13 citations · 24 across the 4 of their papers we have counts for
6 papers
Three-dimensional simulations of accretion disks in pre-CE systems -- II. Accretion efficiency and angular momentum transport
Ana L. Juarez-Garcia, Mike Y. M. Lau, Orsola De Marco +3
Rapid mass transfer preceding a common envelope event is a critical yet poorly understood stage of binary stellar evolution, setting the initial conditions for the common envelope…
Second Generation Planet Formation in Post-AGB Discs - II: Dust Coagulation and Core Accretion
Ali Pourmand, Orsola De Marco, Devika Kamath +1
Observations have established that the circumbinary discs formed around post-asymptotic giant branch (post-AGB) binaries have striking similarities to protoplanetary discs around y…
Weakened inspirals -- I: High mass ratio common envelope interactions in RGB stars
Jack Patrick Nibbs, Orsola De Marco, Lionel Siess +2
The common envelope (CE) interaction between an expanding giant star and a compact companion typically leads to a rapid orbital decay, ending in either a merger or the formation of…
Common envelopes in massive stars III. The obstructive role of radiation transport in envelope ejection
Mike Y. M. Lau, Ryosuke Hirai, Daniel J. Price +2
We present 3D radiation hydrodynamics simulations of common-envelope (CE) evolution involving a 12 solar mass red supergiant donor and a 3 solar mass companion. Existing 3D simulat…
Dust formation during the interaction of binary stars by common envelope
Luis C. Bermúdez-Bustamante, Orsola De Marco, Lionel Siess +7
We performed numerical simulations of the common envelope (CE) interaction between two intermediate-mass asymptotic giant branch (AGB) stars and their low-mass companions. For the…
Dust formation in common envelope binary interactions -- II: 3D simulations with self-consistent dust formation
Luis C. Bermúdez-Bustamante, Orsola De Marco, Lionel Siess +7
We performed numerical simulations of the common envelope (CE) interaction between thermally-pulsing asymptotic giant branch (AGB) stars of 1.7~\Msun and 3.7~\Msun, respectively, a…