| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 18h55m 27.46151s[1] |
| Declination | +06° 36′ 55.1499″[1] |
| Apparent magnitude (V) | 5.57[2] |
| Characteristics | |
| Spectral type | G9 III[3] |
| U−B color index | +0.87[2] |
| B−V color index | +1.041±0.002[4] |
| Astrometry | |
| Radial velocity (Rv) | 23.31±0.09[5] km/s |
| Proper motion (μ) | RA: +7.972[1] mas/yr Dec.: –92.211[1] mas/yr |
| Parallax (π) | 11.5405 ± 0.1636 mas[1] |
| Distance | 283 ± 4 ly (87 ± 1 pc) |
| Absolute magnitude (MV) | 0.87[4] |
| Orbit[5][6] | |
| Primary | HR 7135 A |
| Companion | HR 7135 B |
| Period (P) | 2,994±29 d |
| Semi-major axis (a) | 26.6±3.4 mas |
| Eccentricity (e) | 0.243±0.026 |
| Inclination (i) | 31.9±3.6° |
| Longitude of the node (Ω) | 12.6±7.7° |
| Periastron epoch (T) | 2444276.5±52 JD |
| Argument of periastron (ω) (secondary) | 35±7° |
| Semi-amplitude (K1) (primary) | 4.65±0.13 km/s |
| Details | |
| HR 7135 A | |
| Mass | 1.54[7] M☉ |
| Radius | 10.69+0.17 −0.93[1] R☉ |
| Luminosity | 52.8±0.9[1] L☉ |
| Surface gravity (log g) | 2.7[8] cgs |
| Temperature | 4,666±51[7] K |
| Metallicity [Fe/H] | –0.26[8] dex |
| Rotational velocity (v sin i) | 0.0[8] km/s |
| Age | 3.21[7] Gyr |
| Other designations | |
62 Ser, BD+06°3978, FK5 3509, HD 175515, HIP 92872, HR 7135, SAO 124050[9] | |
| Database references | |
| SIMBAD | data |
HR 7135 is a binary star system. Despite its Flamsteed designationof62 Serpentis, the star can be found in the equatorial constellationofAquila,[10] in front of a dark rift in the Milky Way near the constellation border.[5] It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57.[2] The system is located 283 light years distant from the Sun, based on parallax,[1] and is drifting further away with a radial velocity of 23 km/s.[5]
Discovery of the binary nature of this system is credited to Canadian astronomer H. H. Plaskett in 1922. It is a single-lined spectroscopic binary with an orbital period of 8.2 years and an eccentricity of 0.24.[5][6] The visible component is an aging giant star with a stellar classification of G9 III,[3] having exhausted the supply of hydrogen at its core and expanded to 10.7[1] times the Sun's radius. It is a red clump giant, indicating it is on the horizontal branch and is generating energy via core helium fusion.[11] The star is 3.2[7] billion years old with 1.54[7] times the mass of the Sun. It is radiating 53[1] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,666 K.[7] The star has a very low rate of spin, with the projected rotational velocity being too small to measure.[8]
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