Modeling the Protoplanetary Disks of Two Brown Dwarfs in the Taurus Molecular Cloud. (arXiv:1905.05829v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rilinger_A/0/1/0/all/0/1">Anneliese M. Rilinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espaillat_C/0/1/0/all/0/1">Catherine C. Espaillat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macias_E/0/1/0/all/0/1">Enrique Macías</a>
Measuring the properties of protoplanetary disks around brown dwarfs is
central to understanding the formation of brown dwarfs and their planetary
companions. We present modeling of CFHT Tau 4 and 2M0444, two brown dwarfs with
protoplanetary disks in the Taurus Molecular Cloud. By combining modeling of
the spectral energy distributions and ALMA images, we obtain disk radii and
masses for these objects; these parameters can be used to constrain brown dwarf
formation and planet formation, respectively. We find that the disk around CFHT
Tau 4 has a mass of 0.42 M$_{Jup}$ and a radius of 80 au; we find 2M0444’s disk
to have a mass of 2.05 M$_{Jup}$ and a radius of 100 au. These radii are more
consistent with those predicted by theoretical simulations of brown dwarf
formation via undisturbed condensation from a mass reservoir than those
predicted by ejection from the formation region. Furthermore, the disk mass of
2M0444 suggests that planet formation may be possible in this disk, although
the disk of 2M0444 is likely not massive enough to form planets. The disk
properties measured here provide constraints to theoretical models of brown
dwarf formation and the formation of their planetary companions.
Measuring the properties of protoplanetary disks around brown dwarfs is
central to understanding the formation of brown dwarfs and their planetary
companions. We present modeling of CFHT Tau 4 and 2M0444, two brown dwarfs with
protoplanetary disks in the Taurus Molecular Cloud. By combining modeling of
the spectral energy distributions and ALMA images, we obtain disk radii and
masses for these objects; these parameters can be used to constrain brown dwarf
formation and planet formation, respectively. We find that the disk around CFHT
Tau 4 has a mass of 0.42 M$_{Jup}$ and a radius of 80 au; we find 2M0444’s disk
to have a mass of 2.05 M$_{Jup}$ and a radius of 100 au. These radii are more
consistent with those predicted by theoretical simulations of brown dwarf
formation via undisturbed condensation from a mass reservoir than those
predicted by ejection from the formation region. Furthermore, the disk mass of
2M0444 suggests that planet formation may be possible in this disk, although
the disk of 2M0444 is likely not massive enough to form planets. The disk
properties measured here provide constraints to theoretical models of brown
dwarf formation and the formation of their planetary companions.
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