A dynamically-packed planetary system around GJ 667C with three super-Earths in its habitable zone

By G. Anglada-Escud'e, Mikko Tuomi, E. Gerlach, R. Barnes, R. Heller, J. Jenkins, S. Wende, S. Vogt, R. P. Butler, A. Reiners and 1 more. 2013

315 citations recorded by the source corpus.

Guillen Anglada-Escude, et al, 'A dynamically-packed planetary system around GJ 667J with three super-Earths in its habitable zone', A&A, Vol. 556, A126, first published online 7 August 2013. The version of record is available at doi: http://doi.org/10.1051/0004-6361/201321331. © ESO 2013. Reproduced with permission from Astronomy & Astrophysics. Published by EDP Sciences

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/450ee60bd416cb1ebc7395f64130658d187ee703

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Citations in the corpus

HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS (2014, background): “; Anglada-Escude et al. 2013), and it is expected that this number will greatly increase as time passes (Dressing & Charbonneau 2013; Kopparapu 2013; Gaidos 2013).”
The Habitability of Planets Orbiting M-dwarf Stars (2016, methodology): “About 200 exoplanets have been found around M-dwarf stars, many in their stars’ habitable zones (Anglada-Escudé et al., 2013; Quintana et al., 2014; Rowe et al., 2014; Torres et al., 2015; Crossfield et al., 2015; Barclay et al., 2015; Schlieder et al., 2016; Anglada-Escudé et al., 2016).”
THE INNER EDGE OF THE HABITABLE ZONE FOR SYNCHRONOUSLY ROTATING PLANETS AROUND LOW-MASS STARS USING GENERAL CIRCULATION MODELS (2016, background): “For example, Gl 667Cc (Anglada-Escude et al. 2013), a superEarth around an M-dwarf star with effective temperature Teff = 3350K, has an orbital period of 28.1 days (Robertson et al. 2014)1.”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, background): “These possibly rocky planets (m sin i < 10M⊕) include GJ 163c (Bonfils et al. 2013), GJ 667 Cc (Anglada-Escudé et al. 2013; Delfosse et al. 2013), HD 40307g (Tuomi et al. 2013), Kapteyn b (Anglada-Escudé et al. 2014), and GJ 832c (Wittenmyer et al. 2014).”
High-cadence spectroscopy of M-dwarfs. I. Analysis of systematic effects in HARPS-N line profile measurements on the bright binary GJ 725A+B (2016, methodology): “To assess the significance of the variability and its possible fit to a Keplerian orbit, we use likelihood periodograms as described in Baluev (2009) and in Anglada-Escudé et al. (2013).”