56.
- ↑ Holberg, J. B.; et al. (November 2013), "Where are all the Sirius-like binary systems?", Monthly Notices of the Royal Astronomical Society, 435 (3): 2077−2091, Bibcode:2013MNRAS.435.2077H, doi:10.1093/mnras/stt1433.
This article is issued from Wikipedia - version of the 8/12/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.