For a counterintuitive relative flow direction — parallel to
the disk midplane — we find that the structures generated by these distortions can very roughly approximate the HD 61005 morphology.
Alternatively, turbulence or charging effects might lead to a reservoir of small grains at the surface layer that is not affected by the dust growth and fragmentation cycle dominating the dense
disk midplane.
Interestingly, it shows a prominent equatorial dark lane sandwiched between two brighter features, due to relatively low temperature and high optical depth near
the disk midplane.
Not exact matches
It was injected 9 astronomical units from the central prostar and is now in the
disk's
midplane.
I will present new numerical models that treat dust coagulation / fragmentation, dust dynamics, simple gas - grain chemistry, and vapor diffusion simultaneously, and explore the connection between the water vapor in the
disk atmosphere and the size - distribution and ice - to - rock ratios of the dust grains growing in the
midplane.
These grains weren't seen, which probably means that they have grown and sunk to the
midplane of the
disk where they can aggregate into water - rich planets.