Iota Pegasi
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22h 07m 00.66206s[1] |
| Declination | 25° 20′ 42.3761″[1] |
| Apparent magnitude (V) | 3.77[2] (3.84 + 6.68)[3] |
| Characteristics | |
| Spectral type | F5V + G8V[4] |
| Astrometry | |
| Radial velocity (Rv) | −5.5±0.7[5] km/s |
| Proper motion (μ) | RA: 298.420[1] mas/yr Dec.: 26.161[1] mas/yr |
| Parallax (π) | 84.7637 ± 0.3596 mas[1] |
| Distance | 38.5 ± 0.2 ly (11.80 ± 0.05 pc) |
| Absolute magnitude (MV) | 3.42[2] (3.49 + 6.33)[3] |
| Orbit[4] | |
| Companion | Iota Pegasi B |
| Period (P) | 10.2130253(16) d |
| Semi-major axis (a) | 10.329(16) mas |
| Eccentricity (e) | 0.001764(63) |
| Inclination (i) | 95.83(12)° |
| Longitude of the node (Ω) | 176.262(75)° |
| Periastron epoch (T) | 52997.378(52) |
| Argument of periastron (ω) (secondary) | 272.8(1.8)° |
| Semi-amplitude (K1) (primary) | 48.4757(39) km/s |
| Semi-amplitude (K2) (secondary) | 77.777(16) km/s |
| Details | |
| ι Peg Aa | |
| Mass | 1.33[3] M☉ |
| Radius | 1.526 ± 0.068[6] R☉ |
| Surface gravity (log g) | 4.26[3] cgs |
| Temperature | 6,580[3] K |
| Age | 4−663[4] Myr |
| ι Peg Ab | |
| Mass | 0.82[3] M☉ |
| Radius | 0.73[3] R☉ |
| Surface gravity (log g) | 4.62[3] cgs |
| Temperature | 5,060[3] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
ι Pegasi, Latinized as Iota Pegasi is a double-lined spectroscopic binary[8] star system located within the northern constellation of Pegasus, along a line between Lambda and Kappa Pegasi. It is visible to the naked eye as a yellow-hued point of light with a combined apparent visual magnitude of 3.77.[2] The system is located 38.5 light years from the Sun based on parallax,[1] but is drifting closer with a radial velocity of −5.5 km/s.[5]
The binary nature of this system was discovered by W. W. Campbell in 1899 and the initial orbital elements were estimated by H. D. Curtis in 1904.[8] The primary, designated component Aa, is a yellowish-white star somewhat brighter than the sun. It and the dimmer component Ab orbit each other with a period of about 10 days and an eccentricity of almost zero, meaning they essentially have a circular orbit.[4] They appear to be very young stars, close to zero-age main sequence.[8]
In about four billion years from now, component Aa will evolve off the main sequence into a giant. In the process it will overflow its Roche lobe and begin to transfer mass onto the secondary. This may cause the secondary to acquire enough mass to become the primary component. After both stars have passed through the giant star stage, the end result will be a pair of co-orbiting white dwarfs in about eight billion years.[3]
References
[edit]- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ 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 d e f g h i j Fuhrmann, Klaus (February 2008), "Nearby stars of the Galactic disc and halo - IV", Monthly Notices of the Royal Astronomical Society, 384 (1): 173–224, Bibcode:2008MNRAS.384..173F, doi:10.1111/j.1365-2966.2007.12671.x
- ^ a b c d Konacki, Maciej; et al. (2010). "High-precision Orbital and Physical Parameters of Double-lined Spectroscopic Binary Stars—HD78418, HD123999, HD160922, HD200077, and HD210027". The Astrophysical Journal. 719 (2): 1293–1314. arXiv:0910.4482. Bibcode:2010ApJ...719.1293K. doi:10.1088/0004-637X/719/2/1293. S2CID 119253596.
- ^ a b 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.
- ^ van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal. 694 (2): 1085–1098. arXiv:0901.1206. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID 18370219.
- ^ "iot Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-05.
- ^ a b c Boden, A. F.; et al. (April 1999), "The Visual Orbit of ι Pegasi", The Astrophysical Journal, 515 (1): 356–364, arXiv:astro-ph/9811029, Bibcode:1999ApJ...515..356B, doi:10.1086/307030, S2CID 119362086
External links
[edit]- Kaler, James B. (October 28, 2011). Iota Pegasi. Retrieved 2019-08-05.
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