5 research outputs found
Wavelength-Dependent Extinction and Grain Sizes in Dippers
We have examined inter-night variability of K2-discovered Dippers that are
not close to being viewed edge-on, as determined from previously-reported ALMA
images, using the SpeX spectrograph and the NASA Infrared Telescope facility
(IRTF). The three objects observed were EPIC 203850058, EPIC 205151387, and
EPIC 204638512 (2MASS J16042165-2130284). Using the ratio of the fluxes between
two successive nights, we find that for EPIC 204638512 and EPIC 205151387, we
find that the properties of the dust differ from that seen in the diffuse
interstellar medium and denser molecular clouds. However, the grain properties
needed to explain the extinction does resemble those used to model the disks of
many young stellar objects. The wavelength-dependent extinction models of both
EPIC 204638512 and EPIC 205151387 includes grains at least 500 microns in size,
but lacks grains smaller than 0.25 microns. The change in extinction during the
dips, and the timescale for these variations to occur, imply obscuration by the
surface layers of the inner disks. The recent discovery of a highly
mis-inclined inner disk in EPIC 204638512 is suggests that the variations in
this disk system may point to due to rapid changes in obscuration by the
surface layers of its inner disk, and that other face-on Dippers might have
similar geometries. The He I line at 1.083 microns in EPIC 205151387 and EPIC
20463851 were seen to change from night to night, suggesting that we are seeing
He I gas mixed in with the surface dust.Comment: 13 pages, 6 figures, 2 table
Differences in the gas and dust distribution in the transitional disk of a sun-like young star, PDS 70
We present ALMA 0.87 mm continuum, HCO+ J=4--3 emission line, and CO J=3--2
emission line data of the disk of material around the young, Sun-like star PDS
70. These data reveal the existence of a possible two component transitional
disk system with a radial dust gap of 0."2 +/- 0."05, an azimuthal gap in the
HCO+ J=4--3 moment zero map, as well as two bridge-like features in the gas
data. Interestingly these features in the gas disk have no analogue in the dust
disk making them of particular interest. We modeled the dust disk using the
Monte Carlo radiative transfer code HOCHUNK3D (Whitney et al. 2013) using a two
disk components. We find that there is a radial gap that extends from 15-60 au
in all grain sizes which differs from previous work
Direct images and spectroscopy of a giant protoplanet driving spiral arms in MWC 758
Understanding the driving forces behind spiral arms in protoplanetary disks
remains a challenge due to the faintness of young giant planets. MWC 758 hosts
such a protoplanetary disk with a two-armed spiral pattern that is suggested to
be driven by an external giant planet. We present new thermal infrared
observations that are uniquely sensitive to redder (i.e., colder or more
attenuated) planets than past observations at shorter wavelengths. We detect a
giant protoplanet, MWC 758c, at a projected separation of ~100 au from the
star. The spectrum of MWC 758c is distinct from the rest of the disk and
consistent with emission from a planetary atmosphere with Teff = 500 +/- 100 K
for a low level of extinction (AV<30), or a hotter object with a higher level
of extinction. Both scenarios are commensurate with the predicted properties of
the companion responsible for driving the spiral arms. MWC 758c provides
evidence that spiral arms in protoplanetary disks can be caused by cold giant
planets or by those whose optical emission is highly attenuated. MWC 758c
stands out both as one of the youngest giant planets known, and also as one of
the coldest and/or most attenuated. Furthermore, MWC 758c is among the first
planets to be observed within a system hosting a protoplanetary disk.Comment: Published in Nature Astronom
Wavelength-dependent Extinction and Grain Sizes in âDippersâ
We have examined internight variability of K2-discovered âdippersâ that are not close to being viewed edge-on, as determined from previously reported ALMA images, using the SpeX spectrograph on NASAâs Infrared Telescope Facility. The three objects observed were EPIC 203850058, EPIC 205151387, and EPIC 204638512 (=2MASS J16042165-2130284). Using the ratio of the fluxes between two successive nights, we find that for EPIC 204638512 and EPIC 205151387, we find that the properties of the dust differ from that seen in the diffuse interstellar medium and denser molecular clouds. However, the grain properties needed to explain the extinction does resemble those used to model the disks of many young stellar objects. The wavelength-dependent extinction models of both EPIC 204638512 and EPIC 205151387 includes grains at least 500 ÎŒ m in size, but lacks grains smaller than 0.25 ÎŒ m. The change in extinction during the dips, and the timescale for these variations to occur, imply obscuration by the surface layers of the inner disks. The recent discovery of a highly misinclined inner disk in EPIC 204638512 is suggests that the variations in this disk system may point to due to rapid changes in obscuration by the surface layers of its inner disk, and that other âface-onâ dippers might have similar geometries. The He i line at 1.083 ÎŒ m in EPIC 205151387 and EPIC 20463851 were seen to change from night to night, suggesting that we are seeing He i gas mixed in with the surface dust
Direct images and spectroscopy of a giant protoplanet driving spiral arms in MWC 758
Understanding the driving forces behind spiral arms in protoplanetary disks remains a challenge due to the faintness of young giant planets. MWC 758 hosts such a protoplanetary disk with a two-armed spiral pattern that is suggested to be driven by an external giant planet. We present observations in the thermal infrared that are uniquely sensitive to redder (that is, colder, or more attenuated) planets than past observations at shorter wavelengths. We detect a giant protoplanet, MWC 758c, at a projected separation of roughly 100 au from the star. The spectrum of MWC 758c is distinct from the rest of the disk and consistent with emission from a planetary atmosphere with T eff = 500 ± 100 K for a low level of extinction (A V †30), or a hotter object with a higher level of extinction. Both scenarios are commensurate with the predicted properties of the companion responsible for driving the spiral arms. MWC 758c provides evidence that spiral arms in protoplanetary disks can be caused by cold giant planets or by those whose optical emission is highly attenuated. MWC 758c stands out both as one of the youngest giant planets known, and as one of the coldest and/or most attenuated. Furthermore, MWC 758c is among the first planets to be observed within a system hosting a protoplanetary disk.6 month embargo; first published 06 July 2023This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]