Gliese 752
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Gliese 752 A | |
| Right ascension | 19h 16m 55.257s[1] |
| Declination | +05° 10′ 08.05″[1] |
| Apparent magnitude (V) | ~9.13[1] |
| Gliese 752 B | |
| Right ascension | 19h 16m 57.62s[2] |
| Declination | +05° 09′ 02.2″[2] |
| Apparent magnitude (V) | ~17.30[2] |
| Characteristics | |
| Gliese 752 A | |
| Spectral type | M2.5[1] |
| Apparent magnitude (B) | ~10.63[1] |
| Apparent magnitude (V) | ~9.13[1] |
| Apparent magnitude (R) | ~8.3[1] |
| Apparent magnitude (J) | ~5.58[1] |
| Apparent magnitude (H) | ~4.93[1] |
| Apparent magnitude (K) | ~4.67[1] |
| Variable type | BY[3] |
| Gliese 752 B | |
| Spectral type | M8V[2] |
| Apparent magnitude (B) | ~19.42[2] |
| Apparent magnitude (V) | ~17.30[2] |
| Apparent magnitude (R) | ~15.6[2] |
| Apparent magnitude (J) | 9.908 ± 0.025[2] |
| Apparent magnitude (H) | 9.226 ± 0.026[2] |
| Apparent magnitude (K) | 8.765 ± 0.022[2] |
| Variable type | UV[4] |
| Astrometry | |
| A | |
| Proper motion (μ) | RA: −579[5] mas/yr Dec.: −1333[5] mas/yr |
| Parallax (π) | 169.0615 ± 0.0239[6] mas |
| Distance | 19.292 ± 0.003 ly (5.9150 ± 0.0008 pc) |
| Absolute magnitude (MV) | 10.13[7] |
| B | |
| Proper motion (μ) | RA: −598[8] mas/yr Dec.: −1365[8] mas/yr |
| Parallax (π) | 168.9537 ± 0.0668[9] mas |
| Distance | 19.304 ± 0.008 ly (5.919 ± 0.002 pc) |
| Absolute magnitude (MV) | 18.7[10] |
| Details | |
| Gliese 752 A | |
| Mass | 0.46[7] M☉ |
| Radius | 0.546[7] R☉ |
| Luminosity (bolometric) | 0.0326 ± 0.0004[11] L☉ |
| Temperature | 3354±51[12] K |
| Metallicity | –0.05 ± 0.17[13] |
| Rotation | 46.5±0.3 d[14] |
| Gliese 752 B | |
| Mass | 0.075 ±.05[15] M☉ |
| Radius | ~0.102[7] R☉ |
| Temperature | ~2600[7] K |
| Age | ~1[15] Gyr |
| Other designations | |
| Gliese 752 A: V1428 Aql, HD 180617, HIP 94761, Ross 652, Wolf 1055, TYC 472-1252-1, GSC 00472-01252, 2MASS J19165526+0510086[1] | |
| Gliese 752 B: VB 10, V1298 Aql, 2MASS J19165762+0509021[2] | |
| Database references | |
| SIMBAD | AB |
| A | |
| vB 10 (B) | |
Gliese 752 is a binary star system in the Aquila constellation. This system is relatively nearby, at a distance of about 19 light years.[7] This system consists of two M-type stars. The primary star is the magnitude 9 Gliese (GJ) 752 A. The secondary star is the dim magnitude 17 Gliese (GJ) 752 B, more commonly referred to as VB 10. This stellar pair form a binary star system separated by about 74 arc seconds (~434 AU).[10] This system is also known for its high proper motion of about 1 arc second a year.
In August 2018, a group of scientist using measurements taken from the CARMENES spectrograph, on the Calar Alto Observatory located in Spain, announced they had detected a planet orbiting the larger of the stars, HD 180617 (Gliese 752 A). The measurements indicated the presence of a planet with a minimum mass comparable to Neptune on an orbit partly located within the habitable zone.[11]
The name and number are from the Catalogue of Nearby Stars, published by German astronomer Wilhelm Gliese in 1969.[16]
Interior dynamics of the Gliese 752 stars[]
Before the Hubble Space Telescope observation of Gliese 752 system, astronomers thought magnetic fields in stars required the same dynamo process that creates magnetic fields on the Sun. In the classic solar model heat generated by nuclear fusion reactions at the star's center escapes through a radiative zone just outside the core. The heat travels from the radiative core to the star's surface through a convection zone. In this region, heat bubbles to the surface by motions similar to boiling in a pot of water.
Dynamos, which accelerate electrons to create magnetic forces, operate when the interior of a star rotates faster than its surface. Recent studies of the Sun indicate its convection zone rotates at nearly the same rate at all depths. This means the solar dynamo must operate in the more rapidly rotating radiative core just below the convective zone.[17]
Gliese 752 A characteristics[]
The primary star, also known as Wolf 1055, is a type M2.5 red dwarf with about half the size and mass as the Sun and considerably cooler at 3354±51 K.[12] This star was first observed to be a high proper motion star by the German astronomer Max Wolf with his pioneering use of astrophotography. He added this star to his extensive catalog of such stars in 1919.[18] It is a variable star with the variable star catalog name V1428 Aquilae. It is a BY Draconis type variable star subject to flare events.[1][3]
Planetary system[]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥12.204±1.05[12] M
|