HR 4049

HR 4049

File:HR4049LightCurve.png A light curve for HR 4049. The main plot shows the visual band brightness over one orbital period. The inset plot shows how the amplitude of the brightness change varies as a function of wavelength−1; as the observing wavelength increases, the opacity of the dust decreases, so the dust obscures less of the star's light. Adapted from Jorissen & Frankowski (2008)
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Antlia
Right ascension	Template:RA
Declination	Template:DEC
Apparent magnitude (V)	5.29 - 5.83
Characteristics
Evolutionary stage	Post-AGB
Spectral type	B9.5Ib-II
B−V Template:Engvar	+0.24
Variable type	unique
Astrometry
Radial velocity (Rv)	−33 km/s
Proper motion (μ)	RA: −15.734 mas/yr Dec.: +10.671 mas/yr
Parallax (π)	0.5799±0.1514 mas
Distance	approx. Template:Rnd ly (approx. Template:Rnd pc)
Orbit
Period (P)
Eccentricity (e)
Semi-amplitude (K1) (primary)	km/s
Details
A
Mass	0.56 Template:Solar mass
Radius	Template:Solar radius
Luminosity	6,300 Template:Solar luminosity
Surface gravity (log g)	cgs
Temperature	K
Metallicity [Fe/H]	dex
B
Mass	0.56 Template:Solar mass
Radius	0.6 Template:Solar radius
Luminosity	0.06 Template:Solar luminosity
Surface gravity (log g)	4.6 cgs
Temperature	3,500 K
Metallicity [Fe/H]	{{{metal_fe2}}} dex
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

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 distant.

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. It also shows a strong infrared excess, corresponding closely to a blackbody produced by a disk of material surrounding the star. The star is also undergoing intense mass-loss

HR 4049 has an unseen companion, detected from variations in the doppler shift of its spectral lines. The properties of the companion can only be estimated by making certain assumptions about the inclination of the orbit and the mass function. Given those assumptions, it is thought to be a low luminosity main sequence star.

HR 4049 was discovered to be a variable star by Christoffel Waelkens and Fredy Rufener in 1983. It was given the variable star designation AG Antliae in 1987, but is still more commonly referred to as HR 4049.

HR 4049 is an unusual variable star, ranging between magnitudes 5.29 and 5.83 with a period of 429 days. It has been described as pulsating in a similar fashion to an RV Tauri variable, 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.

Although HR 4049 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.

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