[FKSI, le ‘Fourier–Kelvin Stellar Interferometer’—Un interféromètre spatial sur le chemin de la découverte et de la caractérisation des planètes de type Terre]
Durant les dernières années, un effort considérable a été produit dans l'objectif de missions importantes telles que Darwin et TPF-I (Terrestrial Planet Finder Interferometer) pour la détection de planètes de type Terre autour des étoiles proches. Cependant, certains aspects technologiques critiques tels que le vol en formation, le refroidissement cryogénique, le taux de réjection sur une large bande passante en longueur d'ondes ainsi que le contrôle des sources d'erreurs systématiques rendent improbables les études de Phase A avant la fin de cette décennie. Un interféromètre simplifié comme le ‘Fourier–Kelvin Stellar Interferometer’, opérant dans l'infrarouge proche et moyen (de 3 à 8 microns), permet de caractériser un échantillon important des planètes extrasolaires déjà détectées par méthodes indirectes. Plusieurs autres sujets astrophysiques phares peuvent aussi être abordés par FKSI comme l'étude des disques de débris. Nous discutons dans cet article du fondement d'une mission de type ‘mission moyenne’ dont le coût s'échelonne entre $450–600 million (USD), mission pour laquelle FKSI se positionne.
During the last few years, considerable effort has been directed towards large-scale (>$1 billion USD) missions to detect and characterize Earth-like planets around nearby stars, such as the Terrestrial Planet Finder Interferometer (TPF-I) and Darwin missions. However, technological issues such as formation flying, cryocooling, null depth for broadband signals, control of systematic noise sources, budgetary pressures, and shifting science priorities at NASA and ESA, will prevent these missions from entering Phase A until the middle of the next decade. A simplified nulling interferometer operating in the near- to mid-infrared (e.g. ∼3–8 microns), like the Fourier–Kelvin Stellar Interferometer (FKSI), can characterize the atmospheres of a large sample of the known planets. Many other scientific problems can be addressed with a system like FKSI, including the imaging of debris disks, active galactic nuclei, and low mass companions around nearby stars. We discuss the rationale, both scientific and technological, for a competed mission in the $450–600 million (USD) range, of which FKSI is an example.
Mot clés : Interféromètre, Planètes extrasolaires, Formation des planètes, Disques de débris, Noyaux galactiques actifs
@article{CRPHYS_2007__8_3-4_396_0,
author = {William C. Danchi and Bruno Lopez},
title = {The {Fourier{\textendash}Kelvin} {Stellar} {Interferometer} {(FKSI){\textemdash}A} practical infrared space interferometer on the path to the discovery and characterization of {Earth-like} planets around nearby stars},
journal = {Comptes Rendus. Physique},
pages = {396--407},
publisher = {Elsevier},
volume = {8},
number = {3-4},
year = {2007},
doi = {10.1016/j.crhy.2007.04.002},
language = {en},
}
TY - JOUR AU - William C. Danchi AU - Bruno Lopez TI - The Fourier–Kelvin Stellar Interferometer (FKSI)—A practical infrared space interferometer on the path to the discovery and characterization of Earth-like planets around nearby stars JO - Comptes Rendus. Physique PY - 2007 SP - 396 EP - 407 VL - 8 IS - 3-4 PB - Elsevier DO - 10.1016/j.crhy.2007.04.002 LA - en ID - CRPHYS_2007__8_3-4_396_0 ER -
%0 Journal Article %A William C. Danchi %A Bruno Lopez %T The Fourier–Kelvin Stellar Interferometer (FKSI)—A practical infrared space interferometer on the path to the discovery and characterization of Earth-like planets around nearby stars %J Comptes Rendus. Physique %D 2007 %P 396-407 %V 8 %N 3-4 %I Elsevier %R 10.1016/j.crhy.2007.04.002 %G en %F CRPHYS_2007__8_3-4_396_0
William C. Danchi; Bruno Lopez. The Fourier–Kelvin Stellar Interferometer (FKSI)—A practical infrared space interferometer on the path to the discovery and characterization of Earth-like planets around nearby stars. Comptes Rendus. Physique, Volume 8 (2007) no. 3-4, pp. 396-407. doi : 10.1016/j.crhy.2007.04.002. https://comptes-rendus.academie-sciences.fr/physique/articles/10.1016/j.crhy.2007.04.002/
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