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Mid-infrared Studies of HD 113766 and HD 172555: Assessing Variability in the Terrestrial Zone of Young Exoplanetary Systems | Kate Y. L. Su
; George H. Rieke
; Carl Melis
; Alan P. Jackson
; Paul S. Smith
; Huan Y. A. Meng
; Andras Gaspar
; | Date: |
11 Jun 2020 | Abstract: | We present multi-epoch infrared photometry and spectroscopy obtained with
warm Spitzer, Subaru and SOFIA to assess variability for the young ($sim$20
Myr) and dusty debris systems around HD 172555 and HD 113766A. No variations
(within 0.5%) were found for the former at either 3.6 or 4.5 $mu$m, while
significant non-periodic variations (peak-to-peak of $sim$10-15% relative to
the primary star) were detected for the latter. Relative to the Spitzer IRS
spectra taken in 2004, multi-epoch mid-infrared spectra reveal no change in
either the shape of the prominent 10 $mu$m solid-state features or the overall
flux levels (no more than 20%) for both systems, corroborating that the
population of sub-$mu$m-sized grains that produce the pronounced solid-state
features is stable over a decadal timescale. We suggest that these
sub-$mu$m-sized grains were initially generated in an optically thick clump of
debris of mm-sized vapor condensates resulting from a recent violent impact
between large asteroidal or planetary bodies. Because of the shielding from the
stellar photons provided by this clump, intense collisions led to an
over-production of fine grains that would otherwise be ejected from the system
by radiation pressure. As the clump is sheared by its orbital motion and
becomes optically thin, a population of very fine grains could remain in stable
orbits until Poynting-Robertson drag slowly spirals them into the star. We
further suggest that the 3-5 $mu$m disk variation around HD 113766A is
consistent with a clump/arc of such fine grains on a modestly eccentric orbit
in its terrestrial zone. | Source: | arXiv, 2006.6590 | Services: | Forum | Review | PDF | Favorites |
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