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Three sub-Jupiter-mass planets: WASP-69b & WASP-84b transit active K dwarfs and WASP-70Ab transits the evolved primary of a G4+K3 binary | | D. R. Anderson
; A. Collier Cameron
; L. Delrez
; A. P. Doyle
; F. Faedi
; A. Fumel
; M. Gillon
; Y. Gómez Maqueo Chew
; C. Hellier
; E. Jehin
; M. Lendl
; P. F. L. Maxted
; F. Pepe
; D. Pollacco
; D. Queloz
; D. Ségransan
; I. Skillen
; B. Smalley
; A. M. S. Smith
; J. Southworth
; A. H. M. J. Triaud
; O. D. Turner
; S. Udry
; R. G. West
; | | Date: |
21 Oct 2013 | | Abstract: | We report the discovery of the transiting exoplanets WASP-69b, WASP-70Ab and
WASP-84b, each of which orbits a bright star (V~10). WASP-69b is a bloated
Saturn-mass planet (0.26 M$_{
m Jup}$, 1.06 R$_{
m Jup}$) in a 3.868-d period
around an active mid-K dwarf. We estimate a stellar age of 1 Gyr from both
gyrochronological and age-activity relations, though an alternative
gyrochronological relation suggests an age of 3 Gyr. ROSAT detected X-rays at a
distance of 60$pm$27 arcsec from WASP-69. If the star is the source then the
planet could be undergoing mass-loss at a rate of ~10$^{12}$ g s$^{-1}$. This
is 1-2 orders of magnitude higher than the evaporation rate estimated for HD
209458b and HD 189733b, both of which have exhibited anomalously-large
Lyman-{alpha} absorption during transit. WASP-70Ab is a sub-Jupiter-mass
planet (0.59 M$_{
m Jup}$, 1.16R$_{
m Jup}$) in a 3.713-d orbit around the
primary of a spatially-resolved G4+K3 binary, with a separation of 3.3 arcsec
($geq$800 AU). We exploit the binary nature of the system to construct a H-R
diagram, from which we estimate its age to be 9-10 Gyr. WASP-84b is a
sub-Jupiter-mass planet (0.69 M$_{
m Jup}$, 0.94 R$_{
m Jup}$) in an 8.523-d
orbit around an active early-K dwarf. Of the transiting planets discovered from
the ground to date, WASP-84b has the third-longest period. From a combination
of gyrochronological and age-activity relations we estimate the age of WASP-84
to be ~1 Gyr.
For both the active stars WASP-69 and WASP-84 we find a modulation of the
radial velocities with a period similar to the photometrically-determined
stellar rotation period. We fit the residuals with a low-order harmonic series
and subtract the best fit from the RVs prior to deriving the system parameters.
In each case the solution is essentially unchanged, with much less than a
1-{sigma} change to the planetary mass. We found... | | Source: | arXiv, 1310.5654 | | Services: | Forum | Review | PDF | Favorites | |
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