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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]
Location of Gliese 588 in the constellation Lupus | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
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 | |
Database references | |
SIMBAD | data |
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]
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 intrinstic stellar variability.[15]
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b (unconfirmed) | ≥2.4+1.0 −0.9 M🜨 |
0.049±0.005 | 5.8084+0.0016 −0.0018 |
0.04+0.25 −0.04 |
— | — |
c (unconfirmed) | ≥10.3+6.9 −4.9 M🜨 |
0.530+0.048 −0.054 |
206.0+2.0 −3.3 |
0.06+0.02 −0.06 |
— | — |
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