Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Phoenix |
Right ascension | 01h 50m 54.44s [2] |
Declination | −50° 12′ 22.09″ [2] |
Apparent magnitude (V) | 5.90 – 5.94 [3] |
Characteristics | |
Spectral type | A1Va λ Boo [4] |
Variable type | δ Scuti [3] |
Astrometry | |
Radial velocity (Rv) | 3.0 [5] km/s |
Proper motion (μ) |
RA: -47.85
[2]
mas/
yr Dec.: -3.70 [2] mas/ yr |
Parallax (π) | 12.7260 ± 0.0447 mas [2] |
Distance | 256.3 ± 0.9
ly (78.6 ± 0.3 pc) |
Absolute magnitude (MV) | 1.5 ± 0.1 [1] |
Details | |
Mass | 2.02 ± 0.04 [1] M☉ |
Luminosity | 20.5 ± 0.34 [6] L☉ |
Surface gravity (log g) | 3.91 ± 0.08 [1] cgs |
Temperature | 7,818 ± 38 [6] K |
Rotational velocity (v sin i) | 120 ± 5 [1] km/s |
Age | 813+38 −89 [1] Myr |
Other designations | |
Database references | |
SIMBAD | data |
BD Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 256 light-years (78 parsecs) from Earth. [2] Its absolute magnitude is calculated at 1.5. [1]
BD Phoenicis is a Lambda Boötis star, an uncommon type of peculiar stars that have very low abundances of iron-peak elements. In particular, BD Phoenicis has near-solar carbon and oxygen content, but its iron abundance is only 4% of the solar value. [1] BD Phoenicis is also a pulsating variable of Delta Scuti type, varying its apparent magnitude between 5.90 and 5.94. [3] A study of its light curve detected seven pulsation periods that range from 50 to 84 minutes, the strongest one having a period of 57 minutes and an amplitude of 9 milli-magnitudes. Pulsations are common among Lambda Boötis stars and seem to be more common than on normal main sequence stars of the same spectral type. [1]
BD Phoenicis is an A-type main-sequence star with a spectral type of A1Va. [4] Stellar evolution models indicate it has about double the solar mass and an age of about 800 million years, having completed 83% of its main sequence lifetime. [1] It is radiating 21 times the Sun's luminosity from its photosphere at an effective temperature of 7800 K. [6] BD Phoenicis has a composite spectra that indicate it is a binary star, but nothing is known about the companion. [8] [6]
Observations by the Herschel Space Observatory have detected an infrared excess from BD Phoenicis, indicating that there is a debris disk in the system. By modeling the emission as a black body, it is estimated that the dust has a temperature of 55±2 K and is at a distance of 118±10 au from the star. The existence of debris disks is possibly related to the Lambda Boötis phenomenon. [6]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Phoenix |
Right ascension | 01h 50m 54.44s [2] |
Declination | −50° 12′ 22.09″ [2] |
Apparent magnitude (V) | 5.90 – 5.94 [3] |
Characteristics | |
Spectral type | A1Va λ Boo [4] |
Variable type | δ Scuti [3] |
Astrometry | |
Radial velocity (Rv) | 3.0 [5] km/s |
Proper motion (μ) |
RA: -47.85
[2]
mas/
yr Dec.: -3.70 [2] mas/ yr |
Parallax (π) | 12.7260 ± 0.0447 mas [2] |
Distance | 256.3 ± 0.9
ly (78.6 ± 0.3 pc) |
Absolute magnitude (MV) | 1.5 ± 0.1 [1] |
Details | |
Mass | 2.02 ± 0.04 [1] M☉ |
Luminosity | 20.5 ± 0.34 [6] L☉ |
Surface gravity (log g) | 3.91 ± 0.08 [1] cgs |
Temperature | 7,818 ± 38 [6] K |
Rotational velocity (v sin i) | 120 ± 5 [1] km/s |
Age | 813+38 −89 [1] Myr |
Other designations | |
Database references | |
SIMBAD | data |
BD Phoenicis is a variable star in the constellation of Phoenix. From parallax measurements by the Gaia spacecraft, it is located at a distance of 256 light-years (78 parsecs) from Earth. [2] Its absolute magnitude is calculated at 1.5. [1]
BD Phoenicis is a Lambda Boötis star, an uncommon type of peculiar stars that have very low abundances of iron-peak elements. In particular, BD Phoenicis has near-solar carbon and oxygen content, but its iron abundance is only 4% of the solar value. [1] BD Phoenicis is also a pulsating variable of Delta Scuti type, varying its apparent magnitude between 5.90 and 5.94. [3] A study of its light curve detected seven pulsation periods that range from 50 to 84 minutes, the strongest one having a period of 57 minutes and an amplitude of 9 milli-magnitudes. Pulsations are common among Lambda Boötis stars and seem to be more common than on normal main sequence stars of the same spectral type. [1]
BD Phoenicis is an A-type main-sequence star with a spectral type of A1Va. [4] Stellar evolution models indicate it has about double the solar mass and an age of about 800 million years, having completed 83% of its main sequence lifetime. [1] It is radiating 21 times the Sun's luminosity from its photosphere at an effective temperature of 7800 K. [6] BD Phoenicis has a composite spectra that indicate it is a binary star, but nothing is known about the companion. [8] [6]
Observations by the Herschel Space Observatory have detected an infrared excess from BD Phoenicis, indicating that there is a debris disk in the system. By modeling the emission as a black body, it is estimated that the dust has a temperature of 55±2 K and is at a distance of 118±10 au from the star. The existence of debris disks is possibly related to the Lambda Boötis phenomenon. [6]