Mu Telescopii
Star in the constellation Telescopium
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Mu Telescopii, Latinized from μ Telescopii is a solitary star in the southern constellation Telescopium. It has an apparent visual magnitude of 6.28,[2] placing it near the limit of naked eye visibility. The object is relatively close at a distance of 118 light years[1] but is receding with a heliocentric radial velocity of 8.6 km/s.[5]
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Telescopium |
| Right ascension | 19h 30m 34.6118s[1] |
| Declination | −55° 06′ 36.190″[1] |
| Apparent magnitude (V) | 6.28±0.01[2] |
| Characteristics | |
| Evolutionary stage | main sequence[1] |
| Spectral type | F5 V[3] |
| B−V color index | +0.45[4] |
| Astrometry | |
| Radial velocity (Rv) | 8.6±0.3[5] km/s |
| Proper motion (μ) | RA: +38.548 mas/yr[1] Dec.: −11.540 mas/yr[1] |
| Parallax (π) | 27.6727±0.0284 mas[1] |
| Distance | 117.9 ± 0.1 ly (36.14 ± 0.04 pc) |
| Absolute magnitude (MV) | +3.61[6] |
| Details | |
| Mass | 1.28[7] M☉ |
| Radius | 1.40+0.07 −0.05[8] R☉ |
| Luminosity | 3.22±0.01[9] L☉ |
| Surface gravity (log g) | 4.3±0.1[8] cgs |
| Temperature | 6,570±136[10] K |
| Metallicity [Fe/H] | −0.06[11] dex |
| Rotational velocity (v sin i) | 6.9±0.5[12] km/s |
| Age | 2.12[11] Gyr |
| Other designations | |
| μ Tel, 61 G. Telescopii, CPD−55°8188, HD 183028, HIP 95932, HR 7393, SAO 246131[13][14] | |
| Database references | |
| SIMBAD | data |
Mu Telescopii has a stellar classification of F5 V,[3] indicating that it is an ordinary F-type main sequence star. It has been noted to be chromospherically active.[3] The star is 2.12 billion years[11] old with a current mass of 1.28 M☉,[7] and has a diameter 1.4 times that of the Sun. It is radiating 3.22 times the luminosity of the Sun[9] from its photosphere at an effective temperature of 6,570 K,[10] giving a yellow white hue. Mu Telescopii is slightly metal deficient with an iron abundance 87% that of the Sun[11] and spins with a projected rotational velocity of 6.9 km/s.[12]
It has been observed for infrared excess suggesting the presence of a debris disk but so far, none has been found.[15]