Rings and asymmetries in protoplanetary disks are considered as signposts of ongoing planet formation.In this work,we con-duct three-dimensional radiative transfer simulations to model the intriguing disk around HD143...Rings and asymmetries in protoplanetary disks are considered as signposts of ongoing planet formation.In this work,we con-duct three-dimensional radiative transfer simulations to model the intriguing disk around HD143006 that has three dust rings and a bright arc.A complex geometric configuration,with a misaligned inner disk,is assumed to account for the asymmetric structures.The two-dimensional surface density is constructed by iteratively fitting the ALMA data.We find that the dust tem-perature displays a notable discontinuity at the boundary of the misalignment.The ring masses range from 0.6 to 16 M⊕that are systematically lower than those inferred in the younger HL Tau disk.The arc occupies nearly 20%of the total dust mass.Such a high mass fraction of dust grains concentrated in a local region is consistent with the mechanism of dust trapping into vortices.Assuming a gas-to-dust mass ratio of 30 that is constant throughout the disk,the dense and cold arc is close to the threshold of being gravitationally unstable,with the Toomre parameter Q∼1.3.Nevertheless,our estimate of Q relies on the assumption for the unknown gas-to-dust mass ratio.Adopting a lower gas-to-dust mass ratio would increase the inferred Q value.Follow-up high resolution observations of dust and gas lines are needed to clarify the origin of the substructures.展开更多
Turbulent motions are believed to regulate angular momentum transport and influence dust evolution in protoplanetary disks.Measuring the strength of turbulence is challenging through gas line observations because of t...Turbulent motions are believed to regulate angular momentum transport and influence dust evolution in protoplanetary disks.Measuring the strength of turbulence is challenging through gas line observations because of the requirement for high spatial and spectral resolution data,and an exquisite determination of the temperature.In this work,taking the well-known HD 163296 disk as an example,we investigated the contrast of gaps identified in high angular resolution continuum images as a probe for the level of turbulence.With self-consistent radiative transfer models,we simultaneously analyzed the radial brightness profiles along the disk major and minor axes,and the azimuthal brightness profiles of the B67 and B100 rings.By fitting all the gap contrasts measured from these profiles,we constrained the gas-to-dust scale height ratioΛto be 3.0^(+0.3)_(−0.8),1.2^(+0.1)_(−0.1),and≥6.5 for the D48,B67,and B100 regions,respectively.The varying gas-to-dust scale height ratios indicate that the degree of dust settling changes with radius.The inferred values forΛtranslate into a turbulence level of α_(turb)<3×10^(−3) in the D48 and B100 regions,which is consistent with previous upper limits set by gas line observations.However,turbulent motions in the B67 ring are strong with α_(turb)∼1.2×10^(−2).Due to the degeneracy betweenΛand the depth of dust surface density drops,the turbulence strength in the D86 gap region is not constrained.展开更多
基金support by the National Natural Science Foundation of China(Grant No.11973090)the support by the European Research Council(ERC)under the European Union’s Horizon 2020 Research and Innovation Program(Grant No.757957)the Science Research Grants from the China Manned Space Project(Grant No.CMS-CSST-2021-B06)。
文摘Rings and asymmetries in protoplanetary disks are considered as signposts of ongoing planet formation.In this work,we con-duct three-dimensional radiative transfer simulations to model the intriguing disk around HD143006 that has three dust rings and a bright arc.A complex geometric configuration,with a misaligned inner disk,is assumed to account for the asymmetric structures.The two-dimensional surface density is constructed by iteratively fitting the ALMA data.We find that the dust tem-perature displays a notable discontinuity at the boundary of the misalignment.The ring masses range from 0.6 to 16 M⊕that are systematically lower than those inferred in the younger HL Tau disk.The arc occupies nearly 20%of the total dust mass.Such a high mass fraction of dust grains concentrated in a local region is consistent with the mechanism of dust trapping into vortices.Assuming a gas-to-dust mass ratio of 30 that is constant throughout the disk,the dense and cold arc is close to the threshold of being gravitationally unstable,with the Toomre parameter Q∼1.3.Nevertheless,our estimate of Q relies on the assumption for the unknown gas-to-dust mass ratio.Adopting a lower gas-to-dust mass ratio would increase the inferred Q value.Follow-up high resolution observations of dust and gas lines are needed to clarify the origin of the substructures.
基金supported by the National Natural Science Foundation of China(Grant No.11973090)the Science Research Grants from the China Manned Space Project(Grant No.CMS-CSST-2021-B06)+2 种基金supported by the European Research Council(ERC)under the European Union’s Horizon 2020 Research and Innovation Program(Grant No.757957)supported by the Netherlands Organisation for Scientific Research(Grant No.016.Veni.192.233)STFC Ernest Rutherford Fellowship(Grant No.ST/T003855/1)。
文摘Turbulent motions are believed to regulate angular momentum transport and influence dust evolution in protoplanetary disks.Measuring the strength of turbulence is challenging through gas line observations because of the requirement for high spatial and spectral resolution data,and an exquisite determination of the temperature.In this work,taking the well-known HD 163296 disk as an example,we investigated the contrast of gaps identified in high angular resolution continuum images as a probe for the level of turbulence.With self-consistent radiative transfer models,we simultaneously analyzed the radial brightness profiles along the disk major and minor axes,and the azimuthal brightness profiles of the B67 and B100 rings.By fitting all the gap contrasts measured from these profiles,we constrained the gas-to-dust scale height ratioΛto be 3.0^(+0.3)_(−0.8),1.2^(+0.1)_(−0.1),and≥6.5 for the D48,B67,and B100 regions,respectively.The varying gas-to-dust scale height ratios indicate that the degree of dust settling changes with radius.The inferred values forΛtranslate into a turbulence level of α_(turb)<3×10^(−3) in the D48 and B100 regions,which is consistent with previous upper limits set by gas line observations.However,turbulent motions in the B67 ring are strong with α_(turb)∼1.2×10^(−2).Due to the degeneracy betweenΛand the depth of dust surface density drops,the turbulence strength in the D86 gap region is not constrained.
