Observational constraints on dust disk sizes in tidally truncated protoplanetary disks in multiple systems in the Taurus region. (arXiv:1907.03846v1 [astro-ph.EP])

Observational constraints on dust disk sizes in tidally truncated protoplanetary disks in multiple systems in the Taurus region. (arXiv:1907.03846v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Manara_C/0/1/0/all/0/1">C.F. Manara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tazzari_M/0/1/0/all/0/1">M. Tazzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Long_F/0/1/0/all/0/1">F. Long</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herczeg_G/0/1/0/all/0/1">G.J. Herczeg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lodato_G/0/1/0/all/0/1">G. Lodato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rota_A/0/1/0/all/0/1">A.A. Rota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cazzoletti_P/0/1/0/all/0/1">P. Cazzoletti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plas_G/0/1/0/all/0/1">G. van der Plas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinilla_P/0/1/0/all/0/1">P. Pinilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dipierro_G/0/1/0/all/0/1">G. Dipierro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edwards_S/0/1/0/all/0/1">S. Edwards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harsono_D/0/1/0/all/0/1">D. Harsono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_D/0/1/0/all/0/1">D. Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Y. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menard_F/0/1/0/all/0/1">F. Menard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nisini_B/0/1/0/all/0/1">B. Nisini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ragusa_E/0/1/0/all/0/1">E. Ragusa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehler_Y/0/1/0/all/0/1">Y. Boehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrit_S/0/1/0/all/0/1">S. Cabrit</a>

The impact of stellar multiplicity on the evolution of planet-forming disks
is still the subject of debate. Here we present and analyze disk structures
around 10 multiple stellar systems that were included in an unbiased, high
spatial resolution survey of 32 protoplanetary disks in the Taurus star-forming
region with ALMA. At the unprecedented spatial resolution of ~0.12″ we detect
and spatially resolve the disks around all primary stars, as well as those
around eight secondary and one tertiary stars. The dust radii of disks around
multiple stellar systems are smaller than those around single stars in the same
stellar mass range and in the same region. The disks in multiple stellar
systems have also a steeper decay of the mm-continuum emission at the outer
radius than disks around single stars, suggestive of the impact of tidal
truncation on the shape of the disks in multiple systems. However, the observed
ratio between the dust disk radii and the observed separation of the stars in
the multiple systems is consistent with analytic predictions of the effect of
tidal truncation only if the eccentricities of the binaries are rather high
(typically >0.5), or if the observed dust radii are a factor of two smaller
than the gas radii, as is typical for isolated systems. Similar high resolution
studies targeting the gaseous emission from disks in multiple stellar systems
are required to resolve this question.

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