Groombridge 34 or ADS 246 A
Observation data
Epoch J2000 Equinox J2000 |
| Constellation |
Andromeda |
| Right ascension |
00h 18m 22.89s [1] |
| Declination |
+44° 01′ 22.6″ [1] |
| Apparent magnitude (V) |
8.09/11.06 |
| Characteristics |
| Spectral type |
M1.5V / M3.5V |
| U−B color index |
1.24 |
| B−V color index |
1.56 |
| Variable type |
Flare stars |
| Astrometry |
|
| Radial velocity (Rv) |
+12.0 km/s |
| Proper motion (μ) |
RA: 2888.92 ± 0.60 [1] mas/yr
Dec.: 410.10 ± 0.48 [1] mas/yr |
| Parallax (π) |
278.76 ± 0.77[1] mas |
| Distance |
11.7 ± 0.03 ly
(3.587 ± 0.01 pc) |
| Absolute magnitude (MV) |
10.33/13.29 |
|
| Orbit |
| Companion |
Groombridge 34 B
Gl 15 B |
| Period (P) |
2,600 yr |
| Semimajor axis (a) |
41.15" |
| Eccentricity (e) |
0.00 |
| Inclination (i) |
61.4° |
| Longitude of the node (Ω) |
45.3° |
| Periastron epoch (T) |
1745 |
| Details |
|
| Mass |
0.404[2] / 0.163 M☉ |
| Radius |
0.379±0.006[2] / 0.19 R☉ |
| Surface gravity (log g) |
4.89[2] |
| Luminosity |
0.0064 / 0.00042 L☉ |
| Temperature |
3,730±49[2] / ~3,000 K |
| Metallicity |
[Fe/H] = −0.46[2] |
|
| Other designations |
GX/GQ Andromedae, HD 1326, GCTP 49, BD +43°44, LHS 3/4, GJ 15 A/B, Gl 171-047/171-048, SAO 36248, LTT 10108/10109, LFT 31/32, Vys 085 A/B HIP 1475. |
| Database references |
| SIMBAD |
data |
| Database references |
| SIMBAD |
data |
Groombridge 34 is a binary star system located about 11.7 light years from our own Sun. It consists of two red dwarf stars in a nearly circular orbit with a separation of about 147 astronomical units. Both stars in this pair exhibit variability due to random flares and they have been given variable star designations. (The brighter member Groombridge 34 A is designated GX And, and the other member is designated GQ And).
[edit] See also
[edit] References
- Lippincott, S. L., "Parallax and orbital motion of the 2 nearby long-period visual binaries Groombridge 34 and ADS 9090", 1972, Astronomical Journal, 77, 165.
[edit] External links
[edit] Components
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In left column are stellar classes of primary members of star systems. ‡Distance error margin extends out of declared distance interval. Bold are systems containing at least one component with absolute magnitude of +8.5 or brighter. Italic are systems possibly located within declared distance interval, but probably not.
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