HR 4049
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Antlia |
| Right ascension | 10h 18m 07.59s[1] |
| Declination | –28° 59′ 31.2″[1] |
| Apparent magnitude (V) | 5.53 |
| Characteristics | |
| Spectral type | B9.5Ib-II |
| B−V color index | 0.23 |
| Variable type | Post-AGB Star |
| Astrometry | |
| Radial velocity (Rv) | -33 km/s |
| Proper motion (μ) | RA: –15.86 ± 0.32[1] mas/yr Dec.: 10.85 ± 0.38[1] mas/yr |
| Parallax (π) | 1.23 ± 0.36[1] mas |
| Distance | approx. 2,700 ly (approx. 800 pc) |
| Absolute magnitude (MV) | -3.68 |
| Details | |
| Mass | 1.2 M☉ |
| Radius | 15.1 [2] R☉ |
| Luminosity | 3823 L☉ |
| Temperature | 11500 K |
| Other designations | |
| Database references | |
| SIMBAD | data |
HR 4049, also known as HD 89353 and AG Antliae, is a post-asymptotic-giant-branch star in the constellation Antlia. A very metal-poor star,[3] it is surrounded by a thick unique circumbinary disk enriched in several molecules.[4] With an apparent magnitude of 5.53, the star can readily be seen under ideal conditions.[5] The star, located approximately 813 parsecs (2,650 ly) distant,[5] has been found to be a binary star;[6] however, likely the most unique feature about this star is its peculiar spectrum. The star appears, based on its spectrum in the Balmer series, to be a blue supergiant, although in reality it is an old low-mass star on the post-AGP phase of its life.[7] The star is also undergoing intense mass-loss[8] and is a unique variable, ranging between magnitudes 5.29 and 5.83 with a period of 429 days[9]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Lua error in package.lua at line 80: module 'strict' not found.Vizier catalog entry
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- ↑ 5.0 5.1 Lua error in package.lua at line 80: module 'strict' not found.
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External links
- The Spatial Distribution of Grains Around the Dual Chemistry Post-AGB Star
- Synthetic post-AGB evolution
- Non-linear radiative models of post-AGB stars: Application to HD 56126
- Post-AGB stars as testbeds of nucleosynthesis in AGB stars
- The post-AGB evolution of AGB mass loss variations
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