Reference : WASP-44b, WASP-45b and WASP-46b: three short-period, transiting extrasolar planets
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
WASP-44b, WASP-45b and WASP-46b: three short-period, transiting extrasolar planets
Anderson, D. R. [> > > >]
Collier Cameron, A. [> > > >]
Gillon, Michaël mailto [> > > >]
Hellier, C. [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astrophysique et traitement de l'image]
Jehin, Emmanuel [> > > >]
Lendl, M. [> > > >]
Maxted, P. F. L. [> > > >]
Queloz, D. [> > > >]
Smalley, B. [> > > >]
Smith, A. M. S. [> > > >]
Triaud, A H M J [> > > >]
West, R. G. [> > > >]
Pepe, F. [> > > >]
Pollacco, D. [> > > >]
Ségransan, D. [> > > >]
Todd, I. [> > > >]
Udry, S. [ > > ]
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
Yes (verified by ORBi)
United Kingdom
[en] Astrophysics - Earth and Planetary Astrophysics
[en] We report the discovery of three extrasolar planets that transit their moderately bright (Vmag = 12-13) host stars. WASP-44b is a 0.89-MJup planet in a 2.42-day orbit around a G8V star. WASP-45b is a 1.03-MJup planet which passes in front of the limb of its K2V host star every 3.13 days. Weak Ca H+K emission seen in the spectra of WASP-45 suggests the star is chromospherically active. WASP-46b is a 2.10-MJup planet in a 1.43-day orbit around a G6V star. Rotational modulation of the light curves of WASP-46 and weak Ca H+K emission in its spectra show the star to be photospherically and chromospherically active. We imposed circular orbits in our analyses as the radial velocity data are consistent with (near-)circular orbits, as could be expected from both empirical and tidal-theory perspectives for such short-period, Jupiter-mass planets. We discuss the impact of fitting for eccentric orbits for these type of planets when not supported by the data. The derived planetary and stellar radii depend on the fitted eccentricity and further studies use these quantities in attempts to understand planet structure, the interdependence of parameters and the relevant physics for extrasolar planets. As such, we recommend exercising caution in fitting the orbits of short period, Jupiter-mass planets with an eccentric orbital model when there is no evidence of non-circularity.

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