Bibcode
Demangeon, O. D. S.; Faedi, F.; Hébrard, G.; Brown, D. J. A.; Barros, S. C. C.; Doyle, A. P.; Maxted, P. F. L.; Cameron, A. Collier; Hay, K. L.; Alikakos, J.; Anderson, D. R.; Armstrong, D. J.; Boumis, P.; Bonomo, A. S.; Bouchy, F.; Delrez, L.; Gillon, M.; Haswell, C. A.; Hellier, C.; Jehin, E.; Kiefer, F.; Lam, K. W. F.; Lendl, M.; Mancini, L.; McCormac, J.; Norton, A. J.; Osborn, H. P.; Palle, E.; Pepe, F.; Pollacco, D. L.; Prieto-Arranz, J.; Queloz, D.; Ségransan, D.; Smalley, B.; Triaud, A. H. M. J.; Udry, S.; West, R.; Wheatley, P. J.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 610, id.A63, 19 pp.
Fecha de publicación:
3
2018
Revista
Número de citas
46
Número de citas referidas
42
Descripción
To investigate the origin of the features discovered in the exoplanet
population, the knowledge of exoplanets' mass and radius with a good
precision (≲10%) is essential. To achieve this purpose the
discovery of transiting exoplanets around bright stars is of prime
interest. In this paper, we report the discovery of three transiting
exoplanets by the SuperWASP survey and the SOPHIE spectrograph with mass
and radius determined with a precision better than 15%. WASP-151b and
WASP-153b are two hot Saturns with masses, radii, densities and
equilibrium temperatures of 0.31-0.03+0.04
MJ, 1.13-0.03+0.03 RJ,
0.22-0.02+0.03 ρJ and
1290-10+20 K, and
0.39-0.02+0.02 MJ,
1.55-0.08+0.10 RJ,
0.11-0.02+0.02 ρJ and
1700-40+40 K, respectively. Their host stars are
early G type stars (with mag V 13) and their orbital periods are 4.53
and 3.33 days, respectively. WASP-156b is a super-Neptune orbiting a K
type star (mag V = 11.6). It has a mass of
0.128-0.009+0.010 MJ, a radius of
0.51-0.02+0.02 RJ, a density of
1.0-0.1+0.1 ρJ, an equilibrium
temperature of 970-20+30 K and an orbital period
of 3.83 days. The radius of WASP-151b appears to be only slightly
inflated, while WASP-153b presents a significant radius anomaly compared
to a recently published model. WASP-156b, being one of the few well
characterized super-Neptunes, will help to constrain the still debated
formation of Neptune size planets and the transition between gas and ice
giants. The estimates of the age of these three stars confirms an
already observed tendency for some stars to have gyrochronological ages
significantly lower than their isochronal ages. We propose that high
eccentricity migration could partially explain this behavior for stars
hosting a short period planet. Finally, these three planets also lie
close to (WASP-151b and WASP-153b) or below (WASP-156b) the upper
boundary of the Neptunian desert. Their characteristics support that the
ultra-violet irradiation plays an important role in this depletion of
planets observed in the exoplanet population.
The radial velocity (Tables A.1-A.3) and the high resolution photometric
data are only available at the CDSCDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/610/A63
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