Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge.[11] Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years (3.6 parsecs) from the Sun. This positions the pair among the nearest stars to the Solar System.
 Ultraviolet band light curves for GX Andromedae, with flares marked by red arrows. Adapted from Pettersen and Griffin (1980)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Groombridge 34 A | |
| Right ascension | 00h 18m 22.88498s[2] |
| Declination | +44° 01′ 22.6380″[2] |
| Apparent magnitude (V) | 8.119[3] |
| Groombridge 34 B | |
| Right ascension | 00h 18m 25.82514s[4] |
| Declination | +44° 01′ 38.0924″[4] |
| Apparent magnitude (V) | 11.007[3] |
| Characteristics | |
| Spectral type | M1.4V + M4.1V[3] |
| U−B color index | +1.24/+1.40[5] |
| B−V color index | +1.56/+1.80[5] |
| Variable type | Flare stars |
| Astrometry | |
| Groombridge 34 A | |
| Radial velocity (Rv) | +11.62±0.08[6] km/s |
| Proper motion (μ) | RA: 2,891.518 mas/yr[2] Dec.: 411.832 mas/yr[2] |
| Parallax (π) | 280.7068 ± 0.0203 mas[2] |
| Distance | 11.6191 ± 0.0008 ly (3.5624 ± 0.0003 pc) |
| Absolute magnitude (MV) | 10.32[citation needed] |
| Groombridge 34 B | |
| Radial velocity (Rv) | 10.60±0.15[4] km/s |
| Proper motion (μ) | RA: 2,862.796 mas/yr[4] Dec.: 336.432 mas/yr[4] |
| Parallax (π) | 280.6947 ± 0.0278 mas[4] |
| Distance | 11.620 ± 0.001 ly (3.5626 ± 0.0004 pc) |
| Absolute magnitude (MV) | 13.3[citation needed] |
| Orbit[7] | |
| Period (P) | 1230+930 −110 yr |
| Semi-major axis (a) | 93+42 −6 AU |
| Eccentricity (e) | 0.53+0.23 −0.28 |
| Inclination (i) | 54+11 −16° |
| Longitude of the node (Ω) | 2+35 −43° |
| Periastron epoch (T) | 7140+560 −140 |
| Details | |
| Groombridge 34 A | |
| Mass | 0.393+0.009 −0.008[8] M☉ |
| Radius | 0.385±0.002[8] R☉ |
| Luminosity | 0.02249±0.00019[8] L☉ |
| Habitable zone inner limit | 0.112[9] AU |
| Habitable zone outer limit | 0.239[9] AU |
| Surface gravity (log g) | 4.87±0.04[7] cgs |
| Temperature | 3,601+12 −11[8] K |
| Metallicity [Fe/H] | −0.34±0.09[7] dex |
| Rotation | 43.86±0.56 days[7] |
| Rotational velocity (v sin i) | 1.09±0.79[7] km/s |
| Age | ~3.02[3] Gyr |
| Groombridge 34 B | |
| Mass | 0.15±0.02[7] M☉ |
| Radius | 0.18±0.03[7] R☉ |
| Luminosity | ~8.5×10−4[7] L☉ |
| Habitable zone inner limit | 0.048[9] AU |
| Habitable zone outer limit | 0.103[9] AU |
| Surface gravity (log g) | 5.08±0.15[7] cgs |
| Temperature | 3304±70[7] K |
| Metallicity [Fe/H] | −0.37±0.10[3] dex |
| Age | ~2.754[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | GJ 15 A |
| GJ 15 Ab | |
| GJ 15 B | |
| ARICNS | GJ 15 A |
| GJ 15 B | |
  Groombridge 34 Location of Groombridge 34 in the constellation Andromeda | |
Both components are small, dim red dwarf stars that are too faint to be seen with the naked eye. They orbit around their common barycenter in a fairly eccentric orbit with a separation of about 93 AU and a period of around 1,230 years.[7] Both stars exhibit random variation in luminosity due to flares and they have been given variable star designations: the brighter member Groombridge 34 A is designated GX And, while the smaller component is designated GQ And.[12]
The star system has a relatively high proper motion of 2.9 arc seconds per year,[13] and is moving away from the Solar System at a velocity of 11.6 km/s.[6] It achieved perihelion some 15,000 years ago when it came within 11 ly (3.5 pc) of the Sun.[13]
GX Andromedae
editThe more massive and luminous component of the pair has the variable star designation GX Andromedae. It is a main-sequence red dwarf star of spectral type M1.4[3] that varies its brightness due to stellar flares. Gaia observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.[14]
GQ Andromedae
editThe smaller companion bears the variable star name GQ Andromedae. It is a red dwarf main sequence star that undergoes flare events like the primary; it has a spectral type M4.1,[3] so it also has a lower effective temperature.
