Zobrazeno 1 - 10
of 267
pro vyhledávání: '"Hartquist, T. W."'
At the time of formation, protoplanetary discs likely contain a comparable mass to their host protostars. As a result, gravitational instabilities (GIs) are expected to play a pivotal role in the early phases of disc evolution. However, as these youn
Externí odkaz:
http://arxiv.org/abs/1810.04537
Autor:
Ilee, J. D., Forgan, D. H., Evans, M. G., Hall, C., Booth, R., Clarke, C. J., Rice, W. K. M., Boley, A. C., Caselli, P., Hartquist, T. W., Rawlings, J. M. C.
In this paper, we model the chemical evolution of a 0.25 M$_{\odot}$ protoplanetary disc surrounding a 1 M$_{\odot}$ star that undergoes fragmentation due to self-gravity. We use Smoothed Particle Hydrodynamics including a radiative transfer scheme,
Externí odkaz:
http://arxiv.org/abs/1708.01815
Autor:
Evans, M. G., Ilee, J. D., Hartquist, T. W., Caselli, P., Szucs, L., Purser, S. J. D., Boley, A. C., Durisen, R. H., Rawlings, J. M. C.
Gravitational instabilities (GIs) are most likely a fundamental process during the early stages of protoplanetary disc formation. Recently, there have been detections of spiral features in young, embedded objects that appear consistent with GI-driven
Externí odkaz:
http://arxiv.org/abs/1706.00254
We describe the results of 3D simulations of the interaction of hydrodynamic shocks with Bonnor-Ebert spheres performed with an Adaptive Mesh Refinement code. The calculations are isothermal and the clouds are embedded in a medium in which the sound
Externí odkaz:
http://arxiv.org/abs/1612.02204
Publikováno v:
A&A 596, A28 (2016)
We numerically reproduce the density profiles for filaments that are in magnetohydrostatic and pressure equilibrium with their surroundings obtained in Tomisaka (2014) and show that these equilibria are dynamically stable. If the effect of ambipolar
Externí odkaz:
http://arxiv.org/abs/1609.06879
Autor:
Evans, M. G., Ilee, J. D., Boley, A. C., Caselli, P., Durisen, R. H., Hartquist, T. W., Rawlings, J. M. C.
To date, most simulations of the chemistry in protoplanetary discs have used 1+1D or 2D axisymmetric $\alpha$-disc models to determine chemical compositions within young systems. This assumption is inappropriate for non-axisymmetric, gravitationally
Externí odkaz:
http://arxiv.org/abs/1508.00773
We present 2D adiabatic magnetohydrodynamic (MHD) simulations of a shock interacting with groups of two or three cylindrical clouds. We study how the presence of a nearby cloud influences the dynamics of this interaction, and explore the resulting di
Externí odkaz:
http://arxiv.org/abs/1407.6579
We perform three dimensional hydrodynamic simulations of the ram pressure stripping of the hot extended gaseous halo of a massive galaxy using the k-epsilon sub-grid turbulence model at Mach numbers 0.9, 1.1 and 1.9. The k-epsilon model is used to si
Externí odkaz:
http://arxiv.org/abs/1309.5246
Autor:
Douglas, T. A., Caselli, P., Ilee, J. D., Boley, A. C., Hartquist, T. W., Durisen, R. H., Rawlings, J. M. C.
The formation and earliest stages of protoplanetary discs remain poorly constrained by observations. ALMA will soon revolutionise this field. Therefore, it is important to provide predictions which will be valuable for the interpretation of future hi
Externí odkaz:
http://arxiv.org/abs/1305.3777