<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Sam De Abreu</style></author><author><style face="normal" font="default" size="100%">Rosalie M. Cormier</style></author><author><style face="normal" font="default" size="100%">Mikhail G. Schee</style></author><author><style face="normal" font="default" size="100%">Varvara E. Zemskova</style></author><author><style face="normal" font="default" size="100%">Erica Rosenblum</style></author><author><style face="normal" font="default" size="100%">Nicolas Grisouard</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Two-dimensional numerical simulations of mixing under ice keels</style></title><secondary-title><style face="normal" font="default" size="100%">The Cryosphere</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2024</style></year></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://tc.copernicus.org/articles/18/3159/2024/</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">18</style></volume><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Changes in sea ice conditions directly impact the way the wind transfers energy to the Arctic Ocean. The thinning and increasing mobility of sea ice is expected to change the size and speed of ridges on the underside of ice floes, called ice keels, which cause turbulence and impact upper-ocean stratification. However, the effects of changing ice keel characteristics on below-ice mixing are difficult to determine from sparse observations and have not been directly investigated in numerical or laboratory experiments. Here, for the first time, we examine how the size and speed of an ice keel affect the mixing of various upper-ocean stratifications using 16 two-dimensional numerical simulations of a keel moving through a two-layer flow. We find that the irreversible ocean mixing and the characteristic depth over which mixing occurs each vary significantly across a realistic parameter space of keel sizes, keel speeds, and ocean stratifications. Furthermore, we find that mixing does not increase monotonically with ice keel depth and speed but instead depends on the emergence and propagation of vortices and turbulence. These results suggest that changes to ice keel speed and depth may have a significant impact on below-ice mixing across the Arctic Ocean and highlight the need for more realistic numerical simulations and observational estimates of ice keel characteristics.</style></abstract><issue><style face="normal" font="default" size="100%">7</style></issue></record><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">M.H. Kelsey</style></author><author><style face="normal" font="default" size="100%">R. Agnese</style></author><author><style face="normal" font="default" size="100%">Y.F. Alam</style></author><author><style face="normal" font="default" size="100%">I. Ataee Langroudy</style></author><author><style face="normal" font="default" size="100%">E. Azadbakht</style></author><author><style face="normal" font="default" size="100%">D. Brandt</style></author><author><style face="normal" font="default" size="100%">R. Bunker</style></author><author><style face="normal" font="default" size="100%">B. Cabrera</style></author><author><style face="normal" font="default" size="100%">Y.-Y. Chang</style></author><author><style face="normal" font="default" size="100%">H. Coombes</style></author><author><style face="normal" font="default" size="100%">R.M. Cormier</style></author><author><style face="normal" font="default" size="100%">M.D. Diamond</style></author><author><style face="normal" font="default" size="100%">E.R. Edwards</style></author><author><style face="normal" font="default" size="100%">E. Figueroa-Feliciano</style></author><author><style face="normal" font="default" size="100%">J. Gao</style></author><author><style face="normal" font="default" size="100%">P.M. Harrington</style></author><author><style face="normal" font="default" size="100%">Z. Hong</style></author><author><style face="normal" font="default" size="100%">M. Hui</style></author><author><style face="normal" font="default" size="100%">N.A. Kurinsky</style></author><author><style face="normal" font="default" size="100%">R.E. Lawrence</style></author><author><style face="normal" font="default" size="100%">B. Loer</style></author><author><style face="normal" font="default" size="100%">M.G. Masten</style></author><author><style face="normal" font="default" size="100%">E. Michaud</style></author><author><style face="normal" font="default" size="100%">E. Michielin</style></author><author><style face="normal" font="default" size="100%">J. Miller</style></author><author><style face="normal" font="default" size="100%">V. Novati</style></author><author><style face="normal" font="default" size="100%">N.S. Oblath</style></author><author><style face="normal" font="default" size="100%">J.L. Orrell</style></author><author><style face="normal" font="default" size="100%">W.L. Perry</style></author><author><style face="normal" font="default" size="100%">P. Redl</style></author><author><style face="normal" font="default" size="100%">T. Reynolds</style></author><author><style face="normal" font="default" size="100%">T. Saab</style></author><author><style face="normal" font="default" size="100%">B. Sadoulet</style></author><author><style face="normal" font="default" size="100%">K. Serniak</style></author><author><style face="normal" font="default" size="100%">J. Singh</style></author><author><style face="normal" font="default" size="100%">Z. Speaks</style></author><author><style face="normal" font="default" size="100%">C. Stanford</style></author><author><style face="normal" font="default" size="100%">J.R. Stevens</style></author><author><style face="normal" font="default" size="100%">J. Strube</style></author><author><style face="normal" font="default" size="100%">D. Toback</style></author><author><style face="normal" font="default" size="100%">J.N. Ullom</style></author><author><style face="normal" font="default" size="100%">B.A. VanDevender</style></author><author><style face="normal" font="default" size="100%">M.R. Vissers</style></author><author><style face="normal" font="default" size="100%">M.J. Wilson</style></author><author><style face="normal" font="default" size="100%">J.S. Wilson</style></author><author><style face="normal" font="default" size="100%">B. Zatschler</style></author><author><style face="normal" font="default" size="100%">S. Zatschler</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">G4CMP: Condensed matter physics simulation using the Geant4 toolkit</style></title><secondary-title><style face="normal" font="default" size="100%">Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2023</style></year></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://www.sciencedirect.com/science/article/pii/S0168900223004631?via%3Dihub</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">1055</style></volume><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">G4CMP simulates phonon and charge transport in cryogenic semiconductor crystals using the Geant4 toolkit. The transport code is capable of simulating the propagation of acoustic phonons as well as electron and hole charge carriers. Processes for anisotropic phonon propagation, oblique charge-carrier propagation, and phonon emission by accelerated charge carriers are included. The simulation reproduces theoretical predictions and experimental observations such as phonon caustics, heat-pulse propagation times, and mean charge-carrier drift velocities. In addition to presenting the physics and features supported by G4CMP, this report outlines example applications from the dark matter and quantum information science communities. These communities are applying G4CMP to model and design devices for which the energy transported by phonons and charge carriers is germane to the performance of superconducting instruments and circuits placed on silicon and germanium substrates. The G4CMP package is available to download from GitHub: github.com/kelseymh/G4CMP.</style></abstract></record></records></xml>