GG Lupi
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h 18m 56.3747s[1] |
| Declination | −40° 47′ 17.597″[1] |
| Apparent magnitude (V) | 5.58–6.11[2] |
| Characteristics | |
| Spectral type | B7V (primary) B9V (secondary) |
| U−B color index | −0.46[3] |
| B−V color index | −0.099[3] |
| Variable type | Algol[2] |
| Astrometry | |
| Radial velocity (Rv) | +4.0±1.0[3] km/s |
| Proper motion (μ) | RA: −19.219[1] mas/yr Dec.: −21.791[1] mas/yr |
| Parallax (π) | 6.6639±0.0894 mas[1] |
| Distance | 489 ± 7 ly (150 ± 2 pc) |
| Absolute magnitude (MV) | −0.53[4] |
| Orbit[3] | |
| Period (P) | 1.8495927 d |
| Semi-major axis (a) | 12.01 AU |
| Eccentricity (e) | 0.15 |
| Inclination (i) | 87.5° |
| Details | |
| Primary | |
| Mass | 4.16±0.12[3] M☉ |
| Radius | 2.42±0.05[3] R☉ |
| Surface gravity (log g) | 4.28[3] cgs |
| Temperature | 13,000[3] K |
| Rotational velocity (v sin i) | 97±8[5] km/s |
| Secondary | |
| Mass | 2.64±0.12[3] M☉ |
| Radius | 1.79±0.04[3] R☉ |
| Surface gravity (log g) | 4.30[3] cgs |
| Temperature | 10,600[3] K |
| Rotational velocity (v sin i) | 61±5[5] km/s |
| Age | 20[6] Myr |
| Other designations | |
| HD 135876, HIP 74950, HR 5687, SAO 225647, 2MASS J15185637-4047176[7] | |
| Database references | |
| SIMBAD | data |
GG Lupi is an eclipsing binary star in the southern constellation of Lupus. Most of the time it is a magnitude 5.6 object, making it faintly visible to the naked eye, but during the primary eclipse its brightness falls to 6.1.[2] GG Lupi is located one half-degree (one full moon diameter) west of the third-magnitude star Delta Lupi.
This star was found to be a spectroscopic binary in 1930,[9] and its eclipses were detected in observations during 1964.[10] Its location in the sky, distance (~490 light-years)[1] and proper motion make it a likely member of the Scorpius–Centaurus association within the Gould's Belt star-formation region.[3] The two stars comprising this binary are both very young main-sequence stars of spectral type B. They are estimated to be about 20 million years old, placing them near the zero-age main sequence.[6] Their orbit is somewhat eccentric (e=0.15) and the period of apsidal precession is 102 years.[11]
References
- ^ a b c d e f 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 "GG Lup". The International Variable Star Index. AAVSO. Retrieved 10 December 2022.
- ^ a b c d e f g h i j k l m Budding, 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. S2CID 119257644.
- ^ a b Marcussen, 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. S2CID 244799745.
- ^ a b Andersen, 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. Retrieved 2022-12-10.
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 10 December 2022.
- ^ 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. S2CID 121035980.
- ^ 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. S2CID 120477301.
- ^ 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. S2CID 121307009.