Poster (Scientific congresses and symposiums)
Modeling the η Corvi debris disk from the sub-AU scale to its outermost regions
Lebreton, J.; Beichman, C. A.; Bryden, G. et al.
2014Search for Life Beyond the Solar System. Exoplanets, Biosignatures & Instruments.
 

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Keywords :
Exozodiacal dust; Exoplanets; Eta Corvi
Abstract :
[en] Dusty debris disks surrounding main sequence stars are thought to be analogues to thepopulations of small bodies of the Solar System (asteroids, comets/icy bodies and dust grains), however with often much higher masses and associated dust production rates. Mecanisms such as massive collisions or LHB-like events must therefore be invoked to justify their existence. This is especially striking for the nearby F2V star η Corvi that shows a very strong mid- and far-infrared excess despite an estimated age of ~1.4 Gyr (Lisse et al. 2012, Wyatt et al. 2005). We present new observations of the η Crv debris disk obtained in the far-infrared with Herschel/PACS and SPIRE and in the mid-infrared with the Keck Interferometer Nuller (Millan-Gabet et al. 2011). The Herschel/PACS images at 70, 100 and 160 μm reveal a well resolved belt of cold material at ~130 AU, as well as an unresolved component in the innermost parts of the system. This warmer counterpart is resolved in the mid-infrared as a strong null excess originating from within the ~2x4 AU field-of-view of the interferometer, which is reminiscent of the architecture of the Fomalhaut debris disk (Mennesson et al. 2012, Lebreton et al. 2013). The signature of warm silicate dust is also very clear in Spitzer/IRS high-resolution spectra (Chen et al. 2006) at intermediate wavelengths (10-35 μm). We undertake to establish a consistent model of the debris disk from the sub-AU scale to its outermost regions using the GRaTer radiative transfer code (Augereau et al. 1999a, Lebreton et al. 2013) by adjusting simultaneously the interferometric nulls, the resolved Herschel images and the spectro-photometric data against a large parameter space. Our analysis providesaccurate estimates of the fundamental parameters of the disk: its surface density profile, grain size distribution and mass, making it possible to unveil the origin of the dust and the relation between the cold (~50 K) Kuiper-like belt and the warm (~500 K) exo-zodiacal disk. We further discuss the possible existence of an additional dust population at intermediate temperatures and its nature. η Corvi will be of prime interest for future observations with the JWST. We finally make predictions of the ability of NIRCam and MIRI to image details in the disk at high contrast with both spatial and spectral resolution in order to obtain a better view of this complex planetary system.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Lebreton, J.;  IPAC, Caltech,
Beichman, C. A.;  IPAC/NExScI/JPL, Caltech
Bryden, G.;  JPL, Caltech
Defrere, Denis ;  Université de Liège > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS)
Mennesson, Bertr;  JPL, Caltech
Millan-Gabet, R.;  JPL, Caltech)
Gabor, Pavel
Language :
English
Title :
Modeling the η Corvi debris disk from the sub-AU scale to its outermost regions
Publication date :
01 March 2014
Event name :
Search for Life Beyond the Solar System. Exoplanets, Biosignatures & Instruments.
Event date :
March 2014
Audience :
International
Available on ORBi :
since 12 January 2017

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