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dc.creatorBeichman, Charles A.en_US
dc.creatorLisse, C. M.en_US
dc.creatorTanner, A. M.en_US
dc.creatorBryden, G.en_US
dc.creatorAkeson, R. L.en_US
dc.creatorCiardi, David R.en_US
dc.creatorBoden, Andrew F.en_US
dc.creatorDodson-Robinson, Sarah E.en_US
dc.creatorSalyk, Coletteen_US
dc.creatorWyatt, M. C.en_US
dc.date.accessioned2016-04-28T19:35:08Z
dc.date.available2016-04-28T19:35:08Z
dc.date.issued2011-12en
dc.identifierdoi:10.15781/T2TZ39
dc.identifier.citationBeichman, C. A., C. M. Lisse, A. M. Tanner, G. Bryden, R. L. Akeson, D. R. Ciardi, A. F. Boden, S. E. Dodson-Robinson, C. Salyk, and M. C. Wyatt. "Multi-epoch Observations of HD 69830: High-resolution Spectroscopy and Limits to Variability." The Astrophysical Journal, Vol. 743, No. 1 (Dec., 2011): 85.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34820
dc.description.abstractThe main-sequence solar-type star HD 69830 has an unusually large amount of dusty debris orbiting close to three planets found via the radial velocity technique. In order to explore the dynamical interaction between the dust and planets, we have performed multi-epoch photometry and spectroscopy of the system over several orbits of the outer dust. We find no evidence for changes in either the dust amount or its composition, with upper limits of 5%-7% (1 sigma per spectral element) on the variability of the dust spectrum over 1 year, 3.3% (1 sigma) on the broadband disk emission over 4 years, and 33% (1 sigma) on the broadband disk emission over 24 years. Detailed modeling of the spectrum of the emitting dust indicates that the dust is located outside of the orbits of the three planets and has a composition similar to main-belt, C-type asteroids in our solar system. Additionally, we find no evidence for a wide variety of gas species associated with the dust. Our new higher signal-to-noise spectra do not confirm our previously claimed detection of H(2)O ice leading to a firm conclusion that the debris can be associated with the break-up of one or more C-type asteroids formed in the dry, inner regions of the protoplanetary disk of the HD 69830 system. The modeling of the spectral energy distribution and high spatial resolution observations in the mid-infrared are consistent with a similar to 1 AU location for the emitting material.en_US
dc.description.sponsorshipNational Aeronautics and Space Administrationen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectinfrared: planetary systemsen_US
dc.subjectkuiper belt: generalen_US
dc.subjectplanets anden_US
dc.subjectsatellites: dynamical evolution and stabilityen_US
dc.subjectplanet-disk interactionsen_US
dc.subjectstars: individual (hd 69830)en_US
dc.subjectzodiacal dusten_US
dc.subjectspitzer-space-telescopeen_US
dc.subjectsolar-type starsen_US
dc.subjectsun-like starsen_US
dc.subjectinfrareden_US
dc.subjectinterferometric surveyen_US
dc.subjectdebris disksen_US
dc.subjecthot dusten_US
dc.subjectabsolute calibrationen_US
dc.subjectepsilon-eridanien_US
dc.subjectcollisional evolutionen_US
dc.subjectsize distributionsen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleMulti-Epoch Observations Of Hd 69830: High-Resolution Spectroscopy And Limits To Variabilityen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2011_12_hd69830.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/743/1/85en_US
dc.contributor.utaustinauthorDodson-Robinson, Sarah E.en_US
dc.contributor.utaustinauthorSalyk, Coletteen_US
dc.relation.ispartofserialAstrophysical Journalen_US


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