HD 208527
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 21h 56m 23.98467s[1] |
| Declination | +21° 14′ 23.4961″[1] |
| Apparent magnitude (V) | +6.39[2] |
| Characteristics | |
| Spectral type | M1III or K5V[3][4] |
| B−V color index | 1.698±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | +4.79±0.06[4] km/s |
| Proper motion (μ) | RA: 2.00[1] mas/yr Dec.: 15.30[1] mas/yr |
| Parallax (π) | 2.48 ± 0.38 mas[1] |
| Distance | approx. 1,300 ly (approx. 400 pc) |
| Absolute magnitude (MV) | –1.24[4] |
| Details[4] | |
| Mass | 1.6±0.4 M☉ |
| Radius | 51.1±8.3 R☉ |
| Surface gravity (log g) | 1.6±0.3 cgs |
| Temperature | 4,035±65 K |
| Metallicity [Fe/H] | −0.09±0.16 dex |
| Rotational velocity (v sin i) | 3.6 km/s |
| Age | 2±1.3 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 208527 is a star located in the northern constellation of Pegasus. It has a reddish hue and is dimly visible to the naked eye with an apparent visual magnitude of +6.39.[2] The star is located at a distance of approximately 1,300 light years from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +4.8 km/s.[4]
This was once catalogued as a K-type main-sequence star with a stellar classification of K5V, but is now known as an aging red giant with a class of M1III, based on its dimensions and low surface gravity.[4] This indicates that the two-billion year old star has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It has an estimated 1.6 times the mass of the Sun but has swollen to 51 times the Sun's radius.[4]
Planetary system
From September 2008 to June 2012, the team B.-C. Lee, I. Han and M.-G. Park observed HD 208527 with "the high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO)".
In 2012, a long-period, wide-orbiting planet was deduced by radial velocity. This was published in November, gaining the designation HD 208527 b.[3] Along with HD 220074 b this is one of the first two planets proposed around a red giant.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥9.9±1.7 MJ | 2.1±0.2 | 875.5±5.8 | 0.08±0.04 | — | — |
References
- ^ a b c d e f van Leeuwen, F. (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.
- ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c "hd_208527_b".
- ^ a b c d e f g Lee, B.-C.; et al. (2012). "Planetary companions orbiting M giants HD 208527 and HD 220074". Astronomy & Astrophysics. 549: A2. arXiv:1211.2051. Bibcode:2013A&A...549A...2L. doi:10.1051/0004-6361/201220301. S2CID 73522393.
- ^ "HD 208527". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-25.
