Planets and stellar activity: hide and seek in the CoRoT-7 system
Raphaëlle D. Haywood,A. Collier Cameron,Didier Queloz,S. C. C. Barros,Magali Deleuil,Rim Fares,Michaël Gillon,Antonino F. Lanza,C. Lovis,C. Moutou,Francesco Pepe,Don Pollacco,Alexandre Santerne,Alexandre Santerne,Damien Ségransan,Yvonne C. Unruh +15 more
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In this paper, the authors used the off-transit variations in the star's light curve to estimate the radial-velocity variations induced by the suppression of convective blueshift and the flux blocked by starspots.Abstract:
Since the discovery of the transiting super-Earth CoRoT-7b, several investigations have yielded different results for the number and masses of planets present in the system, mainly owing to the star's high level of activity. We re-observed CoRoT-7 in 2012 January with both HARPS and CoRoT, so that we now have the benefit of simultaneous radial-velocity and photometric data. This allows us to use the off-transit variations in the star's light curve to estimate the radial-velocity variations induced by the suppression of convective blueshift and the flux blocked by starspots. To account for activity-related effects in the radial velocities which do not have a photometric signature, we also include an additional activity term in the radial-velocity model, which we treat as a Gaussian process with the same covariance properties (and hence the same frequency structure) as the light curve. Our model was incorporated into a Monte Carlo Markov Chain in order to make a precise determination of the orbits of CoRoT-7b and CoRoT-7c. We measure the masses of planets b and c to be 4.73 +/- 0.95 and 13.56 +/- 1.08 M-circle plus, respectively. The density of CoRoT-7b is (6.61 +/- 1.72)(R-p/1.58 R-circle plus)(-3) g cm(-3), which is compatible with a rocky composition. We search for evidence of an additional planet d, identified by previous authors with a period close to 9 d. We are not able to confirm the existence of a planet with this orbital period, which is close to the second harmonic of the stellar rotation at similar to 7.9 d. Using Bayesian model selection, we find that a model with two planets plus activity-induced variations is most favoured.read more
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What about the messenger
TL;DR: In this article, NAFU SA and other role players expressed some criticism about government programmes. The criticism was not so much about the objectives and content of these programmes, but rather about their accessibility, or lack thereof, to emerging farmers.
Journal ArticleDOI
A temperate rocky super-Earth transiting a nearby cool star
Jason A. Dittmann,Jonathan Irwin,David Charbonneau,Xavier Bonfils,Xavier Bonfils,Nicola Astudillo-Defru,Raphaëlle D. Haywood,Zachory K. Berta-Thompson,Elisabeth R. Newton,Joseph E. Rodriguez,Jennifer G. Winters,Thiam-Guan Tan,J. M. Almenara,J. M. Almenara,J. M. Almenara,François Bouchy,X. Delfosse,X. Delfosse,T. Forveille,T. Forveille,Christophe Lovis,Felipe Murgas,Felipe Murgas,Felipe Murgas,Francesco Pepe,Nuno C. Santos,Stéphane Udry,A. Wunsche,A. Wunsche,Gilbert A. Esquerdo,David W. Latham,Courtney D. Dressing +31 more
TL;DR: Observations of LHS 1140b, a planet with a radius of 1.4 Earth radii transiting a small, cool star (L HS 1140) 12 parsecs away, measure the mass of the planet to be 6.6 times that of Earth, consistent with a rocky bulk composition, and place an upper limit on the orbital eccentricity.
Journal ArticleDOI
Growth model interpretation of planet size distribution
Li Zeng,Stein B. Jacobsen,Dimitar Sasselov,Michail I. Petaev,Andrew Vanderburg,Mercedes Lopez-Morales,Juan Pérez-Mercader,Thomas R. Mattsson,Gongjie Li,Matthew Z. Heising,Aldo S. Bonomo,Mario Damasso,Travis A. Berger,Hao Cao,Amit Levi,Robin Wordsworth +15 more
TL;DR: In this paper, a growth model and Monte Carlo simulations are used to demonstrate that many intermediate-size exoplanets are water worlds, which matches the second peak of the exoplanet radius bimodal distribution.
Journal ArticleDOI
Mass–radius relation for rocky planets based on prem
TL;DR: In this paper, a semi-empirical mass-radius relation for two-layer rocky planets based on PREM was derived, which is applicable to 1$\sim$8 M$_{\oplus}$ and CMF of 0.26\pm0.4.
Journal ArticleDOI
A rocky planet transiting a nearby low-mass star
Zachory K. Berta-Thompson,Jonathan Irwin,David Charbonneau,Elisabeth R. Newton,Jason A. Dittmann,Nicola Astudillo-Defru,Xavier Bonfils,Michaël Gillon,Emmanuel Jehin,Antony A. Stark,B. Stalder,Francois Bouchy,Xavier Delfosse,Thierry Forveille,Christophe Lovis,Michel Mayor,V. Neves,Francesco Pepe,Nuno C. Santos,Stéphane Udry,A. Wunsche +20 more
TL;DR: In this paper, the authors reported observations of GJ 1132b, a planet with a size of 1.2 Earth radii that is transiting a small star 12 parsecs away.
References
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