Astronomy:HD 217786
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pisces |
| Right ascension | 23h 03m 08.20704s[1] |
| Declination | −00° 25′ 46.6777″[1] |
| Apparent magnitude (V) | 7.78[2] |
| Characteristics | |
| Spectral type | F8V[3] |
| B−V color index | 0.578±0.004[2] |
| Astrometry | |
| Radial velocity (Rv) | +10.00±0.02[2] km/s |
| Proper motion (μ) | RA: −89.933[1] mas/yr Dec.: −168.781[1] mas/yr |
| Parallax (π) | 17.9946 ± 0.0793[1] mas |
| Distance | 181.3 ± 0.8 ly (55.6 ± 0.2 pc) |
| Absolute magnitude (MV) | 4.09[2] + 11.02±0.13[4] |
| Details[5] | |
| A | |
| Mass | 1.02 M☉ |
| Radius | 1.32±0.06 R☉ |
| Luminosity | 1.93±0.04[6] L☉ |
| Surface gravity (log g) | 4.13±0.02 cgs |
| Temperature | 5,882±8[7] K |
| Metallicity | −0.19±0.01 |
| Rotational velocity (v sin i) | 1.18±0.05 km/s |
| Age | 9.40±0.22 Gyr |
| HD 217786 B | |
| Mass | 0.1622+0.0071 −0.0068[4] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 217786 is a binary star[4] system in the equatorial constellation of Pisces. With an apparent visual magnitude of 7.78,[2] it requires binoculars or a small telescope to view. The system is located at a distance of 181 light-years from the Sun based on parallax, and is drifting further away with a radial velocity of +10 km/s.[2] Kinematically, the star system belongs to the thin disk population of the Milky Way.[7]
The primary is an F-type main-sequence star with a stellar classification of F8V. It is much older than Sun with an estimated age of 9.4 billion years and is spinning slowly with a projected rotational velocity of 1.2 km/s. The star has a lower proportion of heavy elements than the Sun, having 65% of solar abundance.[7] It has about the same mass as the Sun but a 32% larger radius.[5] The star is radiating nearly double[6] the luminosity of the Sun from its photosphere at an effective temperature of 5,882 K.[7]
A low-mass stellar companion at a projected separation of 155 AU was discovered in 2016.[4] The proper motion of this co-moving object suggests it is gravitationally-bound to the primary, and their orbit is being viewed edge-on. If the orbit is assumed to be circular, then the orbital period for the pair is ~6.2 Myr.[4] No other companion stars have been detected at separations from 2.74 to 76.80 AUs.[6]
The star system exhibits strong stellar flare activity in the ultraviolet.[9]
Planetary system
In 2010 one superjovian planet or brown dwarf on an eccentric orbit was discovered utilising the radial velocity method.[10] Designated component Ab, the high eccentricity of this object may have been caused by interaction with the secondary star.[4] In 2022, the inclination and true mass of HD 217786 Ab were measured via astrometry, and a second planet was discovered orbiting closer to the star.[11]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | ≥0.023±0.002 MJ | 0.038±0.002 | 2.5+0.00010 −0.00005 |
— | — | — |
| b | 13.852+1.267 −1.311 MJ |
2.446+0.109 −0.119 |
1,301.4+1.2 −0.5 |
0.311+0.002 −0.003 |
69.767+0.601 −0.386° |
— |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 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 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
- ↑ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey 5, Bibcode: 1999MSS...C05....0H
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Ginski, C. et al. (2016), "A lucky imaging multiplicity study of exoplanet host stars – II", Monthly Notices of the Royal Astronomical Society 457 (2): 2173–2191, doi:10.1093/mnras/stw049, Bibcode: 2016MNRAS.457.2173G
- ↑ 5.0 5.1 Quarles, Billy; Li, Gongjie; Kostov, Veselin; Haghighipour, Nader (2020), "Orbital Stability of Circumstellar Planets in Binary Systems", The Astronomical Journal 159 (3): 80, doi:10.3847/1538-3881/ab64fa, Bibcode: 2020AJ....159...80Q
- ↑ 6.0 6.1 6.2 Wittrock, Justin M.; Kane, Stephen R.; Horch, Elliott P.; Howell, Steve B.; Ciardi, David R.; Everett, Mark E. (2017), "Exclusion of Stellar Companions to Exoplanet Host Stars", The Astronomical Journal 154 (5): 184, doi:10.3847/1538-3881/aa8d69, Bibcode: 2017AJ....154..184W
- ↑ 7.0 7.1 7.2 7.3 Maldonado, J.; Villaver, E. (2017), "Searching for chemical signatures of brown dwarf formation", Astronomy & Astrophysics 602: A38, doi:10.1051/0004-6361/201630120, Bibcode: 2017A&A...602A..38M
- ↑ "HD 217786". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+217786.
- ↑ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal 766 (1): 9, doi:10.1088/0004-637X/766/1/9, Bibcode: 2013ApJ...766....9S
- ↑ Moutou, Claire; Mayor, Michel; Lo Curto, Gaspare; Ségransan, Damien; Udry, Stéphane; Bouchy, François; Benz, Willy; Lovis, Christophe et al. (2010), The HARPS search for southern extra-solar planets: XXVI: Seven new planetary systems, doi:10.1051/0004-6361/201015371
- ↑ 11.0 11.1 Feng, Fabo et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series 262 (21): 21. doi:10.3847/1538-4365/ac7e57. Bibcode: 2022ApJS..262...21F.
Coordinates: 
23h 03m 08.2070s, −00° 25′ 46.6777″
 |  |
