CoRoT Results

Oops ...sorry

Here goes another link:

http://www.eso.org/public/news/eso1011/

The wait is over. I wonder when Corot-8 and others have to be released.

It should have a hill sphere radius of about 3 million km. I read somewhere that stable orbits are out to about 1/3 of the distance of the hill sphere. So... ~1 Mkm. This is roughly comparable to the semi-major axis of Callisto.

Sudarsky's class II with wather clouds (Like Polyphemus lol) or class II with clarified atmosphere?

Rings not?
http://www.eso.org/public/archives/releases/sciencepapers/eso1011/eso1011.pdf

Difficult to really say anything based on the light curve. The rings detectability would be a strong function of their inclination. The planet could have rings and they be well aligned with the planet's orbit, thus having a small transit depth signature. And of course there's always the possibility the planet really doesn't have appreciable rings in the first place.

Other photometry? Corot'a?
http://www.obspm.fr/actual/nouvelle/mar10/corot.en.shtml

Quote :

Figure 1 | Light curve and model fit of the CoRoT-9b transit. a, Phase-folded light curve from CoRoT around the first observed transit of Corot-9b, with the phase set to zero at mid-transit. The data from the three color-bands of CoRoT have been summed to a ‘white’ band and the points have been binned from an original cadence of 32 seconds to a duration of 96 seconds; the error bars indicate the dispersion of the points within the bins. The second transit observed by CoRoT is not shown, as it was only partially detected; its first 2 hours had been lost in an instrument interruption.

Ie limits on the satellites have not yet installed. Fully observed Corot only one transit.

But on the other hand the star is too faint. (V = 13.8 ) This apparently makes it impossible to find large satellites (the size of Earth or Mars), even at HST.

Here for example
http://arxiv.org/abs/0712.1374
Precision photometry from the Hubble HD189733b was 50 kilometers radius, or 1 part per million.
The difference between the HD189733 and Corot-9 7 stellar magnitudes, or 500 times. So 1 * 500 = 500 part per million. This is a planet with a radius of 2 radius of the Earth.

From this twitter post, moons of this planet would be hot due to less efficient heat management.

And CoRoT-9 b is most definitely not in the habitable zone (ref), despite an alluring title on the ESA's CoRoT web page.

Timeline for CoRoT-9b discovery:

• CoRoT begins observing on 15 April 2008.
  
• Transit of the planet observed on 16 May 2008.
  
• First SOPHIE RV measurement 5 August 2008.
  
• The second transit would have occurred on 20 August 2008 but was incompletely observed due to instrument interruption.
  
• Second SOPHIE RV measurement 25 August 2008. RV variation over this period found to be compatible with giant planet.
  
• CoRoT ends observing on 7 September 2008 (145 days of observation)
  
• HARPS begins observing 21 September 2008
  
• Ground-based telescopes observe transit on 1 June 2009. Confirms transit is associated with the star, not a background event.
  
• HARPS ends observing 20 September 2009
  

Takes a while to confirm these planets!

Not sure whether the observed transits are sufficient to determine much in the way of TTV.

Borislav wrote:

Here for example
http://arxiv.org/abs/0712.1374
Precision photometry from the Hubble HD189733b was 50 kilometers radius, or 1 part per million.
The difference between the HD189733 and Corot-9 7 stellar magnitudes, or 500 times. So 1 * 500 = 500 part per million. This is a planet with a radius of 2 radius of the Earth.

I was wrong.
http://arxiv.org/abs/0907.3909


Ie even Kepler could detect the size of the moon in half the Earth's radius from Corot-9. And with HST observation probably have the opportunity to discover more small satellites.

Stalker wrote:

Sudarsky's class II with wather clouds (Like Polyphemus lol) or class II with clarified atmosphere?

Paper points out that since class III has lower albedo than class II, there is a region where the planet could "lock" into either III or II, and CoRoT-9b falls into that region. On the other hand since gas giants apparently cool down from a hot initial state, I'd guess it'd lock into class III, but this is an exoplanet where unexpected weirdness is standard.

http://online.kitp.ucsb.edu/online/exoplanets_c10/deleuil/pdf/Deleuil_ExoPlanetsConf_KITP.pdf


The graph 15 stars. Apparently it is all the planets COROT to Corot-15b. It turns out the first two long-periodic fields, yet there is nothing less than the super-Earth COROT-7b

Corot 8b & 10b through 14b Just shown up on EPE!

http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=47175

15b a Brown Dwarf according to ESA

At last some candidates. Cheers

Very nice
CoRoT increases their lead!
How will Kepler respond tomorrow?

Why not downloaded articles?
http://smsc.cnes.fr/COROT/Fr/publis_2010_06_14.htm

Borislav wrote:

Why not downloaded articles?
http://smsc.cnes.fr/COROT/Fr/publis_2010_06_14.htm

My guess is that they were not properly put in a place from where they could be downloaded.
You can get some of the papers from the Extrasolar Planet Encyclopaedia's Bibliography section.

Edit:
CoRoT-10 b paper: http://arxiv.org/abs/1006.2949

Welcome to (to-be-confirmed) Corot-7 d

http://exoplanet.eu/planet.php?p1=CoRoT-7&p2=d

Looking like a very compact version of HD 40307. Pity the host star is so active.

An Investigation into the Radial Velocity Variations of CoRoT-7
http://arxiv.org/abs/1006.5476

Abstract wrote:

CoRoT-7b, the first transiting ``superearth'' exoplanet, has a radius of 1.7 R_Earth and a mass of 4.8 M_Earth. Ground-based radial velocity measurements also detected an additional companion with a period of 3.7 days (CoRoT-7c) and a mass of 8.4 M_Earth. The mass of CoRoT-7b is a crucial parameter for planet structure models, but is difficult to determine because CoRoT-7 is a modestly active star and there is at least one additional companion. A Fourier analysis was performed on spectral data for CoRoT-7 taken with the HARPS spectrograph. These data include RV measurements, spectral line bisectors, the full width at half maximum of the cross-correlation function, and Ca II emission. The latter 3 quantities vary due to stellar activity and were used to assess the nature of the observed RV variations. An analysis of a sub-set of the RV measurements where multiple observations were made per night was also used to estimate the RV amplitude from CoRoT-7b that was less sensitive to activity variations. Our analysis indicates that the 0.85-d and 3.7-d RV signals of CoRoT-7b and CoRoT-7c are present in the spectral data with a high degree of statistical significance. We also find evidence for another significant RV signal at 9 days. An analysis of the activity indicator data reveals that this 9-d signal most likely does not arise from activity, but possibly from an additional companion. If due to a planetary companion the mass is m = 19.5 M_Earth, assuming co-planarity with CoRoT-7b. A dynamical study of the three planet system shows that it is stable over several hundred millions of years. Our analysis yields a RV amplitude of 5.04 +/- 1.09 m/s for CoRoT-7b which corresponds to a planet mass of m = 6.9 +/- 1.4 M_Earth. This increased mass would make the planet CoRoT-7b more Earth-like in its internal structure.