Observability of Forming Planets and their Circumplanetary Disks III. — Polarized Scattered Light. (arXiv:1906.01416v3 [astro-ph.EP] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Szulagyi_J/0/1/0/all/0/1">J. Szulágyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garufi_A/0/1/0/all/0/1">A. Garufi</a>
There are growing amount of very high-resolution polarized scattered light
images of circumstellar disks. Nascent giant planets planets are surrounded by
their own circumplanetary disks which may scatter and polarize both the
planetary and stellar light. Here we investigate whether we could detect
circumplanetary disks with the same technique and what can we learn from such
detections. Here we created scattered light mock observations at 1.245 microns
(J band) for instruments like SPHERE and GPI, for various planetary masses
(0.3, 1.0, 5.0, 10.0 $rm{M_{Jup}}$), disk inclinations (90, 60, 30, 0 degrees)
and planet position angles (0, 45, 90 degrees). We found that the detection of
a circumplanetary disk at 50AU from the star is significantly favored if the
planet is massive ($geq 5 rm{M_{Jup}}$) and the system is nearly face-on
($leq 30^circ$). In these cases the accretion shock front on the surface of
the circumplanetary disks are strong and bright enough to help the visibility
of this subdisk. Its detection is hindered by the neighboring circumstellar
disk that also provides a strong polarized flux. However, the comparison
between the $PI$ and the $Q_phi$ maps is a viable tool to pinpoint the
presence of the circumplanetary disk within the circumstellar disk, as the two
disks are behaving differently on those images.
There are growing amount of very high-resolution polarized scattered light
images of circumstellar disks. Nascent giant planets planets are surrounded by
their own circumplanetary disks which may scatter and polarize both the
planetary and stellar light. Here we investigate whether we could detect
circumplanetary disks with the same technique and what can we learn from such
detections. Here we created scattered light mock observations at 1.245 microns
(J band) for instruments like SPHERE and GPI, for various planetary masses
(0.3, 1.0, 5.0, 10.0 $rm{M_{Jup}}$), disk inclinations (90, 60, 30, 0 degrees)
and planet position angles (0, 45, 90 degrees). We found that the detection of
a circumplanetary disk at 50AU from the star is significantly favored if the
planet is massive ($geq 5 rm{M_{Jup}}$) and the system is nearly face-on
($leq 30^circ$). In these cases the accretion shock front on the surface of
the circumplanetary disks are strong and bright enough to help the visibility
of this subdisk. Its detection is hindered by the neighboring circumstellar
disk that also provides a strong polarized flux. However, the comparison
between the $PI$ and the $Q_phi$ maps is a viable tool to pinpoint the
presence of the circumplanetary disk within the circumstellar disk, as the two
disks are behaving differently on those images.
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