Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Dorado |
Right ascension | 05h 33m 37.51253s [1] |
Declination | −62° 29′ 23.3231″ [1] |
Apparent magnitude (V) | 3.46 to 4.08 [2] |
Characteristics | |
Spectral type | F4-G4Ia-II [3] |
U−B color index | +0.55 [3] |
B−V color index | +0.70 [4] |
R−I color index | +0.48 [4] |
Variable type | δ Cephei [2] |
Astrometry | |
Radial velocity (Rv) | +7.2 [5] km/s |
Proper motion (μ) |
RA: +0.800
[1]
mas/
yr Dec.: +9.458 [1] mas/ yr |
Parallax (π) | 3.1119 ± 0.2845 mas [1] |
Distance | 1112+52 −49 ly (341+16 −15 pc) [6] |
Absolute magnitude (MV) | −3.91±0.11 [7] |
Details | |
Mass | 7.7±0.2 [8] M☉ |
Radius | 67.8±0.7 [9] R☉ |
Luminosity | 3,200 [7] L☉ |
Surface gravity (log g) | 1.3 [10] cgs |
Temperature | 5,445 [7] K |
Metallicity [Fe/H] | –0.13 [10] dex |
Rotational velocity (v sin i) | 0 [3] km/s |
Age | 42.5±2.7 [8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Beta Doradus, Latinized from β Doradus, is the second brightest star in the southern constellation of Dorado. [12] It is a Classical Cepheid variable, with an apparent magnitude that varies between 3.46 to 4.08. [2] Based upon a measurement that uses its parallax measured with the Gaia spacecraft, its color and apparent brightness, it is located at a distance of 1,110 light-years (340 parsecs) from Earth. [6]
Beta Doradus is a Cepheid variable that regularly changes magnitude from a low of 4.08 to a high of 3.46 [2] over a period of 9.84318 days. [14] The light curve of this magnitude change follows a nearly regular saw-tooth pattern, with average amplitude variations period to period about 0.005 magnitude from average amplitude of 0.62 magnitude. [14] During each radial pulsation cycle, the radius of the star varies by 3.9 R☉ around a mean of 67.8 R☉. [9] Its spectral type and luminosity class are likewise variable, from F-type to G-type and from a supergiant to a bright giant. [3]
Far ultraviolet emissions have been detected from this star with the Far Ultraviolet Spectroscopic Explorer, while X-ray emissions were detected with the XMM-Newton space telescope. The X-ray luminosity is about 1 × 1029 erg/s and the emission varies with the pulsation period, suggesting a connection with the pulsation process. The peak X-ray emissions are in the 0.6–0.8 keV energy range, which occurs for plasmas with temperatures of 7–10 million K. [15]
Observation data Epoch J2000.0 Equinox J2000.0 ( ICRS) | |
---|---|
Constellation | Dorado |
Right ascension | 05h 33m 37.51253s [1] |
Declination | −62° 29′ 23.3231″ [1] |
Apparent magnitude (V) | 3.46 to 4.08 [2] |
Characteristics | |
Spectral type | F4-G4Ia-II [3] |
U−B color index | +0.55 [3] |
B−V color index | +0.70 [4] |
R−I color index | +0.48 [4] |
Variable type | δ Cephei [2] |
Astrometry | |
Radial velocity (Rv) | +7.2 [5] km/s |
Proper motion (μ) |
RA: +0.800
[1]
mas/
yr Dec.: +9.458 [1] mas/ yr |
Parallax (π) | 3.1119 ± 0.2845 mas [1] |
Distance | 1112+52 −49 ly (341+16 −15 pc) [6] |
Absolute magnitude (MV) | −3.91±0.11 [7] |
Details | |
Mass | 7.7±0.2 [8] M☉ |
Radius | 67.8±0.7 [9] R☉ |
Luminosity | 3,200 [7] L☉ |
Surface gravity (log g) | 1.3 [10] cgs |
Temperature | 5,445 [7] K |
Metallicity [Fe/H] | –0.13 [10] dex |
Rotational velocity (v sin i) | 0 [3] km/s |
Age | 42.5±2.7 [8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Beta Doradus, Latinized from β Doradus, is the second brightest star in the southern constellation of Dorado. [12] It is a Classical Cepheid variable, with an apparent magnitude that varies between 3.46 to 4.08. [2] Based upon a measurement that uses its parallax measured with the Gaia spacecraft, its color and apparent brightness, it is located at a distance of 1,110 light-years (340 parsecs) from Earth. [6]
Beta Doradus is a Cepheid variable that regularly changes magnitude from a low of 4.08 to a high of 3.46 [2] over a period of 9.84318 days. [14] The light curve of this magnitude change follows a nearly regular saw-tooth pattern, with average amplitude variations period to period about 0.005 magnitude from average amplitude of 0.62 magnitude. [14] During each radial pulsation cycle, the radius of the star varies by 3.9 R☉ around a mean of 67.8 R☉. [9] Its spectral type and luminosity class are likewise variable, from F-type to G-type and from a supergiant to a bright giant. [3]
Far ultraviolet emissions have been detected from this star with the Far Ultraviolet Spectroscopic Explorer, while X-ray emissions were detected with the XMM-Newton space telescope. The X-ray luminosity is about 1 × 1029 erg/s and the emission varies with the pulsation period, suggesting a connection with the pulsation process. The peak X-ray emissions are in the 0.6–0.8 keV energy range, which occurs for plasmas with temperatures of 7–10 million K. [15]