LS IV-14 116
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Aquarius[2] |
| Right ascension | +20h 57m 38.875s[3] |
| Declination | −14° 25′ 44.01″[3] |
| Apparent magnitude (V) | +12.93[4] |
| Characteristics | |
| Spectral type | sdB0.5VIIHe18[5] |
| B−V color index | −0.16[4] |
| Variable type | sdBVr[6][7] |
| Astrometry | |
| Proper motion (μ) | RA: +7.409 mas/yr[3] Dec.: −128.265 mas/yr[3] |
| Parallax (π) | 2.3406±0.0543 mas[3] |
| Distance | 1,390 ± 30 ly (427 ± 10 pc) |
| Details | |
| Mass | 0.38[8] M☉ |
| Radius | 0.122[8] R☉ |
| Luminosity | 21[8] L☉ |
| Surface gravity (log g) | 5.94±0.04[9] cgs |
| Temperature | 34,950±250[9] K |
| Other designations | |
| 2MASS J20573887-1425437, UCAC4 378-169675, V366 Aquarii | |
| Database references | |
| SIMBAD | data |
LS IV-14 116 is a hot subdwarf located approximately 2,000 light years away on the border between the constellations Capricornus and Aquarius. It has a surface temperature of approximately 34,000 ± 500 kelvins.[10] Along with stars HE 2359-2844 and HE 1256-2738, LS IV-14 116 forms a new group of star called heavy metal subdwarfs. These are thought to be stars contracting to the extended horizontal branch after a helium flash and ejection of their atmospheres at the tip of the red giant branch.[11]
Amir Ahmad and C. Simon Jeffery discovered that the star is a variable star, in 2004, and published their discovery in 2005. They detected two pulsation periods, 1950 and 2900 seconds.[13] The star's atmosphere contains 10,000 times more zirconium (per unit mass) than the Sun's; it also has between 1,000 and 10,000 times the amount of strontium, germanium and yttrium than the Sun. The heavy metals are believed to be in cloud layers in the atmosphere where the ions of each metal have a particular opacity that allows radiational levitation to balance gravitational settling.[10]
