171 G. Puppis

In today's world, 171 G. Puppis is a relevant topic that has captured the attention of society in general. Its impact has been felt in different aspects of daily life, generating debates, reflections and significant changes in various areas. As 171 G. Puppis continues to be a focus of interest and controversy, it is essential to fully analyze its implications and consequences, as well as explore possible solutions and paths forward. In this article, we will delve into the fascinating world of 171 G. Puppis, exploring its roots, its current dimensions and its possible evolution in the future.

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 mas[1]
Distance49.6 ± 0.4 ly
(15.2 ± 0.1 pc)
Absolute magnitude (MV)+4.57[5]
Details
171 Pup A
Mass0.81[6] M☉
Surface gravity (log g)4.24[6] cgs
Temperature5,852[6] K
Metallicity −0.81[6] dex
Rotational velocity (v sin i)4.4[5] km/s
Other designations
CD−33°4113, GJ 288, HD 63077, HIP 37853, HR 3018, SAO 198404[7]
Database references
SIMBADAB
A
B
ARICNSA
B

171 G. 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. ^ a b c d e 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.
  2. ^ a b c Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ 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, S2CID 119476992.
  4. ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
  5. ^ a b Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  6. ^ a b c d 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, S2CID 118786105.
  7. ^ "171 Pup -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-08-11.
  8. ^ 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, S2CID 30955275, 7.
  9. ^ 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, S2CID 118586009, 56.
  10. ^ 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, arXiv:1307.8047, Bibcode:2013MNRAS.435.2077H, doi:10.1093/mnras/stt1433.