Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Cetus |
Right ascension | 01h 36m 13.61558s[2] |
Declination | −11° 20′ 32.6318″[2] |
Apparent magnitude (V) | 14.16±0.01[3] |
Characteristics | |
Evolutionary stage | White dwarf |
Spectral type | DA4.0[4] |
U−B color index | −0.5[5] |
B−V color index | 0.2[5] |
Variable type | ZZ Cet (DAV)[5] |
Astrometry | |
Proper motion (μ) | RA: +460.845[2] mas/yr Dec.: −116.448[2] mas/yr |
Parallax (π) | 30.5249 ± 0.0546 mas[2] |
Distance | 106.8 ± 0.2 ly (32.76 ± 0.06 pc) |
Absolute magnitude (MV) | 11.78±0.06[6] |
Details[6] | |
Mass | 0.65±0.02 M☉ |
Radius | 0.0118±0.0002 R☉ |
Luminosity | 0.0029±0.0002 L☉ |
Surface gravity (log g) | 8.108±0.025 cgs |
Temperature | 12,281±125 K |
Rotation | 37.84±1.99 h |
Other designations | |
Database references | |
SIMBAD | data |
Ross 548 is a white dwarf in the equatorial constellation of Cetus.[7] With a mean apparent visual magnitude of 14.2[3] it is much too faint to be visible to the naked eye. Based on parallax measurements, it is located at a distance of 107 light years from the Sun.[2] It was found to be variable in 1970[8] and in 1972 it was given the variable star designation ZZ Ceti.[9] This is a pulsating white dwarf of the DAV type that is the prototype of the ZZ Ceti variable class.[10], pp. 891, 895.[3]
This DA-class white dwarf is the surviving core of a red giant star that ceased nuclear fusion while shedding its outer envelope. It has a (presumably) homogeneous core of carbon and oxygen, a relatively thin outer envelope of hydrogen, and a helium mantle. The object has 65% of the mass of the Sun, with 1.2% of the Sun's radius. It is radiating 0.3% of the luminosity of the Sun at an effective temperature of 12,281 K. Ross 548 is spinning with a period of ~38 hours.[6] The dominant pulsation mode of this object has a period of 213.1326 seconds. It has up to 11 known pulsation modes in total.[3]
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