Astronomy:171 G. Puppis

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Short description: Star in the constellation Puppis
171 G. Puppis
Observation data
{{#ifeq:J2000.0|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| [[History:Epoch|Epoch J2000.0]]      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0}}
Constellation Puppis
A
Right ascension  07h 45m 35.02168s[1]
Declination −34° 10′ 20.5143″[1]
Apparent magnitude (V) 5.38[2]
B
Right ascension  07h 45m 38.42749s[3]
Declination −33° 55′ 51.3414″[3]
Apparent magnitude (V) 16.7[4]
Characteristics
A
Evolutionary stage Subgiant[5]
Spectral type F9 V[6]
U−B color index −0.085[2]
B−V color index +0.56[2]
Astrometry
A
Radial velocity (Rv)+102.6[7] km/s
Proper motion (μ) RA: −221.54[1] mas/yr
Dec.: +1,722.11[1] mas/yr
Parallax (π)65.75 ± 0.51[1] mas
Distance49.6 ± 0.4 ly
(15.2 ± 0.1 pc)
Absolute magnitude (MV)+4.57[8]
Orbit[9]
PrimaryAa
CompanionAb
Period (P)8,406+29
−7 days
Semi-major axis (a)9.15+0.31
−0.33 astronomical unit|AU
Eccentricity (e)0.443+0.002
−0.001
Argument of periastron (ω)
(secondary)		184.38+0.16
−0.17°
Semi-amplitude (K1)
(primary)		4.762±0.013 km/s
Details
Aa
Mass0.85[10] M☉
Radius1.13+0.10
−0.09[9] R☉
Luminosity1.80+0.49
−0.28[9] L☉
Surface gravity (log g)4.34+0.07
−0.09[9] cgs
Temperature5,858±70[10] K
Metallicity [Fe/H]−0.78±0.06[10] dex
Rotational velocity (v sin i)4.4[8] km/s
Ab
Mass≥0.42±0.03[9] M☉
B
Mass0.507±0.007[11] M☉
Radius0.0135[11][lower-alpha 1] R☉
Luminosity6.2×10−5[11] L☉
Surface gravity (log g)7.882±0.008[11] cgs
Temperature4,405±15[11] K
Other designations
GJ 288, HD 63077, HR 3018[12]
A: CD−33°4113, HIP 37853, HR 3018, SAO 198404
B: VB 3, WD 0743-336
Database references
SIMBADA
B
ARICNSA
B

171 G. Puppis (171 Pup) is a triple[13] 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 23 years. The orbit has a semi-major axis of 9.15 AU and a mild eccentricity of 0.443.[9] The primary has a spectral class of F9V,[6] matching a late F-type main-sequence star. However, stellar evolution models suggest it has left the main sequence and is now a subgiant.[5][14] Little is known about the secondary, but its mass should be at least 0.42 M☉.[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 with a classification of DC11.0 and a temperature of 4,600 K, making it one of the coolest white dwarfs known.[15]

171 G. Puppis is believed to be among the oldest star systems in the solar neighbourhood, being of the Population II. The primary's metal-to-hydrogen ratio is a logarithm of −0.78, translating to 16% of the Sun's abundance.[10] In the early universe, the metallicity of the interstellar medium was much lower than that of the current universe.[16]

Notes

  1. ↑ Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:(5,7724,405)4⋅10−4.2076=0.0135 R⊙.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 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. ↑ 3.0 3.1 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ Tokovinin, Andrei (2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series 235 (1): 6. doi:10.3847/1538-4365/aaa1a5. Bibcode: 2018ApJS..235....6T. 
  5. ↑ 5.0 5.1 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  6. ↑ 6.0 6.1 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, doi:10.1086/504637, Bibcode: 2006AJ....132..161G. 
  7. ↑ 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, pp. 57, Bibcode: 1967IAUS...30...57E. 
  8. ↑ 8.0 8.1 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, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 9.6 Barbato, D.; Ségransan, D.; Udry, S.; Unger, N.; Bouchy, F.; Lovis, C.; Mayor, M.; Pepe, F. et al. (2023-06-01), "The CORALIE survey for southern extrasolar planets - XIX. Brown dwarfs and stellar companions unveiled by radial velocity and astrometry" (in en), Astronomy & Astrophysics 674: A114, doi:10.1051/0004-6361/202345874, ISSN 0004-6361, Bibcode: 2023A&A...674A.114B.  171 Pup A's database entry at VizieR.
  10. ↑ 10.0 10.1 10.2 10.3 Fuhrmann, Klaus; Chini, Rolf (2021-03-11), "On ancient solar-type stars – II", Monthly Notices of the Royal Astronomical Society 501 (4): 4903–4916, doi:10.1093/mnras/staa3942, ISSN 0035-8711. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 Vincent, O.; Barstow, M. A.; Jordan, S.; Mander, C.; Bergeron, P.; Dufour, P. (2024-01-26), "Classification and parameterization of a large Gaia sample of white dwarfs using XP spectra" (in en), Astronomy & Astrophysics 682: A5, doi:10.1051/0004-6361/202347694, ISSN 0004-6361, Bibcode: 2024A&A...682A...5V. 
  12. ↑ "171 Pup -- Double or multiple star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+63077, retrieved 2016-08-11. 
  13. ↑ Tokovinin, Andrei et al. (July 2012), "Revealing Companions to Nearby Stars with Astrometric Acceleration", The Astronomical Journal 144 (1): 10, doi:10.1088/0004-6256/144/1/7, 7, Bibcode: 2012AJ....144....7T. 
  14. ↑ "20.2.1 astrophysical_parameters‣ 20.2 Astrophysical parameter tables ‣ Chapter 20 Datamodel description ‣ Part V Gaia archive ‣ Gaia Data Release 3 Documentation release 1.3". https://gea.esac.esa.int/archive/documentation/GDR3/Gaia_archive/chap_datamodel/sec_dm_astrophysical_parameter_tables/ssec_dm_astrophysical_parameters.html#astrophysical_parameters-evolstage_flame. 
  15. ↑ 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, doi:10.1093/mnras/stt1433, Bibcode: 2013MNRAS.435.2077H. 
  16. ↑ "Populations I and II | Definition, Examples, & Facts | Britannica" (in en). https://www.britannica.com/science/Population-I. 



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