A5038736041- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Astro and Planetary Science
- Astrophysics and Star Formation Studies
- Astronomical Observations and Instrumentation
- Gamma-ray bursts and supernovae
- Adaptive optics and wavefront sensing
- Calibration and Measurement Techniques
- Solar and Space Plasma Dynamics
- History and Developments in Astronomy
- Astrophysical Phenomena and Observations
- Planetary Science and Exploration
- Atmospheric Ozone and Climate
- High-pressure geophysics and materials
- Spacecraft Design and Technology
- Spectroscopy and Laser Applications
- Scientific Research and Discoveries
- Space Exploration and Technology
- Scientific Measurement and Uncertainty Evaluation
- Pulsars and Gravitational Waves Research
- Astronomical and nuclear sciences
- Spectroscopy and Chemometric Analyses
- Space Satellite Systems and Control
- Galaxies: Formation, Evolution, Phenomena
- Geophysics and Gravity Measurements
University of Birmingham
2017-2025
University of Geneva
2010-2020
University of Cambridge
2016-2019
University of Toronto
2015-2017
The Scarborough Hospital
2015-2017
Institute of Astronomy
2017
Cavendish Hospital
2016
Massachusetts Institute of Technology
2013-2015
Swiss National Science Foundation
2014-2015
Kavli Institute for Particle Astrophysics and Cosmology
2014-2015
Context. Several competing scenarios for planetary-system formation and evolution seek to explain how hot Jupiters came be so close their parent stars. Most planetary parameters evolve with time, making it hard distinguish between models. The obliquity of an orbit respect the stellar rotation axis is thought more stable than other such as eccentricity. planets, date, appear aligned axis; few misaligned planets far detected are massive (> 2MJ).
Thousands of exoplanets have now been discovered with a huge range masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface their host star. However, essential nature these remains largely mysterious: there is no known, discernible pattern linking presence, size, or orbital parameters planet its parent We little idea whether chemistry linked formation environment, type star drives physics planet's birth, evolution. ARIEL was conceived observe number...
We have detected low-amplitude radial-velocity variations in two stars, USNO-B1.0 1219-0005465 (GSC 02265-00107 = WASP-1) and 0964-0543604 00522-01199 WASP-2). Both stars were identified as being likely host of transiting exoplanets the 2004 SuperWASP wide-field transit survey. Using newly-commissioned spectrograph SOPHIE at Observatoire de Haute-Provence, we found that both objects exhibit reflex orbital with amplitudes characteristic planetary-mass companions in-phase photometric orbits....
Abstract We have collected transit times for the TRAPPIST-1 system with Spitzer Space Telescope over four years. add to these ground-based, HST, and K2 transit-time measurements, revisit an N -body dynamical analysis of seven-planet using our complete set from which we refine mass ratios planets star. next carry out a photodynamical light curves derive density host star planet densities. find that all seven planets’ densities may be described single rocky mass–radius relation is depleted in...
Context. The TRAPPIST-1 system hosts seven Earth-sized, temperate exoplanets orbiting an ultra-cool dwarf star. As such, it represents a remarkable setting to study the formation and evolution of terrestrial planets that formed in same protoplanetary disk. While sizes are all known better than 5% precision, their densities have significant uncertainties (between 28% 95%) because poor constraints on planet's masses. Aims.The goal this paper is improve our knowledge planetary masses using...
We present the discovery by WASP-South survey, in close collaboration with Euler and TRAPPIST telescopes, of WASP-121 b, a new remarkable short-period transiting hot Jupiter, whose planetary nature has been statistically validated PASTIS software. The planet mass $1.183_{-0.062}^{+0.064}$ $M_{\mathrm{Jup}}$, radius 1.865 $\pm$ 0.044 $R_{\mathrm{Jup}}$, transits every $1.2749255_{-0.0000025}^{+0.0000020}$ days an active F6-type main-sequence star ($V$=10.4, $1.353_{-0.079}^{+0.080}$...
One notable example of exoplanet diversity is the population circumbinary planets, which orbit around both stars a binary star system. There are, so far, only 16 known exoplanets, all lie in same orbital plane as host binary. Suggestions indicate that planets could also exist on orbits highly inclined to binary, close 90°, polar orbits. No such have been found yet, but gas and debris discs observed, if these were form then those would be left orbit. We report strong evidence for exoplanet,...
