Astronomy:AG Draconis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Draco |
| Right ascension | 16h 01m 41.01257s[2] |
| Declination | +66° 48′ 10.1312″[2] |
| Apparent magnitude (V) | 7.9 - 10.3[3] |
| Characteristics | |
| Spectral type | K3 IIIep[4] + WD[5] |
| B−V color index | 1.425±0.094[6] |
| Variable type | Z And[7] |
| Astrometry | |
| Radial velocity (Rv) | −147.42±0.30[6] km/s |
| Proper motion (μ) | RA: −7.135[2] mas/yr Dec.: −5.602[2] mas/yr |
| Parallax (π) | 0.2101 ± 0.0268[2] mas |
| Distance | approx. 16,000 ly (approx. 4,800 pc) |
| Orbit[8] | |
| Period (P) | 549.73 d |
| Eccentricity (e) | 0.06 |
| Periastron epoch (T) | 2447622.28 JD |
| Argument of periastron (ω) (secondary) | 359.8° |
| Semi-amplitude (K1) (primary) | 4.67 km/s |
| Details[5] | |
| AG Dra A | |
| Mass | 1.5 M☉ |
| Radius | 35 R☉ |
| Metallicity [Fe/H] | −1.3 dex |
| AG Dra B | |
| Luminosity | ~ 103 L☉ |
| Temperature | ~ 105 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
AG Draconis is a binary star system in the northern constellation of Draco. It consists of a giant star and a white dwarf that revolve around each other every 550 days.
Discovery
AG Draconis has been catalogued since the start of the 20th century, as BD+67°922. However, its unusual nature did not start to come to light until the middle of the century. It was noted as an emission-line object in 1943,[10] although its nature was not understood.[11] The emission spectrum was serendipitously discovered to be variable by Nancy Grace Roman when she observed the star and found that the spectrum had completely changed since earlier observations.[12] It was given the variable star designation AG Draconis in 1964.[13]
Variability
AG Draconis spends most of its time in a quiescent phase near visual magnitude 9.8, with only small semi-regular variations thought to be due to pulsations of the giant star. At its faintest, it can reach magnitude 10.3.[3] The semi-regular variations have periods of 340 - 370 days. Variations at ultraviolet wavelengths occur with a period of 550 days, which is the orbital period.[5]
Every 12-16 years, outbursts occur and last for several years.[5] The brightness can increase to visual magnitude 7.9,[3] although usually not this bright.[5]
System
The a sin i value for the primary is 50.69 R☉, where a is the semimajor axis and i is the (unknown) orbital inclination.[8] The larger star is thought to be an orange hued giant around 1.5 times as massive as the Sun that has swollen to around 35 times the diameter of the Sun with a spectral type measured at K3IIIep.[5] The smaller star is a compact hot white dwarf around 0.4 times as massive as the Sun, with a surface temperature of around 80,000 K.[14]
References
- ↑ Gális, R.; Hric, L.; Smelcer, L. (February 2015). "AG Draconis - a symbiotic mystery". Open European Journal on Variable Stars 169: 4–9. Bibcode: 2015OEJV..169....4G. https://ui.adsabs.harvard.edu/abs/2015OEJV..169....4G. Retrieved 2 January 2022.
- ↑ 2.0 2.1 2.2 2.3 2.4 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.
- ↑ 3.0 3.1 3.2 "AG Draconis". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=13733.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Hric, L. et al. (September 2014). "Outburst activity of the symbiotic system AG Dra". Monthly Notices of the Royal Astronomical Society 443 (2): 1103–1112. doi:10.1093/mnras/stu1162. Bibcode: 2014MNRAS.443.1103H.
- ↑ 6.0 6.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 8.0 8.1 Gális, R.; Hric, L.; Friedjung, M.; Petrík, K. (1999). "Resonances as the general cause of the outbursts in the symbiotic system AG Draconis". Astronomy and Astrophysics 348: 533. Bibcode: 1999A&A...348..533G.
- ↑ "AG Dra". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=AG+Dra.
- ↑ Janssen, Edith M.; Vyssotsky, A. N. (1943). "A Peculiar Emission-Line Object". Publications of the Astronomical Society of the Pacific 55 (326): 244. doi:10.1086/125560. Bibcode: 1943PASP...55..244J.
- ↑ Wilson, Ralph E. (1950). "The Spectrum of HD 4174". Publications of the Astronomical Society of the Pacific 62 (363): 14. doi:10.1086/126211. Bibcode: 1950PASP...62...14W.
- ↑ Roman, Nancy G. (1953). "The Spectrum of BD+67°922". The Astrophysical Journal 117: 467. doi:10.1086/145717. Bibcode: 1953ApJ...117..467R.
- ↑ Robinson, L. J. (1964). "AG Draconis". Information Bulletin on Variable Stars 73: 1. Bibcode: 1964IBVS...73....1R.
- ↑ Sion, Edward M. et al. (2012). "On the Nature of the Hot Component in the Symbiotic, Supersoft X-Ray Binary AG Draconis". The Astronomical Journal 144 (6): 5. doi:10.1088/0004-6256/144/6/171. 171. Bibcode: 2012AJ....144..171S.
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