Rho Telescopii
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Telescopium |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | +5.17[2] |
| Characteristics | |
| Spectral type | F6 V[3] |
| B−V Template:Engvar | +0.53[2] |
| Astrometry | |
| Radial velocity (Rv) | Template:Val[4] km/s |
| Proper motion (μ) | RA: +32.47[1] mas/yr Dec.: −115.24[1] mas/yr |
| Parallax (π) | 17.63±0.59 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | 1.69[5] |
| Details | |
| Mass | 1.97[4] Template:Solar mass |
| Luminosity | 25.6[6] Template:Solar luminosity |
| Surface gravity (log g) | 3.51[4] cgs |
| Temperature | Template:Val[4] K |
| Metallicity [Fe/H] | +0.01[7] dex |
| Rotational velocity (v sin i) | Template:Val[5] km/s |
| Age | 1.30[4] Gyr |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist[8] | |
| Database references | |
| SIMBAD | data |
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Rho Telescopii (ρ Tel, ρ Telescopii) is an astrometric binary[9] star system in the southern constellation of Telescopium. It is visible to the naked eye, with an apparent visual magnitude of +5.17.[2] Based upon an annual parallax shift of 17.63 mas as measured from Earth,[1] it is located approximately 185 light years from the Sun.
This appears to be a single-lined spectroscopic binary as it displays radial velocity variation with a period of 1.7 days.[9] The visible component is an F-type main sequence star with a stellar classification of F6 V.[3] It has about double the mass of the Sun and is radiating 25.6[6] times the solar luminosity from its photosphere at an effective temperature of 6,303 K.[4] The star is a bright X-ray source with a luminosity of Template:Val.[10]
Relative to neighboring stars, Rho Telescopii has a peculiar velocity of 17.2 km s−1.[11] It may be a member of the Tucana-Horologium association.[12]
| Age | Source |
|---|---|
| Template:Val Myr | Tetzlaff et al. (2011)[11] |
| 30 Myr | Lagrange et al. (2013)[9] |
| 0.20 Gyr | Ballering et al. (2013)[13] |
| 1.30 Gyr | Casagrande et al. (2011)[4] |
References
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