91̽»¨

Skip to main content
Department Of Physics text logo
  • Research
    • Our research
    • Our research groups
    • Our research in action
    • Research funding 91̽»¨
    • Summer internships for undergraduates
  • Study
    • Undergraduates
    • Postgraduates
  • Engage
    • For alumni
    • For business
    • For schools
    • For the public
  • Support
91̽»¨
Stellar_flare_hits_HD_189733_b_(artist's_impression)

This artist's impression shows the hot Jupiter HD 189733b, as it passes in front of its parent star, as the latter is flaring, driving material away from the planet. The escaping atmosphere is seen silhouetted against the starlight. The surface of the star, which is around 80% the mass of the Sun, is based on observations of the Sun from NASA's Solar Dynamics Observatory.

Credit: NASA, ESA, L. Calçada, Solar Dynamics Observatory

Prof Suzanne Aigrain

Professor of Astrophysics

Research theme

  • Astronomy and astrophysics
  • Exoplanets and planetary physics

Sub department

  • Astrophysics

Research groups

  • Exoplanets and Stellar Physics
Suzanne.Aigrain@physics.ox.ac.uk
Telephone: 01865 (2)73339
Denys Wilkinson Building, room 762
  • About
  • Publications

Transiting exoplanets from the CoRoT space mission: I. CoRoT-Exo-1b: A low-density short-period planet around a G0V star

Astronomy and Astrophysics 482:3 (2008)

Authors:

P Barge, A Baglin, M Auvergne, H Rauer, A Léger, J Schneider, F Pont, S Aigrain, JM Almenara, R Alonso, M Barbieri, P Bordé, F Bouchy, HJ Deeg, De La Reza, M Deleuil, R Dvorak, A Erikson, M Fridlund, M Gillon, P Gondoin, T Guillot, A Hatzes, G Hebrard, L Jorda, P Kabath, H Lammer, A Llebaria, B Loeillet, P Magain, T Mazeh, C Moutou, M Ollivier, M Pätzold, D Queloz, D Rouan, A Shporer, G Wuchterl

Abstract:

Context. The pioneer space mission for photometric planet searches, CoRoT, steadily monitors about 12 000 stars in each of its fields of view. Transit candidates can be detected early in the processing of the data and before the end of a run of observation.Aims. We report the detection of the first planet discovered by CoRoT and characterizing it with the help of follow-up observations.Methods. Raw data were filtered from outliers and residuals at the orbital period of the satellite. The orbital parameters and the radius of the planet were estimated by best fitting the phase folded light curve with 34 successive transits. Doppler measurements with the SOPHIE spectrograph permitted us to secure the detection against binaries and to estimate the mass of the planet.Results. The accuracy of the data is very high with a dispersion in the 2.17 min binned phase-folded light curve that does not exceed ~3.10 in flux unit. The planet orbits a mildly metal-poor G0V star of magnitude in 1.5 days. The estimated mass and radius of the star are 0.950.15 and 1.110.05 . We find the planet has a radius of 1.490.08 , a mass of 1.030.12 , and a particularly low mean density of 0.380.05 gcm. . © 2008 ESO.

Transiting exoplanets from the CoRoT space mission: III. The spectroscopic transit of CoRoT-Exo-2b with SOPHIE and HARPS

Astronomy and Astrophysics 482:3 (2008)

Authors:

F Bouchy, D Queloz, M Deleuil, B Loeillet, AP Hatzes, S Aigrain, R Alonso, M Auvergne, A Baglin, P Barge, W Benz, P Bordé, HJ Deeg, R De La Reza, R Dvorak, A Erikson, M Fridlund, P Gondoin, T Guillot, G Hébrard, L Jorda, H Lammer, A Léger, A Llebaria, P Magain, M Mayor, C Moutou, M Ollivier, M Pätzold, F Pepe, F Pont, H Rauer, D Rouan, J Schneider, AHMJ Triaud, S Udry, G Wuchterl

Abstract:

We report on the spectroscopic transit of the massive hot-Jupiter CoRoT-Exo-2b observed with the high-precision spectrographs SOPHIE and HARPS. By modeling the radial velocity anomaly occurring during the transit due to the Rossiter-McLaughlin (RM) effect, we determine the sky-projected angle between the stellar spin and the planetary orbital axis to be close to zero = 7.2 4.5 deg, and we secure the planetary nature of CoRoT-Exo-2b. We discuss the influence of the stellar activity on the RM modeling. Spectral analysis of the parent star from HARPS spectra are presented. © 2008 ESO.

WASP-3b: a strongly irradiated transiting gas-giant planet

\mnras 385 (2008) 1576-1584-1576-1584

Authors:

D Pollacco, I Skillen, A Collier Cameron, B Loeillet, HC Stempels, F Bouchy, NP Gibson, L Hebb, G Hébrard, YC Joshi, I McDonald, B Smalley, AMS Smith, RA Street, S Udry, RG West, DM Wilson, PJ Wheatley, S Aigrain, K Alsubai, CR Benn, VA Bruce, DJ Christian, WI Clarkson, B Enoch, A Evans, A Fitzsimmons, CA Haswell, C Hellier, S Hickey, ST Hodgkin, K Horne, M Hrudková, J Irwin, SR Kane, FP Keenan, TA Lister, P Maxted, M Mayor, C Moutou, AJ Norton, JP Osborne, N Parley, F Pont, D Queloz, R Ryans, E Simpson

The Monitor project: the search for transits in the open cluster NGC 2362

(2008)

Authors:

Adam A Miller, Jonathan Irwin, Suzanne Aigrain, Simon Hodgkin, Leslie Hebb

Transiting exoplanets from the CoRoT space mission I - CoRoT-Exo-1b: a low-density short-period planet around a G0V star

(2008)

Authors:

P Barge, A Baglin, M Auvergne, H Rauer, A Leger, J Schneider, F Pont, S Aigrain, J-M Almenara, R Alonso, M Barbieri, P Borde, F Bouchy, H-J Deeg, R De la Reza, M Deleuil, R Dvorak, A Erikson, M Fridlund, M Gillon, P Gondoin, T Guillot, A Hatzes, G Hebrard, L Jorda, P Kabath, H Lammer, A Llebaria, B Loeillet, P Magain, T Mazeh, C Moutou, M Ollivier, M Patzold, D Queloz, D Rouan, A Shporer, G Wuchterl

Pagination

  • First page First
  • Previous page Prev
  • …
  • Page 84
  • Page 85
  • Page 86
  • Page 87
  • Current page 88
  • Page 89
  • Page 90
  • Page 91
  • Page 92
  • …
  • Next page Next
  • Last page Last

Footer 91̽»¨

  • Contact us
  • Giving to the Dept of Physics
  • Work with us
  • Media

User account menu

  • Log in

Follow us

FIND US

Clarendon Laboratory,

Parks Road,

91̽»¨,

OX1 3PU

CONTACT US

Tel: +44(0)1865272200

Department Of Physics text logo

© 91̽»¨ - Department of Physics

Cookies | Privacy policy | Accessibility statement

  • Home
  • Research
  • Study
  • Engage
  • Our people
  • News & Comment
  • Events
  • Our facilities & services
  • About us
  • Giving to Physics