HR 7135
Star in the constellation Aquila
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HR 7135 is a binary star system. Despite its Flamsteed designation of 62 Serpentis, the star can be found in the equatorial constellation of Aquila,[11] in front of a dark rift in the Milky Way near the constellation border.[6] It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57.[3] The system is located 283 light years distant from the Sun, based on parallax,[2] and is drifting further away with a radial velocity of 23 km/s.[6]
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Aquila[1] |
| Right ascension | 18h 55m 27.46151s[2] |
| Declination | +06° 36′ 55.1499″[2] |
| Apparent magnitude (V) | 5.57[3] |
| Characteristics | |
| Evolutionary stage | red clump[4] |
| Spectral type | G9 III[5] |
| U−B color index | +0.87[3] |
| B−V color index | +1.041±0.002[1] |
| Astrometry | |
| Radial velocity (Rv) | 23.31±0.09[6] km/s |
| Proper motion (μ) | RA: +7.972[2] mas/yr Dec.: −92.211[2] mas/yr |
| Parallax (π) | 11.5405±0.1636 mas[2] |
| Distance | 283 ± 4 ly (87 ± 1 pc) |
| Absolute magnitude (MV) | 0.87[1] |
| Orbit[6][7] | |
| Primary | HR 7135 A |
| Name | 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[8] M☉ |
| Radius | 10.69+0.17 −0.93[2] R☉ |
| Luminosity | 52.8±0.9[2] L☉ |
| Surface gravity (log g) | 2.7[9] cgs |
| Temperature | 4,666±51[8] K |
| Metallicity [Fe/H] | −0.26[9] dex |
| Rotational velocity (v sin i) | 0.0[9] km/s |
| Age | 3.21[8] Gyr |
| Other designations | |
| 62 Ser, BD+06°3978, FK5 3509, HD 175515, HIP 92872, HR 7135, SAO 124050[10] | |
| Database references | |
| SIMBAD | data |
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.[6][7] The visible component is an aging giant star with a stellar classification of G9 III,[5] having exhausted the supply of hydrogen at its core and expanded to 10.7[2] 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.[4] The star is 3.2[8] billion years old with 1.54[8] times the mass of the Sun. It is radiating 53[2] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,666 K.[8] The star has a very low rate of spin, with the projected rotational velocity being too small to measure.[9]