We report the discovery of transiting giant planet WASP-17b, least-dense currently known. It is 1.6 Saturn masses but 1.5-2 Jupiter radii, giving a density 6-14 per cent that Jupiter. WASP-17b in 3.7-day orbit around sub-solar metallicity, V = 11.6, F6 star. Preliminary detection Rossiter-McLaughlin effect suggests retrograde (lambda ~ -150 deg), indicative violent history involving planet-planet or star-planet scattering. WASP-17b's bloated radius could be due to tidal heating resulting...
We report on the discovery of a new extremely short period transiting extrasolar planet, WASP-19b. The planet has mass Mpl = 1.15 ± 0.08 MJ, radius Rpl 1.31 0.06 RJ, and orbital P 0.7888399 0.0000008 days. Through spectroscopic analysis, we determine host star to be slightly super-solar metallicity ([M/H] 0.1 dex) G-dwarf with Teff 5500 100 K. In addition, detect periodic, sinusoidal flux variations in light curve which are used derive rotation for Prot 10.5 0.2 relatively stellar suggests...
We present twenty-three transit light curves and seven occultation for the ultra-short period planet WASP-43 b, in addition to eight new measurements of radial velocity star. Thanks this extensive data set, we improve significantly parameters system. Notably, largely improved precision on stellar density (2.41+-0.08 rho_sun) combined with constraining age be younger than a Hubble time allows us break degeneracy solution mentioned discovery paper. The resulting mass size are 0.717+-0.025...
The gaseous giant planets WASP-4b and WASP-5b are transiting 12-magnitude solar-type stars in the Southern hemisphere. aim of present work is to refine parameters these systems using high cadence VLT/FORS2 <i>z<i/>-band transit photometry high-resolution VLT/UVES spectroscopy. For WASP-4, new estimates for planet radius mass from a combined analysis our VLT data with previously published radial velocities <i>R<i/><sub><i>J<i/><sub/> <i>M<i/><sub><i>J<i/><sub/>, resulting density . host star...
We present radial-velocity sequences acquired during three transits of the exoplanet HD 189733b and one transit CoRoT-3b. applied a combined Markov-Chain Monte Carlo analysis spectroscopic photometric data on these stars, to determine full set system parameters including project spin-orbit misalignement angle an unprecedented precision via Rossiter-McLaughlin effect: beta = 0.85 degrees (+0.32 -0.28) . This small but non-zero inclination planetary orbit is important understand origin system....
We present seven new transiting hot Jupiters from the WASP-South survey. The planets are all typical orbiting stars F4 to K0 with magnitudes of V = 10.3 12.5. orbital periods in range 3.9--4.6 d, planetary masses 0.4--2.3 Mjup and radii 1.1--1.4 Mjup. In line known Jupiters, densities Jupiter-like inflated (rho 0.13--1.07 rho_jup). use increasing numbers investigate distribution their 3--4-d "pile-up".
We report the discovery of <i>WASP-8b<i/>, a transiting planet <i>2.25<i/> <i>±<i/> 0.08 <i>M<i/><sub>Jup<sub/> on strongly inclined eccentric 8.15-day orbit, moving in retrograde direction to rotation its late-G host star. Evidence is found that star multiple stellar system with two other companions. The dynamical complexity indicates it may have experienced secular interactions such as Kozai mechanism or formation differs from "classical" disc-migration theory.
We report the discovery of transiting exoplanets WASP-69b, WASP-70Ab and WASP-84b, each which orbits a bright star ($V\sim10)$. WASP-69b is bloated Saturn-mass planet (0.26 $M_{\rm Jup}$, 1.06 $R_{\rm Jup}$) in 3.868-d period around an active, $\sim$1-Gyr, mid-K dwarf. ROSAT detected X-rays $60 \pm 27"$ from WASP-69. If source then could be undergoing mass-loss at rate $\sim$10$^{12}$ g s$^{-1}$. This 1 to 2 orders magnitude higher than evaporation estimated for HD 209458b 189733b, both have...