AD Phoenicis
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Phoenix |
| Right ascension | 01h 16m 38.07s[1] |
| Declination | −39° 42′ 31.33″[1] |
| Apparent magnitude (V) | 10.27 – 10.80[2] |
| Characteristics | |
| Evolutionary stage | F9/G0V[3] |
| B−V color index | 0.56[3] |
| Variable type | W UMa[2] |
| Astrometry | |
| Radial velocity (Rv) | 28.87 ± 1.47[3] km/s |
| Proper motion (μ) | RA: −3.24[1] mas/yr Dec.: +23.04[1] mas/yr |
| Parallax (π) | 4.9818 ± 0.0311[1] mas |
| Distance | 655 ± 4 ly (201 ± 1 pc) |
| Orbit | |
| Period (P) | 0.37992361 days[4] |
| Semi-major axis (a) | 2.46 R☉[4] |
| Inclination (i) | 76.92 ± 0.06[4]° |
| Semi-amplitude (K1) (primary) |
89.04±3.10[3] km/s |
| Semi-amplitude (K2) (secondary) |
242.41±1.42[3] km/s |
| Details[4] | |
| Primary | |
| Mass | 1.004 M☉ |
| Radius | 1.18 R☉ |
| Temperature | 6,155 K |
| Secondary | |
| Mass | 0.378 M☉ |
| Radius | 0.77 R☉ |
| Temperature | 6,115 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
AD Phoenicis is a variable star in the constellation of Phoenix. An eclipsing binary, its apparent magnitude has a maximum of 10.27, dimming to 10.80 during primary and secondary eclipses, which are approximately equal.[2] From parallax measurements by the Gaia spacecraft, the system is located at a distance of 655 light-years (201 parsecs) from Earth.[1]
AD Phoenicis is a contact binary of W Ursae Majoris type, composed of two stars so close that their surfaces touch each other. They are separated by 2.46 solar radii and orbit each other with a period of 0.3799 days. The primary star has a mass of 1.00 solar mass and a radius of 1.18 solar radii, while the secondary has 0.38 solar masses and 0.77 solar radii. Their surface temperatures are very similar, 6,155 and 6,115 K, which is the reason for the eclipses being equal-depth. In visible light, the primary star contributes to 71.2% of the system's luminosity, while the secondary contributes to the rest (28.8%). The eclipses light curve shows an assymetric feature that is best explained by a large star spot in the surface of the primary, about 700 K cooler than the rest of the photosphere.[4]
Variations in the orbital period of the system have been detected, which were modeled as a continuous decrease in the period plus a cyclic oscilation. The period decrease of about 1.5×10−7 days per year is likely caused by mass transfer from the secondary to the primary star, while the oscilation can be explained by a third star in the system or by a magnetic activity cycle. In the third star hypothesis, its orbit would have a period of 56.2 ± 0.9 years and an eccentricity of 0.36 ± 0.01. A minimum mass of 0.257 solar masses is calculated, which corresponds to a red dwarf of spectral type M4–M5, consistent with the lack of photometric and spectroscopic evidence for this star.[4]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Template:Cite DR2
- ↑ 2.0 2.1 2.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 3.0 3.1 3.2 3.3 3.4 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
