GG Lupi
| Observation data EpochJ2000EquinoxJ2000 | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h18m56.3747s[2] |
| Declination | −40° 47′ 17.597″[2] |
| Apparent magnitude(V) | 5.58 - 6.11[3] |
| Characteristics | |
| Spectral type | B7V (primary) B9V (secondary) |
| U−Bcolor index | −0.46[4] |
| B−Vcolor index | −0.099[4] |
| Variable type | Algol[3] |
| Astrometry | |
| Radial velocity(Rv) | +4.0±1.0[4]km/s |
| Proper motion(μ) | RA:−19.219[2]mas/yr Dec.:−21.791[2]mas/yr |
| Parallax(π) | 6.6639 ± 0.0894mas[2] |
| Distance | 489 ± 7ly (150 ± 2pc) |
| Absolute magnitude(MV) | −0.53[5] |
| Orbit[4] | |
| Period(P) | 1.8495927d |
| Semi-major axis(a) | 12.01AU |
| Eccentricity(e) | 0.15 |
| Inclination(i) | 87.5° |
| Details | |
| Primary | |
| Mass | 4.16±0.12[4]M☉ |
| Radius | 2.42±0.05[4]R☉ |
| Surface gravity(logg) | 4.28[4]cgs |
| Temperature | 13,000[4]K |
| Rotational velocity(vsini) | 97±8[6]km/s |
| Secondary | |
| Mass | 2.64±0.12[4]M☉ |
| Radius | 1.79±0.04[4]R☉ |
| Surface gravity(logg) | 4.30[4]cgs |
| Temperature | 10,600[4]K |
| Rotational velocity(vsini) | 61±5[6]km/s |
| Age | 20[7]Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
GG Lupiis aneclipsing binarystar in the southern constellation ofLupus.Most of the time it is amagnitude5.6 object, making it faintly visible to the naked eye, but during the primary eclipse its brightness falls to 6.1.[3]GG Lupi is located 1/2 degree (one full moon diameter) west of the 3rd magnitude starDelta Lupi.
This star was found to be aspectroscopic binaryin 1930,[9]and its eclipses were detected in observations during 1964.[10]Its location in the sky, distance (~490light years)[2]andproper motionmake it a likely member of theScorpius–Centaurus Associationwithin theGould's Beltstar formation region.[4] The two stars comprising this binary are both very young main sequence stars ofspectral type B.They are estimated to be about 20 million years old, placing them near thezero-age main sequence.[7]Their orbit is somewhat eccentric (e=0.15) and the period ofapsidal precessionis 102 years.[11]
References
[edit]- ^"MAST: Barbara A. Mikulski Archive for Space Telescopes".Space Telescope Science Institute.Retrieved10 December2022.
- ^abcdefVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData 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.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
- ^abc"GG Lup".The International Variable Star Index.AAVSO.Retrieved10 December2022.
- ^abcdefghijklmBudding, E.; Butland, R.; Blackford, M. (April 2015)."Absolute parameters of young stars: GG Lup and μ1 Sco".Monthly Notices of the Royal Astronomical Society.448(4): 3784–3796.arXiv:1502.04360.Bibcode:2015MNRAS.448.3784B.doi:10.1093/mnras/stv234.
- ^Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38(5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015.S2CID119257644.
- ^abMarcussen, Marcus L.; Albrecht, Simon H. (2022)."The BANANA Project. VI. Close Double Stars are Well Aligned with Noticeable Exceptions; Results from an Ensemble Study Using Apsidal Motion and Rossiter-McLaughlin Measurements".The Astrophysical Journal.933(2): 227.arXiv:2112.00824.Bibcode:2022ApJ...933..227M.doi:10.3847/1538-4357/ac75c2.S2CID244799745.
- ^abAndersen, J.; Clausen, J. V.; Gimenez, A. (October 1993). "Absolute dimensions of eclipsing binaries. XX. GG LUPI: young metal-deficient B stars".Astronomy and Astrophysics.277:439–451.Bibcode:1993A&A...277..439A.
- ^"V* GG Lup -- Eclipsing Binary".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2022-12-10.
- ^Neubauer, F. J. (August 1930). "Forty-two Spectroscopic Binary Stars".Publications of the Astronomical Society of the Pacific.42(248): 235.Bibcode:1930PASP...42..235N.doi:10.1086/124043.S2CID121035980.
- ^Smith, Lindsey F. (April 1966)."HR 5687: A New Eclipsing Binary".Publications of the Astronomical Society of the Pacific.78(462): 168.Bibcode:1966PASP...78..168S.doi:10.1086/128320.S2CID120477301.
- ^Wolf, M.; Zejda, M. (July 2005)."Apsidal motion in southern eccentric eclipsing binaries: V539 Ara, GG Lup, V526 Sgr and AO Vel".Astronomy and Astrophysics.437(2): 545–551.Bibcode:2005A&A...437..545W.doi:10.1051/0004-6361:20041868.S2CID121307009.
