HR 4049
Protoplanetary nebula in the constellation Antlia
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HR 4049, also known as HD 89353 and AG Antliae, is a binary post-asymptotic-giant-branch (post-AGB) star in the constellation Antlia. A very metal-poor star, it is surrounded by a thick unique circumbinary disk enriched in several molecules. With an apparent magnitude of about 5.5, the star can readily be seen with the naked eye under ideal conditions. It is located approximately 1,400 parsecs (4,600 ly) distant.
 | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Antlia[1] |
| Right ascension | 10h 18m 07.59s[2] |
| Declination | −28° 59′ 31.2″[2] |
| Apparent magnitude (V) | 5.29 – 5.83[3] |
| Characteristics | |
| Evolutionary stage | Post-AGB + main sequence[4] |
| Spectral type | B9.5Ib-II[3] |
| B−V color index | +0.24[5] |
| Variable type | unique[3] |
| Astrometry | |
| Radial velocity (Rv) | −30.12±0.09[6] km/s |
| Proper motion (μ) | RA: −16.290 mas/yr[2] Dec.: +10.720 mas/yr[2] |
| Parallax (π) | 0.7107±0.0984 mas[2] |
| Distance | approx. 4,600 ly (approx. 1,400 pc) |
| Orbit[6] | |
| Period (P) | 428.474±0.002 days |
| Eccentricity (e) | 0.29±0.01 |
| Inclination (i) | 60–75° |
| Periastron epoch (T) | 2,458,383.2±0.6 HJD |
| Argument of periastron (ω) (secondary) | 242.3±0.3° |
| Semi-amplitude (K1) (primary) | 15.52±0.13 km/s |
| Details | |
| A | |
| Mass | 0.75±0.05[6] M☉ |
| Radius | 76 ± 11[6][a] R☉ |
| Luminosity | 16,600+5,300 −4,000[6] L☉ |
| Surface gravity (log g) | +1.0±0.5[4] cgs |
| Temperature | 7,500±500[6] K |
| Metallicity [Fe/H] | −4.5[7] dex |
| B | |
| Mass | 0.70–0.82[6] M☉ |
| Radius | 0.6[4] R☉ |
| Luminosity | 0.06[4] L☉ |
| Surface gravity (log g) | 4.6[4] cgs |
| Temperature | 3,500[4] K |
| Other designations | |
| AG Antliae, CD−28°8070, 2MASS J10180758-2859308, GSC 06630-01759, HD 89353, FK5 1265, PPM 257470, HIP 50456, SAO 178644, HR 4049 | |
| Database references | |
| SIMBAD | data |
Characteristics
HR 4049 has a 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-AGB phase of its life. Its atmosphere is extremely deficient in heavy elements, over with a metallicity over 30,000 lower than the Sun.[8][9] It also shows a strong infrared excess, corresponding closely to a 1,200 K blackbody produced by a disk of material surrounding the star.[10] The star is also undergoing intense mass-loss[11] Its companion has only been detected from variations in the doppler shift of its spectral lines. It is thought to be a low luminosity main sequence star.[4]
Although HR 4049 A apparently has the spectrum of a blue supergiant, it is an old low-mass star which has exhausted nuclear fusion and is losing its outer layers as it transitions towards a white dwarf and possibly a planetary nebula. During this phase it has a luminosity several thousand times that of the Sun, although a mass around half that of the Sun. The mass can only be guessed from the expected mass of the white dwarf that it is becoming.[12]
Variability
HR 4049 is an unusual variable star, ranging between magnitudes 5.29 and 5.83 with a period of 429 days.[14] It has been described as pulsating in a similar fashion to an RV Tauri variable,[15] although the preferred interpretation is that the variations are produced by variable extinction produced by the material around the star and that the period is the same as the orbital period.[4]
It was discovered to be a variable star by Christoffel Waelkens and Fredy Rufener in 1983[16] and was given the variable star designation AG Antliae in 1987,[17] but is still more commonly referred to as HR 4049.[6]
Notes
- Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:
