Zobrazeno 1 - 10
of 90
pro vyhledávání: '"Browning, Matthew K."'
Convection in stars and planets must be maintained against viscous and Ohmic dissipation. Here, we present the first systematic investigation of viscous dissipation in simulations of rotating, density-stratified plane layers of convection. Our simula
Externí odkaz:
http://arxiv.org/abs/2401.11883
We review the state of the art of three dimensional numerical simulations of solar and stellar dynamos. We summarize fundamental constraints of numerical modelling and the techniques to alleviate these restrictions. Brief summary of the relevant obse
Externí odkaz:
http://arxiv.org/abs/2305.16790
We present numerical simulations, using two complementary setups, of rotating Boussinesq thermal convection in a three-dimensional Cartesian geometry with misaligned gravity and rotation vectors. This model represents a small region at a non-polar la
Externí odkaz:
http://arxiv.org/abs/2002.02461
Autor:
Drake, Jeremy J., Alvarado-Gómez, Julián D., Airapetian, Vladimir, Cauley, P. Wilson, Argiroffi, Costanza, Browning, Matthew K., Christian, Damian J., Cohen, Ofer, Corrales, Lia, Danchi, William, de Val-Borro, Miguel, Dong, Chuanfei, Forman, William, France, Kevin, Gallo, Elena, Garcia-Sage, Katherine, Garraffo, Cecilia, Gelino, Dawn M., Gronoff, Guillaume, Günther, H. Moritz, Harper, Graham M., Haywood, Raphaëlle D., Karovska, Margarita, Kashyap, Vinay, Kastner, Joel, Kim, Jinyoung Serena, Leutenegger, Maurice A., Linsky, Jeffrey, López-Morales, Mercedes, Micela, Giusi, Moschou, Sofia-Paraskevi, Oskinova, Lidia, Osten, Rachel A., Owen, James E., Poppenhaeger, Katja, Principe, David A., Pye, John P., Sciortino, Salvatore, Tzanavaris, Panayiotis, Wargelin, Brad, Wheatley, Peter J., Williams, Peter K. G., Winston, Elaine, Wolk, Scott J.
It is now recognized that energetic stellar photon and particle radiation evaporates and erodes planetary atmospheres and controls upper atmospheric chemistry. Key exoplanet host stars will be too faint at X-ray wavelengths for accurate characterizat
Externí odkaz:
http://arxiv.org/abs/1903.12338
Some low-mass stars appear to have larger radii than predicted by standard 1D structure models; prior work has suggested that inefficient convective heat transport, due to rotation and/or magnetism, may ultimately be responsible. We examine this issu
Externí odkaz:
http://arxiv.org/abs/1803.02664
Autor:
Currie, Laura K., Browning, Matthew K.
Convection in astrophysical systems must be maintained against dissipation. Although the effects of dissipation are often assumed to be negligible, theory suggests that in strongly stratified convecting fluids, the dissipative heating rate can exceed
Externí odkaz:
http://arxiv.org/abs/1707.08858
Autor:
Mayne, N. J., Debras, F., Baraffe, I., Thuburn, John, Amundsen, David S., Acreman, David M., Smith, Chris, Browning, Matthew K., Manners, James, Wood, Nigel
Publikováno v:
A&A 604, A79 (2017)
We present highlights from a large set of simulations of a hot Jupiter atmosphere, nominally based on HD 209458b, aimed at exploring both the evolution of the deep atmosphere, and the acceleration of the zonal flow or jet. We find the occurrence of a
Externí odkaz:
http://arxiv.org/abs/1704.00539
Autor:
Weber, Maria A., Browning, Matthew K., Boardman, Suzannah, Clarke, Joshua, Pugsley, Samuel, Townsend, Edward
Evidence of surface magnetism is now observed on an increasing number of cool stars. The detailed manner by which dynamo-generated magnetic fields giving rise to starspots traverse the convection zone still remains unclear. Some insight into this flu
Externí odkaz:
http://arxiv.org/abs/1703.04982
Autor:
Weber, Maria A., Browning, Matthew K.
Many fully convective stars exhibit a wide variety of surface magnetism, including starspots and chromospheric activity. The manner by which bundles of magnetic field traverse portions of the convection zone to emerge at the stellar surface is not es
Externí odkaz:
http://arxiv.org/abs/1606.00380
Observations have suggested that some low-mass stars have larger radii than predicted by 1-D structure models. Some theoretical models have invoked very strong interior magnetic fields (of order 1 MG or more) as a possible cause of such large radii.
Externí odkaz:
http://arxiv.org/abs/1512.05692