[ OHP Home page | OAMP Home page ]
Press release from LAM - OHP / OAMP / INSU-CNRS /
Université de Provence / Université de Genève. This press release (in french) and the submitted scientific paper (in english) are also on-line at
www.oamp.fr. See also
astro-ph.
New extra-solar planet transits near-by star 5 October 2005
French version
An international team of astronomers led by
François Bouchy has announced the discovery of a new transiting extra-solar
planet. The planet HD189733b, in the constellation Vulpecula, was detected and
studied by the combination of two different methods, radial velocities and
photometric transits, using the telescopes at Haute-Provence Observatory (OHP).
It is one of the few extra-solar planets for which scientists have been able to
accurately determine both its radius (1.26 Jupiter radii) and mass (1.15 Jupiter
masses). Thus, and also due to its nearness, about 60 light-years from Earth,
the extra-solar planet HD 189733b offers exciting new possibilities for
follow-up studies.
| | The star HD189733 is
shown by the green arrow. It is located less that 0.15° (about half the
diameter of the Moon) from the M27 "Dumbell" planetary nebulae (photo by Daniel
Jaroschik) | | |
A new extra-solar planet has been found at Haute-Provence Observatory on
September 15, 2005 by an international team of astronomers from the Laboratoire
d'Astrophysique de Marseille (LAM), the Observatoire de Haute-Provence (OHP) and
Observatoire de Genève.
This discovery was made, using the Doppler method, with
the
ELODIE spectrograph at the 1.93-m telescope, the same one used ten years
earlier to find the very first extra-solar planet 51 Peg b. Simultaneously, the
CCD camera at the 1m20 telescope was used to detect the transit of the
extra-solar planet across the disk of the star. This phenomenon can be explained
by the favorable orientation of the system as seen from the Earth: the orbital
plane is seen edge-on and the extra-solar planet crosses the disk of the star,
occulting it partially. The scientific team has thus been able to derive both
the exact mass and radius of the planet, concluding that it is a large "hot
Jupiter". The planetary system in HD189733 is particularly interesting for
several reasons:
- This new extra-solar planet joins the very exclusive group of
planets outside our solar system that scientists have been able to measure
precisely. Even if 160 extra-solar planets are presently known, accurate
values for masses and radii are known only for 9 systems. HD189733b has a mass
365 times that of the Earth and a radius 14 times larger. Its density is
comparable to that of Saturn. This extra-solar planet is located nearby, only 63
light-years away. The star HD189733 can be seen using binoculars (visual
magnitude 7.7) in the constellation Vulpecula (The Fox). It just happens to be
located by in the
vicinity of the famous M27 "Dumbell" planetary nebula, well known to amateur
astronomers.
- Its orbital period is one of the shortest known (only 2.2 days),
nearly 2000 times faster than Jupiter, which takes 12 years to make a trip
around the Sun. Due to the favorable orientation of its orbital plane, the
planet HD189733b occults the central star every 2.2 days, producing a
photometric transit (analogous to the Venus transit of the Sun seen in June
2004), a small decrease of flux lasting 2 hours.
- The transit of HD 189733b produces a decrease in luminosity of 3% which
makes this system the one with the deepest partial occultation
of the nine known transiting systems.
This is due to the small size of the star (3/4 the size of the Sun)
and the large size of the planet (1.26 times the size of Jupiter).
- The central star of this new planetary system is bright (V=7.7); most
ground-based and space-borne telescopes will soon try to measure other
interesting parameters, in particular its atmosphere. The small distance
separating the planet from its star (only 3/100 of the Earth-Sun distance)
implies that its atmosphere must be very hot, several hundred degrees. Attemps
will be made to measure the reflectivity of its atmosphere, its chemical
composition and the rate of evaporation. The light emitted by the planet itself
may even be within reach of interferometry.
The extra-solar planet HD189733b will transit its host star on Wednesday,
October 5, 2005 at 20h40 UT and every 53 hours thereafter. The members of the
team will not miss this date and will try to obtain more data on this planet.
Observations of this type made from a ground-based observatory (for example
from OHP) allow the discovery of giant planets around other stars, but the
transit method from space will make possible the discovery of even smaller
planets: this is the aim of the COROT space mission to be launched in 2006.
Reference: ELODIE
metallicity-biased search for transiting Hot Jupiters : II. A very hot Jupiter
transiting the bright K star HD189733, Bouchy et al.,
submitted to Astronomy and Astrophysics.
| | Radial velocities of the star HD189733
obtained with the ELODIE echelle spectrograph on the 1.93-m OHP telescope
showing the presence of a planet 1.15 times heavier than Jupiter located at 0.03
AU from the star. Radial-velocities measure the gravitational pull on the star
by the planet. | | |
| | Differential photometric measurements of
the star HD189733 obtained with the CCD camera on the 1.2-m telescope showing
the transit of a planet 1.25 times the size of
Jupiter. | | |
|
| The 1.2-m
OHP telescope which was used to observe the photometric transit of HD189733. The
1.93-m dome, where the radial velocities were measured, is seen in the
background. |
1Members of the team :
F. Bouchy, Laboratoire d’Astrophysique de Marseille, Observatoire de Haute
Provence
C. Moutou, Laboratoire d’Astrophysique de Marseille
N. Iribarne, S. Ilovaisky, Observatoire de Haute Provence
S. Udry, M. Mayor, F. Pont, R. Da Silva, D. Queloz, D. Segransan, Observatoire
de Genève
N.C. Santos, Lisbon Observatory
S. Zucker, Weizmann Institute of Science, Israel
Contact points : - François Bouchy
Observatoire Astronomique Marseille Provence, (33) 1 44 32 80 79
- Claire Moutou
Laboratoire d'Astrophysique de Marseille, (33) 4 91
05 59 66
- Stéphane Udry
Observatoire de Genève, (41) 22 37 92
467
- Michel Mayor
Observatoire de Genève, (41) 22 37 92 460
2, place Le Verrier 13248 Marseille cedex 4 France
Tél. : (+33) 4 95 04 41 00 Fax : (+33) 4 91 62 11 90
www.oamp.fr |