Astronomy:HD 166724
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Corona Australis |
| Right ascension | 18h 13m 59.67590s[1] |
| Declination | –42° 34′ 31.3558″[1] |
| Apparent magnitude (V) | +9.33[2] |
| Characteristics | |
| Spectral type | K0IV/V[3] |
| B−V color index | 0.861±0.032[2] |
| Astrometry | |
| Radial velocity (Rv) | −17.51±0.20[1] km/s |
| Proper motion (μ) | RA: +36.061[1] mas/yr Dec.: –80.180[1] mas/yr |
| Parallax (π) | 22.0344 ± 0.0177[1] mas |
| Distance | 148.0 ± 0.1 ly (45.38 ± 0.04 pc) |
| Absolute magnitude (MV) | 6.20[2] |
| Details[4] | |
| Mass | 0.81±0.02 M☉ |
| Radius | 0.80+0.01 −0.02[5] R☉ |
| Luminosity | 0.388±0.001[5] L☉ |
| Surface gravity (log g) | 4.43±0.08 cgs |
| Temperature | 5,101+50 −41[5] K |
| Metallicity [Fe/H] | −0.09±0.03 dex |
| Age | 4.0±3.8 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| Extrasolar Planets Encyclopaedia | data |
HD 166724 is a star in the southern constellation of Corona Australis. It is invisible to the naked eye with an apparent visual magnitude of +9.33.[2] The star is located at a distance of 148 light-years (45 parsecs) from the Sun based on parallax, but is drifting closer with a radial velocity of −18 km/s.[1] It is predicted to come as close as 97.0 light-years in around 1.2 million years from now.[2] The star has an absolute magnitude of 6.20.[2]
The stellar classification of HD 166724 is K0IV/V,[3] showing blended features of a K-type main-sequence star with a more evolved subgiant star. It is slightly active with chromospheric activity being demonstrated by an emission peak in the Ca II K absorption line.[4] The age of the star is poorly constrained, but it is spinning slowly with a period of around 30 days.[4] It has 81% of the mass of the Sun and 80%[4] of the Sun's girth. The star is radiating 39%[5] of the luminosity of the Sun from its photosphere at an effective temperature of 5,101 K.[4]
Planetary system
From 1998 to 2012, the star was under observance from the CORALIE echelle spectrograph at La Silla Observatory. In 2012, a long-period, wide-orbiting exoplanet was deduced by radial velocity variations. This was published in November. The discoverers noted that HD 166724 b is among "the three most eccentric planets with a period larger than 5 years" alongside HD 98649 b and HD 219077 b; but unlike them, too dim as a candidate for direct imaging with current technology. The reason for this high orbital eccentricity is unknown.[4] In 2023, the inclination and true mass of HD 166724 b were determined via astrometry.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 3.8+0.65 −0.29 MJ |
5.17+0.38 −0.49 |
13.0+1.4 −1.8 |
0.729+0.018 −0.017 |
68+15 −16 or 112+16 −15° |
— |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 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 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 2, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1978mcts.book.....H
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Marmier, M. et al. (2013). "The CORALIE survey for southern extrasolar planets XVII. New and updated long period and massive planets". Astronomy and Astrophysics 551: A90. doi:10.1051/0004-6361/201219639. Bibcode: 2013A&A...551A..90M.
- ↑ 5.0 5.1 5.2 5.3 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.
- ↑ "HD 166724". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+166724.
- ↑ 7.0 7.1 Xiao, Guang-Yao et al. (May 2023). "The Masses of a Sample of Radial-Velocity Exoplanets with Astrometric Measurements". Research in Astronomy and Astrophysics 23 (5): 055022. doi:10.1088/1674-4527/accb7e. Bibcode: 2023RAA....23e5022X.
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