 ψ Draconis in optical light | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| ψ Dra A | |
| Right ascension | 17 41 56.35536 |
| Declination | +72° 08′ 55.8481″ |
| Apparent magnitude (V) | 4.58 |
| ψ Dra B | |
| Right ascension | 17 41 58.10460 |
| Declination | +72° 09′ 24.8581″ |
| Apparent magnitude (V) | 5.82 |
| Characteristics | |
| ψ Dra A | |
| Spectral type | F5IV-V |
| U−B color index | +0.01 |
| B−V color index | +0.43 |
| ψ Dra B | |
| Spectral type | F8V |
| U−B color index | +0.04 |
| B−V color index | +0.525 |
| Astrometry | |
| ψ Dra A | |
| Radial velocity (Rv) | -13.30 ± 0.2 km/s |
| Proper motion (μ) | RA: 25.32 mas/yr Dec.: -268.47 mas/yr |
| Parallax (π) | 43.79 ± 0.45 mas |
| Distance | 74.5 ± 0.8 ly (22.8 ± 0.2 pc) |
| ψ Dra B | |
| Radial velocity (Rv) | -11.20 ± 0.3 km/s |
| Proper motion (μ) | RA: 34.89 mas/yr Dec.: -275.94 mas/yr |
| Parallax (π) | 43.36 ± 0.51 mas |
| Distance | 75.2 ± 0.9 ly (23.1 ± 0.3 pc) |
| Orbit | |
| Primary | ψ Dra Aa |
| Companion | ψ Dra Ab |
| Period (P) | 6774+271 −167 d |
| Semi-major axis (a) | 9.1+0.4 −0.3 AU |
| Eccentricity (e) | 0.679+0.006 −0.004 |
| Inclination (i) | 31 ± 1° |
| Periastron epoch (T) | 2450388+169 −273 |
| Argument of periastron (ω) (secondary) | 32.6 ± 0.7° |
| Semi-amplitude (K1) (primary) | 5.18+0.04 −0.03 km/s |
| Semi-amplitude (K2) (secondary) | 11.1 ± 0.2 km/s |
| Details | |
| ψ Dra A | |
| Mass | 1.38+0.15 −0.08 / 0.70 ± 0.07 M☉ |
| Radius | 1.2–1.3 R☉ |
| Surface gravity (log g) | 3.90 ± 0.11 cgs |
| Temperature | 6544 ± 42 / 4400 ± 300 K |
| Metallicity | −0.10 ± 0.05 dex |
| ψ Dra B | |
| Mass | 1.19 ± 0.07 M☉ |
| Radius | 1.5 R☉ |
| Surface gravity (log g) | 4.20 ± 0.12 cgs |
| Temperature | 6212 ± 75 K |
| Age | 3.3 ± 1.0 G years |
| Other designations | |
| Dziban, 31 Dra, ADS 10759 AB, Gliese 694.1 | |
| ψ Dra A: BD+72° 804, HD 162003, HIP 86614, HR 6636, SAO 8890 | |
| ψ Dra B: BD+72° 805, HD 162004, HIP 86620, HR 6637, SAO 8891 | |
| Database references | |
| SIMBAD | ψ Dra AB |
| ψ Dra A | |
| ψ Dra B | |
Psi Draconis (ψ Draconis, abbreviated Psi Dra, ψ Dra), also designated 31 Draconis, is a triple star system in the northern constellation of Draco. The system is fairly close, and is located about 75 light-years (23 parsecs) from the Sun, based on its parallax.
Psi Draconis was considered a binary star consisting of an F-type subgiant and an F-type main-sequence star, designated Psi Draconis A (officially named Dziban /ˈzaɪbən/, from the traditional name of the system) and Psi Draconis B, respectively. In 2015, Psi Draconis A was itself found to be a double-lined spectroscopic binary, making the system a triple. The companion to Psi Draconis A was designated Psi Draconis C by its discoverers.
Also in 2015, Psi Draconis B was discovered to be orbited by an exoplanet, designated Psi Draconis Bb.
Nomenclature
ψ Draconis (Latinised to Psi Draconis) is the system's Bayer designation and 31 Draconis its Flamsteed designation. The designation of the components – ψ Draconis A and B – derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).
Psi Draconis bore the traditional name of Dziban or Dsiban, derived from the Arabic Adh-Dhi'ban, meaning "The two wolves" or "The two jackals". In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name Dziban for the component Psi Draconis A on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.
In Chinese astronomy, Psi Draconis is called 女史, Pinyin: Nǚshǐ, meaning Female Protocol, because this star is marking itself and stands alone in the asterism Female Protocol in the Purple Forbidden enclosure (see Chinese constellation). 女史 (Nǚshǐ) has been Latinised into Niu She by R.H. Allen, meaning "the Palace Governess", or "a Literary Woman".
Properties
ψ Draconis AC and ψ Draconis B are separated by about 31 arcseconds. Only a very small fraction of the orbit has been observed: an orbital period of 10,000 years has been calculated, but it is extremely preliminary and likely to be in high error.
ψ Draconis A and C have varying radial velocities in respect to Earth, indicating that there must be orbital motion. The orbital period is estimated to be around 20 years, and the eccentricity must be fairly high, around 0.679.
Planetary system
Psi Draconis Bb is a Jupiter-like exoplanet orbiting Psi Draconis B, the secondary star. The planet was discovered when periodic Doppler shifts in the star's spectrum revealed the presence of a planet, similar to the spectroscopic binary nature of Psi Draconis AC. Its minimum mass is 1.53 MJ, and it orbits its host star every 8.5 years taking a relatively eccentric orbit.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥1.53 ± 0.10 MJ | 4.43 ± 0.04 | 3117 ± 42s | 0.40 ± 0.05 | — | — |
References
- ^ van Leeuwen, F.; et al. (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.
- ^ Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
- Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ "psi01 Dra A". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 March 2017.
- ^ "psi01 Dra B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 17 March 2017.
- ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ Gullikson, Kevin; Endl, Michael; Cochran, William D.; MacQueen, Phillip J. (2015). "Mining Planet Search Data for Binary Stars: The ψ Draconis system". The Astrophysical Journal. 815 (1): 62. arXiv:1511.01903. Bibcode:2015ApJ...815...62G. doi:10.1088/0004-637X/815/1/62. S2CID 59408173.
- ^ Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) – Third edition – Comments and statistics". Astronomy & Astrophysics. 367 (2): 521–24. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754.
- ^ Endl, Michael; Brugamyer, Erik J.; Cochran, William D.; MacQueen, Phillip J.; Robertson, Paul; Meschiari, Stefano; Ramirez, Ivan; Shetrone, Matthew; Gullikson, Kevin; Johnson, Marshall C.; Wittenmyer, Robert; Horner, Jonathan; Ciardi, David R.; Horch, Elliott; Simon, Attila E.; Howell, Steve B.; Everett, Mark; Caldwell, Caroline; Castanheira, Barbara G. (2016). "Two New Long-Period Giant Planets from the Mcdonald Observatory Planet Search and Two Stars with Long-Period Radial Velocity Signals Related to Stellar Activity Cycles". The Astrophysical Journal. 818 (1): 34. arXiv:1512.02965. Bibcode:2016ApJ...818...34E. doi:10.3847/0004-637X/818/1/34. S2CID 39476347.
- ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
- Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 .
- ^ Star Name – R.H. Allen p.212
- "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- "WG Triennial Report (2015–2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
- (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 10 日 Archived 2011-05-21 at the Wayback Machine
- "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Archived from the original on 2017-04-30. Retrieved 2017-03-24.
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