GG Lupi

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GG Lupi
GGLupLightCurve.png
A light curve for GG Lupi, plotted from TESS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Lupus
Right ascension 15h 18m 56.3747s [2]
Declination −40° 47′ 17.597″ [2]
Apparent magnitude  (V)5.58 - 6.11 [3]
Characteristics
Spectral type B7V (primary) B9V (secondary)
U−B color index −0.46 [4]
B−V color 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 ± 0.0894  mas [2]
Distance 489 ± 7  ly
(150 ± 2  pc)
Absolute magnitude  (MV)−0.53 [5]
Orbit [4]
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 [4]   M☉
Radius 2.42±0.05 [4]   R☉
Surface gravity (log g)4.28 [4]   cgs
Temperature 13,000 [4]   K
Rotational velocity (v sin i)97±8 [6]  km/s
Secondary
Mass 2.64±0.12 [4]   M☉
Radius 1.79±0.04 [4]   R☉
Surface gravity (log g)4.30 [4]   cgs
Temperature 10,600 [4]   K
Rotational velocity (v sin i)61±5 [6]  km/s
Age 20 [7]   Myr
Other designations
HD  135876, HIP  74950, HR  5687, SAO  225647, 2MASS J15185637-4047176 [8]
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. [3] GG Lupi is located 1/2 degree (one full moon diameter) west of the 3rd 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) [2] and proper motion make it a likely member of the Scorpius–Centaurus Association within the Gould's Belt star formation region. [4] 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. [7] Their orbit is somewhat eccentric (e=0.15) and the period of apsidal precession is 102 years. [11]

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<span class="mw-page-title-main">Gamma Lupi</span>

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Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

<span class="mw-page-title-main">HR 7484</span> Star in the constellation Cygnus

HR 7484 is a binary star system in the northern constellation of Cygnus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 24.71, it is located 132 light years away. The system is moving closer with a heliocentric radial velocity of −14 km/s.

<span class="mw-page-title-main">DH Cephei</span> Binary star system in the constellation Cepheus

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<span class="mw-page-title-main">GG Carinae</span>

GG Carinae is a binary star system in the southern constellation of Carina, abbreviated GG Car. It is a variable star with a brightness that fluctuates around an apparent visual magnitude of 8.67, making it too faint to be visible to the naked eye. The distance to this system is approximately 8,000 light years based on parallax measurements.

<span class="mw-page-title-main">Y Cygni</span> Binary star in the constellation Cygnus

Y Cygni is an eclipsing and double-lined spectroscopic binary star system in the constellation of Cygnus. It is located about 4,900 light-years from Earth. The system was one of the first binaries with a convincing detection of the apsidal precession.

<span class="mw-page-title-main">RS Sagittarii</span> Eclipsing binary star system in the constellation Sagittarius

RS Sagittarii is an eclipsing binary star system in the southern constellation of Sagittarius, abbreviated RS Sgr. It is a double-lined spectroscopic binary with an orbital period of 2.416 days, indicating that the components are too close to each other to be individually resolved. The system has a combined apparent visual magnitude of 6.01, which is bright enough to be faintly visible to the naked eye. During the primary eclipse the brightness drops to magnitude 6.97, while the secondary eclipse is of magnitude 6.28. The distance to this system is approximately 1,420 light years based on parallax measurements.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 10 December 2022.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 "GG Lup". The International Variable Star Index. AAVSO. Retrieved 10 December 2022.
  4. 1 2 3 4 5 6 7 8 9 10 11 12 13 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 .
  5. ↑ 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.
  6. 1 2 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.
  7. 1 2 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.
  8. ↑ "V* GG Lup -- Eclipsing Binary". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2022-12-10.
  9. ↑ 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.
  10. ↑ 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.
  11. ↑ 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.
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