----- Submission 1 (Mon Aug 18 17:05:48 GMT 2003) -----
Successfully submitted: Mon Aug 18 17:06:05 GMT 2003
----- Submission 2 (Tue Aug 19 10:08:37 GMT 2003) -----
Successfully submitted: Tue Aug 19 10:08:46 GMT 2003
----- Submission 3 (Tue Aug 19 16:32:11 GMT 2003) -----
----- Submission 4 (Wed Aug 20 14:20:07 GMT 2003) -----
Buufer corrected to your recommandations.
Thanks for your help.Is the exoplanet HD209458b's exosphere in a "blowoff" state ?Using HST Lyman alpha observations, we have detected an extended tail shaped upper atmosphere around the extra-solar planet HD209458b. The Cycle 10 STIS G140M observations revealed an absorption of 15+/-4% of the stellar Lyman alpha emission line during the planetary transit in front of the star (Vidal-Madjar, et al. 2003). This showed that HI evaporation is taking place within a highly extended upper atmosphere.
Very recent studies on the evaporation mechanism are now indicating that instead of ``Jeans escape'' a more probable mechanism is complete atmospheric ``blowoff'' as suffered by the telluric planets in the early solar system. This mecanism could be directly tested with HST by searching for the escape of species slightly heavier than HI.
It is easy to show that neither oxygen nor carbon would be detected with HST if only ``Jeans escape'' takes place while both species, under ``blowoff'' conditions, should reach the Roche limit of the planet and escape as hydrogen. If this is the case an absorption during transit of about 15% should be observed for both. Twelve orbits with the STIS G140L spectrograph will allow us to detect the presence of these species during three transits with a better than 5% accuracy, needed to detect an object of the size of the planetary Roche lobe. Simultaneously these observations will confirm and give more precision about the extention of the HI cometary like tail expected to occult the star well after the end of the visible transit.
This proposed investigation is a unique opportunity to further study hot giant planets upper atmospheres, reveal the precise evaporation mechanism and give new constraints on the ``hot Jupiters'' lifetime. This could explain the lack of planets discovered so far at less than 0.04~AU from their star.
We ask for HST observations under Director Discretionnary time to have access to the
coming transits observable in the early fall of 2003.We propose to observe during the planetary transit in front of the star HD 209458 all the stellar lines including CII, OI and Lyman-Alpha lines using STIS/G140L mode.
The transit occurs every 3.5 days and lasts about 3 hours. Thus each visit allows to obtain scientific data for about 2 consecutive orbits during the transit. We will perform 4 visits of 3 orbits beginning before the occultation.
The observations of all stellar emission lines before or after the occultation will be used as reference spectra to check the level of stellar variations. We will thus obtain a total time of about 16000 seconds on the target during the occultation. A total of 12 orbits are used to perform the present program.
The observations are Time-critical; they must be obtained at a particular phase of the planet orbit: occultation. The list of possible schedules is calculted from the radial velocity and photometric surveys of this famous target (Mayor et al., updated value in june 2003). The occultation lasts about 3 hours. To obtain a good S/N ratio, we propose to observe several transits. We also propose to schedule the observation close to opposition to minimize the perturbation by the terrestrial Lyman-Alpha airglow. This is specified with the BETWEEN keyword.
However, we are aware that it may not be possible to follow this requirement and simultaneously follow the need of an observation at a particular phase of the occultation. This BETWEEN requirement must thus be considered as a preference, not critical for the science.STAR FORMATION0falsefalsefalsefalseSUPPORTEDSTARG V-IVStar of extra-solar planet. Proper motion and flux data from Hipparcos/Tycho Catalogue and SIMBAD.
B-V = 0.594, V-I = 0.66, TYPE=G0VHIP108859GSC1688-01821J200000 00 0.00+00 00 0.00J2000+/- 3.5 months from opposition. Dayglow not critical, but better if minimized.
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