Astronomy:HD 164427
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pavo |
| Right ascension | 18h 04m 42.58968s[1] |
| Declination | −59° 12′ 34.4678″[1] |
| Apparent magnitude (V) | 6.88[2] |
| Characteristics | |
| Spectral type | G0+V[3] |
| B−V color index | 0.624±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | +3.40±0.25[1] km/s |
| Proper motion (μ) | RA: −196.087[1] mas/yr Dec.: −51.219[1] mas/yr |
| Parallax (π) | 23.4516 ± 0.1836[1] mas |
| Distance | 139 ± 1 ly (42.6 ± 0.3 pc) |
| Absolute magnitude (MV) | 3.98±0.06[4] |
| Orbit[5] | |
| Period (P) | 108.53855±0.00033 d |
| Semi-major axis (a) | 0.513+0.015 −0.016 astronomical unit|AU |
| Eccentricity (e) | 0.54944±0.00073 |
| Inclination (i) | 9.340+0.066 −0.058° |
| Longitude of the node (Ω) | 337.69+0.41 −0.49° |
| Periastron epoch (T) | 2457368.358±0.017 |
| Argument of periastron (ω) (secondary) | −3.187+0.078 −0.070° |
| Semi-amplitude (K1) (primary) | 2.2162+0.0028 −0.0031 km/s |
| Details[5] | |
| Mass | 1.19±0.14 M☉ |
| Radius | 1.404±0.037 R☉ |
| Luminosity | 2.66+0.48 −0.34 L☉ |
| Surface gravity (log g) | 4.216+0.062 −0.069 cgs |
| Temperature | 6,220+310 −240 K |
| Metallicity [Fe/H] | −0.06+0.22 −0.25 dex |
| Age | 6.6+1.3 −0.9[4] Gyr |
| HD 164427 B | |
| Mass | 0.339+0.002 −0.003 M☉ |
| Mass | 355.5+2.6 −2.9 MJup |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 164427 is a star with a likely red dwarf companion in the southern constellation of Pavo. It has an apparent visual magnitude of 6.88,[2] placing it just below the nominal limit for visibility with the typical naked eye. The annual parallax shift of 23.5 mas[1] yields a distance estimate of 139 light-years (43 parsecs). It is moving further from the Earth with a heliocentric radial velocity of +3.4 km/s.[1]
This is an inactive[7] G-type main-sequence star given a stellar classification of G0+V by Gray et al. (2006),[3] although Evans et al. (1964) classified it as a subgiant star with luminosity class IV.[7] It is 6.6 billion years old with 1.125 times the mass of the Sun and 1.40 times the Sun's radius.[8] The star is somewhat over-luminous for its class,[7] radiating 2.33[2] times the Sun's luminosity from its photosphere at an effective temperature of 5,876 K.[3]
Companions
In 2001, a brown dwarf candidate companion was announced by Anglo-Australian Planet Search program. It was detected by the Doppler velocity technique with an echelle spectrograph attached to the 3.92m Anglo-Australian Telescope.[7] A magnitude 12.60 companion star designated HD 164427 B lies at an angular separation of 28.90″ along a position angle of 336°, as of 2010.[9] This is a suspected common proper motion companion with 52% of the Sun's mass[10] and a physical separation of as much as 1,090 astronomical unit|AU.[7]
HD 164427 b was initially thought to be a brown dwarf based on its minimum mass of 46 times that of Jupiter.[7] In 2023, an astrometric orbit for this object was published using data from Gaia, showing its true mass to be 0.34 M☉, making it a likely red dwarf star.[5] This stellar companion orbits at nearly half an astronomical unit or Earth-to-Sun distance away from its primary. The angular separation between the two stars as viewed from Earth is 11.76 milliarcseconds. It takes 108.55 Earth days to orbit eccentrically around HD 164427. It has a very high semi-amplitude of almost 1400 m/s, because this is a very massive object which exerts strong gravitational pull on its tugging star.[7]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 3.2 Gray, R. O. et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal 132 (1): 161–170. doi:10.1086/504637. Bibcode: 2006AJ....132..161G.
- ↑ 4.0 4.1 Holmberg, J. et al. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics Supplement Series 501 (3): 941–947. doi:10.1051/0004-6361/200811191. Bibcode: 2009A&A...501..941H.
- ↑ 5.0 5.1 5.2 Unger, N. et al. (December 2023). "Exploring the brown dwarf desert with precision radial velocities and Gaia DR3 astrometric orbits". Astronomy & Astrophysics 680: A16. doi:10.1051/0004-6361/202347578. Bibcode: 2023A&A...680A..16U.
- ↑ "HD 164427". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+164427.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 Tinney, C. G. et al. (2001). "First Results from the Anglo-Australian Planet Search: A Brown Dwarf Candidate and a 51 Peglike Planet". The Astrophysical Journal 551 (1): 507–511. doi:10.1086/320097. Bibcode: 2001ApJ...551..507T. http://www.iop.org/EJ/article/0004-637X/551/1/507/53098.html.
- ↑ Takeda, Genya et al. (February 2007). "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog". The Astrophysical Journal Supplement Series 168 (2): 297–318. doi:10.1086/509763. Bibcode: 2007ApJS..168..297T.
- ↑ Mason, B. D. et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M.
- ↑ Tokovinin, Andrei (April 2014). "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs". The Astronomical Journal 147 (4): 14. doi:10.1088/0004-6256/147/4/87. 87. Bibcode: 2014AJ....147...87T.
External links
- "NLTT 45831 -- High proper-motion Star". SIMBAD. http://simbad.u-strasbg.fr/simbad/sim-id?protocol=html&Ident=HD+164427&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. Retrieved December 21, 2007.
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