Gliese 588
Star in the constellation Lupus
From Wikipedia, the free encyclopedia
Gliese 588 is a nearby red dwarf star of spectral type M2.5, located in the constellation Lupus at 19.30 light-years from Earth.[1] It emits a very stable light flux, with no detectable pulsations.[5]
  Gliese 588 Location of Gliese 588 in the constellation Lupus | |
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h 32m 12.93231s[1] |
| Declination | −41° 16′ 32.1304″[1] |
| Apparent magnitude (V) | 9.311[2] |
| Characteristics | |
| Spectral type | M2.5V[2] |
| U−B color index | +1.14[3] |
| B−V color index | +1.51[3] |
| Astrometry | |
| Radial velocity (Rv) | 21.06±0.12[1] km/s |
| Proper motion (μ) | RA: -1176.447 mas/yr[1] Dec.: -1030.970 mas/yr[1] |
| Parallax (π) | 168.9965±0.0270 mas[1] |
| Distance | 19.300 ± 0.003 ly (5.9173 ± 0.0009 pc) |
| Absolute magnitude (MV) | 10.44[4] |
| Details[5] | |
| Mass | 0.43±0.05 M☉ |
| Radius | 0.42±0.03 R☉ |
| Surface gravity (log g) | 4.82±0.08 cgs |
| Temperature | 3555±41 K |
| Metallicity [Fe/H] | 0.06±0.08 dex |
| Rotation | 61.3±6.5 d[6] |
| Other designations | |
| CD−40 9712, GJ 588, HIP 76074, LHS 397, LTT 6210, TYC 7844-1976-1, 2MASS J15321302-4116314[2] | |
| Database references | |
| SIMBAD | data |
History of observations
According to Luyten's (1979) (catalogue LHS, as well as NLTT), this object was discovered by Innes.[7][8] In 1903–1927 Innes was the director of the Union Observatory (UO), South Africa.
However, in the Ci 20 catalogue (see number 934) this star was designated as "CD -40 7021", not "UO".[9] This may indicate that GJ 588 was first catalogued earlier, in the Cordoba Durchmusterung by John M. Thome in 1894.[10][11] Note: the real CD designation of Gliese 588 is "CD-40 9712",[12] not "CD -40 7021":[9] GJ 588 has a RA of 15 hours, but the real CD -40 7021 has a RA of 11 hours.[13][10]
Search for planets
In 2019, two planet candidates detected by radial velocity around Gliese 588 were reported in a preprint, among 118 planets around M dwarf stars. These would have minimum masses about 2.4 and 10.3 times that of Earth, and orbit with periods of 5.8 and 206 days.[14] A 2024 study did not find evidence for planets around this star; radial velocity signals with different periods were detected and attributed to intrinsic stellar variability.[15]