protoplanetary disks
Volatiles in Protoplanetary Disks
... Because protoplanetary disks are complicated structures, the multi-wavelength molecular mapping method should be used with some caution, however. The flux of each line will arise from a range of disk ...
141
Multiwavelength optical properties of compact dust aggregates in protoplanetary disks
... We have shown how to best approximate the optical properties of dust aggregates in protoplanetary disks. The best match with the exact aggregate computations was reached with the DHS model with e ff ective ...
10
Dust Evolution Can Produce Scattered Light Gaps in Protoplanetary Disks
... The general behavior described above, including the region depleted of small particles noted in IV, have already appeared in various numerical simulations of particle evolution in protoplanetary disks ( ...
6
Ro-vibrational excitation of an organic molecule (HCN) in protoplanetary disks
... Context. Organic molecules are important constituents of protoplanetary disks. Their ro-vibrational lines observed in the near- and mid-infrared are commonly detected toward T Tauri disks. These ...
19
Warm dust surface chemistry in protoplanetary disks Formation of phyllosilicates
... Hydration at silicate grain surfaces is an alternative mecha- nism that has been shown to occur experimentally (Rietmeijer et al. 2004; Yamamoto & Tachibana 2016; Guillou et al. 2015). As an activated process, the ...
17
A 'Rosetta Stone' for protoplanetary disks : the synergy of multi wavelength observations
... in disks, with the former structures being common in millimeter imaging and the latter in the visible/near-IR scattered ...Some disks that show clear holes in mm interferometry show no holes in ...
37
Chemical Processes in Protoplanetary Disks. II. On the Importance of Photochemistry and X-Ray Ionization
... Protoplanetary disks are physically and thus, chemically, complex objects (see, e.g., Bergin et al. 2007). They are heavily irradiated by UV radiation from their parent T Tauri star and are permeated by ...
19
An ALMA Survey of DCN/H13CN and DCO+/H13CO+in Protoplanetary Disks
... As a first-order approximation, the disk-averaged D/H analysis in the previous subsection assumed that the deuterated isotopologues are largely co-spatial with their non-deuterated forms. Here, we examine the ef- fects ...
37
Protoplanetary Disks in ρ Ophiuchus as Seen from ALMA
... detect disks associated with 29 single sources, 11 binaries, 3 triple systems, and 4 transition ...these protoplanetary disks with that of the disk population of the Taurus – Auriga molecular ...that ...
19
Chemical complexity in protoplanetary disks in the era of ALMA and Rosetta
... a protoplanetary disk around a T Tauri ...in protoplanetary disks given that the disk inherits only simple ices (H 2 O, CO 2 , CO, N 2 , CH 4 , NH 3 , and CH 3 ...
6
The Physical Structure of Protoplanetary Disks: The Serpens Cluster Compared with Other Regions
... time disks become fainter and the disk fractions ...flat disks present wider, overlapping ...for disks around Herbig Ae/Be ...within disks have short timescales, happening repeatedly, making ...
15
Mid IR water and silicate relation in protoplanetary disks
... Dust is assumed to constitute only 1% of the disk mass, but it is a bolometric source of opacity, able to suppress line fluxes. Dust also plays a role in the thermal balance of the disk, due to the photoelectric e ff ...
7
CN rings in full protoplanetary disks around young stars as probes of disk structure
... of protoplanetary disks have shown that lines from CO and its isotopologues, the molecules usually adopted to measure the disk mass, are much weaker than ex- pected in many disks ...
12
Understanding the water emission in the mid and far IR from protoplanetary disks around T Tauri stars
... Water is a fundamental component of protoplanetary disks. Its role is already pivotal in the disk formation phase as an im- portant coolant in the cloud collapse (see, e.g., recent works, Zinnecker & ...
30
The 69 {$μ$}m forsterite band in spectra of protoplanetary disks. Results from the Herschel DIGIT programme
... For one source in our sample, HD 100546, we seem to be able to rule out the radial-mixing scenario. For this system a full radiative transfer model (Mulders et al. 2011) is available which shows that the forsterite is ...
25
Evidence for a correlation between mass accretion rates onto young stars and the mass of their protoplanetary disks
... p-value = 0.3). When considering uncertainties on the measure- ments we find a value for the correlation coe ffi cient of 0.5 + −0.6 0.4 , and thus we find no correlation. We obtain the same statistically insignificant ...
6
X ray radiative transfer in protoplanetary disks : The role of dust and X ray background fields
... We note that we do not treat the depletion of gas-phase ele- ment abundances and the dust composition, which determines the element abundances in solids, consistently. Our approach here is to use the same dust properties ...
19
Radiation thermo chemical models of protoplanetary disks : grain and polycyclic aromatic hydrocarbon charging
... in protoplanetary disks is computed consistently with the ohmic and ambipolar diffusion, whose resistivities depend on the abundance of the charge carriers (free electrons, gas-phase atomic and molecular ...
28
On the Commonality of 10-30 AU Sized Axisymmetric Dust Structures in Protoplanetary Disks
... gas-rich protoplanetary disks should drive millimeter- / meter-sized particles inward to the central star before large bodies can ...four disks ( TW Hya, HL Tau, HD 163296, and DM Tau ) , a sample of ...
7
Chemical Evolution of Protoplanetary Disks—The Effects of Viscous Accretion, Turbulent Mixing, and Disk Winds
... We calculate the chemical evolution of protoplanetary disks considering radial viscous accretion, vertical turbulent mixing, and vertical disk winds. We study the effects on the disk chemical structure when ...
22