Iota Pegasi
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Pegasus |
| Right ascension | 22h 07m 00.666s[1] |
| Declination | 25° 20′ 42.40″[1] |
| Apparent magnitude (V) | 3.84/6.68[2] |
| Characteristics | |
| Spectral type | F5V/G9V |
| Astrometry | |
| Proper motion (μ) | RA: 296.53 ± 0.59[1] mas/yr Dec.: 27.29 ± 0.58[1] mas/yr |
| Parallax (π) | 85.28 ± 0.63[1] mas |
| Distance | 38.2 ± 0.3 ly (11.73 ± 0.09 pc) |
| Absolute magnitude (MV) | 3.49/6.33[2] |
| Orbit | |
| Companion | Iota Pegasi B |
| Period (P) | 0.028 yr |
| Semi-major axis (a) | 0.0094" |
| Eccentricity (e) | 0.02 |
| Details | |
| ι Peg A | |
| Mass | 1.33[2] M☉ |
| Radius | 1.526 ± 0.068[3] R☉ |
| Surface gravity (log g) | 4.26[2] cgs |
| Temperature | 6,580[2] K |
| ι Peg B | |
| Mass | 0.82[2] M☉ |
| Radius | 0.73[2] R☉ |
| Surface gravity (log g) | 4.62[2] cgs |
| Temperature | 5,060[2] K |
Iota Pegasi (24 Peg, HD 210027) is a star located within the constellation Pegasus. It is about 38 light-years from Earth.[1] It is a spectroscopic binary system.[4]
Iota Pegasi A is a yellowish-white star somewhat brighter than the sun. It and the dimmer Iota Pegasi B orbit each other with a period of about 10 days. In about four billion years from now, component A 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.[2]
References
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- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Lua error in package.lua at line 80: module 'strict' not found. Vizier catalog entry
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 2.9 Lua error in package.lua at line 80: module 'strict' not found.
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