Planetary system
editIn August 2014, a planet orbiting around Groombridge 34 A was reported.[15] The planet's existence was deduced from analysis of the radial velocities of the parent star by the Eta-Earth Survey using HIRES at Keck Observatory. At the time of its discovery, it was the sixth-nearest-known exoplanet.
Using the CARMENES spectrograph combined with the measurements of the HARPS and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.[16]
This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 ME for Groombridge 34 Ab and 36 ME for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fourth-closest confirmed multi-planet system to the Sun, hosting the longest-period Neptune-mass exoplanet discovered so far.[7]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥3.03+0.46 −0.44 M🜨 |
0.072+0.003 −0.004 |
11.4407+0.0017 −0.0016 |
0.094+0.091 −0.065 |
— | — |
| c | ≥36+25 −18 M🜨 |
5.4+1.0 −0.9 |
~7,600 | 0.27+0.28 −0.19 |
— | — |
See also
editReferences
edit- ^ Pettersen, B. R.; Griffin, R. F. (December 1980). "Non-emission-line flare stars". The Observatory. 100: 198–202. Bibcode:1980Obs...100..198P. Retrieved 30 October 2022.
- ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g h Mann, Andrew W.; et al. (May 2015), "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius", The Astrophysical Journal, 804 (1): 38, arXiv:1501.01635, Bibcode:2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64, S2CID 19269312, 64.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
- ^ a b c d e f g h i j k l m Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv:1804.03476. Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID 54990041.
- ^ a b c d Pineda, J. Sebastian; Youngblood, Allison; France, Kevin (September 2021). "The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars". The Astrophysical Journal. 918 (1): 23. arXiv:2106.07656. Bibcode:2021ApJ...918...40P. doi:10.3847/1538-4357/ac0aea. S2CID 235435757. 40.
- ^ a b c d Cantrell, Justin R.; et al. (October 2013), "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors", The Astronomical Journal, 146 (4): 99, arXiv:1307.7038, Bibcode:2013AJ....146...99C, doi:10.1088/0004-6256/146/4/99, S2CID 44208180.
- ^ "V* GX And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-02-09.
{{cite web}}: CS1 maint: postscript (link) - ^ Groombridge, Stephen (1838), Airy, George Biddell (ed.), A Catalogue of Circumpolar Stars, J. Murray, p. 2.
- ^ Petit, M. (October 1990), "Catalogue des étoiles variables ou suspectes dans le voisinage du Soleil", Astronomy and Astrophysics Supplement (in French), 85 (2): 971, Bibcode:1990A&AS...85..971P.
- ^ a b Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
- ^ Morris, Brett M.; Agol, Eric; Davenport, James R. A.; Hawley, Suzanne L. (2018). "Spotting stellar activity cycles in Gaia astrometry". Monthly Notices of the Royal Astronomical Society. 476 (4): 5408. arXiv:1802.09943. Bibcode:2018MNRAS.476.5408M. doi:10.1093/mnras/sty568. S2CID 73564680.
- ^ Howard, Andrew W.; et al. (October 2014), "The NASA-UC-UH ETA-Earth Program. IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth", The Astrophysical Journal, 794 (1): 9, arXiv:1408.5645, Bibcode:2014ApJ...794...51H, doi:10.1088/0004-637X/794/1/51, S2CID 17361592, 51.
- ^ Trifonov, Trifon; Kürster, Martin; Zechmeister, Mathias; Tal-Or, Lev; Caballero, José A.; Quirrenbach, Andreas; Amado, Pedro J.; Ribas, Ignasi; Reiners, Ansgar; et al. (2018). "The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems". Astronomy and Astrophysics. 609. A117. arXiv:1710.01595. Bibcode:2018A&A...609A.117T. doi:10.1051/0004-6361/201731442. S2CID 119340839.