Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Puppis |
Right ascension | 06h 48m 04.69996s [1] |
Declination | −44° 18′ 58.4377″ [1] |
Apparent magnitude (V) | 8.287 [2] |
Characteristics | |
Spectral type | sdO6p |
U−B color index | −1.259 [2] |
B−V color index | −0.270 [2] |
Variable type | HMXB [3] |
Astrometry | |
Radial velocity (Rv) | 12.10 [4] km/s |
Proper motion (μ) |
RA: −4.73
[1]
mas/
yr Dec.: 5.39 [1] mas/ yr |
Parallax (π) | 1.20 ± 0.50 mas [1] |
Distance | 650 [3] pc |
Orbit [3] | |
Period (P) | 1.55 days |
Eccentricity (e) | 0.0 |
Inclination (i) | 82° |
Details | |
sdO5.5 [5] | |
Mass | 1.50 [3] M☉ |
Radius | 1.45 [6] R☉ |
Luminosity | 3,943 [6] L☉ |
Surface gravity (log g) | 4.25 [6] cgs |
Temperature | 47,500 [6] K |
WD | |
Mass | 1.28 [3] M☉ |
Radius | 1,600 [7] km |
Temperature | 225,000 [7] K |
Other designations | |
Database references | |
SIMBAD | data |
HD 49798 is a binary star in the constellation Puppis about 650 parsecs (circa 2119 light-years) from Earth. It has an apparent magnitude of 8.3, making it one of the brightest known O class subdwarf stars. [8]
HD 49798 was discovered in 1964 to be a rare hydrogen-deficient O class subdwarf, and was the brightest known at the time. [9] This was identified as a binary star, but the companion could not be detected visually or spectroscopically. [10]
The X-ray source RX J0648.0-4418 was discovered close to HD 49798's location in the sky. Only the space telescope XMM-Newton was able to identify the source. It is a white dwarf with about 1.3 solar masses, in orbit about HD 49798 and rotating once every 13 seconds. [11] This is detected from the 13-second X-ray pulse, which results from the stellar wind accreting onto the compact object. [8] It has been proposed that the white dwarf is surrounded by a debris disk. In this model, the material of the disk would be funneled onto the poles of the dwarf via the magnetic field, which would explain the observed X-ray pulses. [8] This system is considered a likely candidate to explode as a type Ia supernova within a few thousand years. [12] [13]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Puppis |
Right ascension | 06h 48m 04.69996s [1] |
Declination | −44° 18′ 58.4377″ [1] |
Apparent magnitude (V) | 8.287 [2] |
Characteristics | |
Spectral type | sdO6p |
U−B color index | −1.259 [2] |
B−V color index | −0.270 [2] |
Variable type | HMXB [3] |
Astrometry | |
Radial velocity (Rv) | 12.10 [4] km/s |
Proper motion (μ) |
RA: −4.73
[1]
mas/
yr Dec.: 5.39 [1] mas/ yr |
Parallax (π) | 1.20 ± 0.50 mas [1] |
Distance | 650 [3] pc |
Orbit [3] | |
Period (P) | 1.55 days |
Eccentricity (e) | 0.0 |
Inclination (i) | 82° |
Details | |
sdO5.5 [5] | |
Mass | 1.50 [3] M☉ |
Radius | 1.45 [6] R☉ |
Luminosity | 3,943 [6] L☉ |
Surface gravity (log g) | 4.25 [6] cgs |
Temperature | 47,500 [6] K |
WD | |
Mass | 1.28 [3] M☉ |
Radius | 1,600 [7] km |
Temperature | 225,000 [7] K |
Other designations | |
Database references | |
SIMBAD | data |
HD 49798 is a binary star in the constellation Puppis about 650 parsecs (circa 2119 light-years) from Earth. It has an apparent magnitude of 8.3, making it one of the brightest known O class subdwarf stars. [8]
HD 49798 was discovered in 1964 to be a rare hydrogen-deficient O class subdwarf, and was the brightest known at the time. [9] This was identified as a binary star, but the companion could not be detected visually or spectroscopically. [10]
The X-ray source RX J0648.0-4418 was discovered close to HD 49798's location in the sky. Only the space telescope XMM-Newton was able to identify the source. It is a white dwarf with about 1.3 solar masses, in orbit about HD 49798 and rotating once every 13 seconds. [11] This is detected from the 13-second X-ray pulse, which results from the stellar wind accreting onto the compact object. [8] It has been proposed that the white dwarf is surrounded by a debris disk. In this model, the material of the disk would be funneled onto the poles of the dwarf via the magnetic field, which would explain the observed X-ray pulses. [8] This system is considered a likely candidate to explode as a type Ia supernova within a few thousand years. [12] [13]