ﻻ يوجد ملخص باللغة العربية
We report the sky-projected orbital obliquity (spin-orbit angle) of WASP-84b, a 0.70-$M_{rm Jup}$ planet in a 8.52-day orbit around a G9V/K0V star, to be $lambda = 0.3 pm 1.7^circ$. We obtain a true obliquity of $psi = 14.8 pm 8.0^circ$ from a measurement of the inclination of the stellar spin axis with respect to the sky plane. Due to the young age and the weak tidal forcing of the system, we suggest that the orbit of WASP-84b is unlikely to have both realigned and circularised from the misaligned and/or eccentric orbit likely to have arisen from high-eccentricity migration. Therefore we conclude that the planet probably migrated via interaction with the protoplanetary disc. This would make it the first short-orbit, giant planet to have been shown to have migrated via this pathway. Further, we argue that the distribution of obliquities for planets orbiting cool stars ($T_{rm eff}$ < 6250 K) suggests that high-eccentricity migration is an important pathway for the formation of short-orbit, giant planets.
DS Tuc Ab is a Neptune-sized planet that orbits around a member of the 45 Myr old Tucana-Horologium moving group. Here, we report the measurement of the sky-projected angle between the stellar spin axis and the planets orbital axis, based on the obse
We report the discovery of the transiting exoplanets WASP-69b, WASP-70Ab and WASP-84b, each of which orbits a bright star ($Vsim10)$. WASP-69b is a bloated Saturn-mass planet (0.26 $M_{rm Jup}$, 1.06 $R_{rm Jup}$) in a 3.868-d period around an active
WASP-12b is a transiting hot Jupiter on a 1.09-day orbit around a late-F star. Since the planets discovery in 2008, the time interval between transits has been decreasing by $29pm 2$ msec year$^{-1}$. This is a possible sign of orbital decay, althoug
To investigate the origin of the features discovered in the exoplanet population, the knowledge of exoplanets mass and radius with a good precision is essential. In this paper, we report the discovery of three transiting exoplanets by the SuperWASP s
Transition discs are expected to be a natural outcome of the interplay between photoevaporation (PE) and giant planet formation. Massive planets reduce the inflow of material from the outer to the inner disc, therefore triggering an earlier onset of