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SCIENTIFIC ORGANIZATION SCIENTIFIC RESULTS DATA DELIVERY MEETINGS COROTSKY MEDIA GALLERY
 
COnvection, ROtation
& planetary Transits
THE SKY OBSERVED BY COROT 
The candidates stars catalogue for the seismology mission sismologie holds:
11 primary stars and
813 secondary stars.
For the exoplanets mission it holds at least 200 000 candidates for the observation

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CoRoT has two main scientific objectives:

The stellar seismology

The purpose of stellar seismology is to analyse the vibration modes of the stars which, submitted to forces of gravity, pressure and Coriolis, behave as oscillators with many specific modes. The eigen frequency (between 1 minute and 3 hours), the amplitude (a few ppm in Fourier space) and the lifetime (a few days) of these modes make it possible to determine some important parameters of stellar physics, such as the size and the composition of the core, the limits between radiative and convective zones, or the internal profile of rotation. These oscillating modes, which generate variations of luminosity at the surface of the star, are the only information, with neutrinos, coming from the depth of the stars. Acquired and collected on stars with different mass, age and chemical composition, the CoRoT light curves bring a significant amount of data of a new kind about stellar evolution.
During the whole mission 150 stars will be observed, with magnitude between 6 and 9.
 
 
 
The search for exoplanets (telluric)

The method used is the method of the "planetary transits" which consists in detecting a planet by the small periodic drop of brightness on the disc of the star it orbits around. This photometric method, complementary to the radial velocities, has the interest to unveil both orbit period and size (radius) of the planets detected. According to existence hypotheses, the Corot mission should discover, in addition to a large number of giants (hot Jupiters), a few tens of rocky planets (exoEarths). Potential rings or satellites could also be detected around giant extrasolar planets. The chromatric analysis of the CoRoT light curves, thanks to a dispersion device (prism) mounted in front of the exoplanet channel CCDs, allows to help identifying the different families of detected events (transits, stellar activity, eclipsing binaries...).
Till the end of the mission, almost 200 000 stars will be surveyed.
 
 
The others scientific objectives of CoRoT:

The Additional programmes

During the mission, up to 200 000 objects in the magnitude R range {5.5, 16} will be observed with sampling times from 1second to 15 minutes, a relative accuracy of 100 ppm per measurement.

Numerous programmes concerning various fields of astrophysics benefit from these data, as i.e. stellar activity and magnetism, intrinsic variability, detection of comets, of small size Kuiper belt objects...

An additionnal programme is defined as follows:

    Adressing different scientific questions than the Core Program (CP) but using the same data
    Asking for different targets and/or observing procedures than CP
    In the same fields of view
    In different fields of view

The selection of the additionnal programmes is made by the Scientific Council
AOs are issued regularly for the successive runs?
Authors of selected AP become Guest Investigators (GI)
They have the same rights as the CO-Is on the data they have required.


Latest Update 20/02/2012

 
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