English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The abundance and distribution of ice in protoplanetary disks (PPD) iscritical to understand the linkage between the composition of circumstellarmatter and the composition of exoplanets. Edge-on PPDs are a useful tool toconstrain such ice composition and its location in the disk, as ice spectralsignatures can be observed in absorption against the continuum emission arisingfrom the warmer central disk regions. The aim of this work is to model iceabsorption features in PPDs and determine how well the abundance of the mainice species across the disk can be determined within the uncertainty of thephysical parameter space. The edge-on PPD around HH 48 NE, a target of the JWSTERS program IceAge, is used as a reference system. We use RADMC-3D to raytracethe mid-infrared continuum. Using a constant parameterized ice abundance, iceopacities are added to the dust opacity in regions wherever the disk is coldenough for the main carbon, oxygen and nitrogen carriers to freeze out. Theglobal abundance of the main ice carriers in HH 48 NE can be determined withina factor of 3, when taking the uncertainty of the physical parameters intoaccount. Ice features in PPDs can be saturated at an optical depth <1, due tolocal saturation. Spatially observed ice optical depths cannot be directlyrelated to column densities due to radiative transfer effects. Verticalsnowlines will not be a clear transition due to the radially increasing heightof the snowsurface, but their location may be constrained from observationsusing radiative transfer modeling. Radial snowlines are not really accesible.Not only the ice abundance, but also inclination, settling, grain sizedistribution and disk mass have strong impact on the observed ice absorptionfeatures in disks. Relative changes in ice abundance can be inferred fromobservations only if the source structure is well constrained

The edge-on protoplanetary disk HH 48 NE II. Modeling ices and silicates