Probing the Inner Disk Emission of the Herbig Ae Stars HD 163296 and HD 190073. (arXiv:1811.03778v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Setterholm_B/0/1/0/all/0/1">Benjamin R. Setterholm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monnier_J/0/1/0/all/0/1">John D. Monnier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_C/0/1/0/all/0/1">Claire L. Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreplin_A/0/1/0/all/0/1">Alexander Kreplin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_S/0/1/0/all/0/1">Stefan Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baron_F/0/1/0/all/0/1">Fabien Baron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aarnio_A/0/1/0/all/0/1">Alicia Aarnio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_J/0/1/0/all/0/1">Jean-Philippe Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvet_N/0/1/0/all/0/1">Nuria Calvet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cure_M/0/1/0/all/0/1">Michel Curé</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanaan_S/0/1/0/all/0/1">Samer Kanaan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kloppenborg_B/0/1/0/all/0/1">Brian Kloppenborg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouquin_J/0/1/0/all/0/1">Jean-Baptiste Le Bouquin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millan_Gabet_R/0/1/0/all/0/1">Rafael Millan-Gabet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rubinstein_A/0/1/0/all/0/1">Adam E. Rubinstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sitko_M/0/1/0/all/0/1">Michael L. Sitko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sturmann_J/0/1/0/all/0/1">Judit Sturmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brummelaar_T/0/1/0/all/0/1">Theo A. ten Brummelaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Touhami_Y/0/1/0/all/0/1">Yamina Touhami</a>
The physical processes occurring within the inner few astronomical units of
proto-planetary disks surrounding Herbig Ae stars are crucial to setting the
environment in which the outer planet-forming disk evolves and put critical
constraints on the processes of accretion and planet migration. We present the
most complete published sample of high angular resolution H- and K-band
observations of the stars HD 163296 and HD 190073, including 30 previously
unpublished nights of observations of the former and 45 nights of the latter
with the CHARA long-baseline interferometer, in addition to archival VLTI data.
We confirm previous observations suggesting significant near-infrared emission
originates within the putative dust evaporation front of HD 163296 and show
this is the case for HD 190073 as well. The H- and K-band sizes are the same
within $(3 pm 3)%$ for HD 163296 and within $(6 pm 10)%$ for HD 190073. The
radial surface brightness profiles for both disks are remarkably Gaussian-like
with little or no sign of the sharp edge expected for a dust evaporation front.
Coupled with spectral energy distribution analysis, our direct measurements of
the stellar flux component at H and K bands suggest that HD 190073 is much
younger (<400 kyr) and more massive (~5.6 M$_odot$) than previously thought,
mainly as a consequence of the new Gaia distance (891 pc).
The physical processes occurring within the inner few astronomical units of
proto-planetary disks surrounding Herbig Ae stars are crucial to setting the
environment in which the outer planet-forming disk evolves and put critical
constraints on the processes of accretion and planet migration. We present the
most complete published sample of high angular resolution H- and K-band
observations of the stars HD 163296 and HD 190073, including 30 previously
unpublished nights of observations of the former and 45 nights of the latter
with the CHARA long-baseline interferometer, in addition to archival VLTI data.
We confirm previous observations suggesting significant near-infrared emission
originates within the putative dust evaporation front of HD 163296 and show
this is the case for HD 190073 as well. The H- and K-band sizes are the same
within $(3 pm 3)%$ for HD 163296 and within $(6 pm 10)%$ for HD 190073. The
radial surface brightness profiles for both disks are remarkably Gaussian-like
with little or no sign of the sharp edge expected for a dust evaporation front.
Coupled with spectral energy distribution analysis, our direct measurements of
the stellar flux component at H and K bands suggest that HD 190073 is much
younger (<400 kyr) and more massive (~5.6 M$_odot$) than previously thought,
mainly as a consequence of the new Gaia distance (891 pc).
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