<?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%">D. Huang</style></author><author><style face="normal" font="default" size="100%">Y. Li</style></author><author><style face="normal" font="default" size="100%">Khan, A</style></author><author><style face="normal" font="default" size="100%">Sossi, P.</style></author><author><style face="normal" font="default" size="100%">Giardini, D</style></author><author><style face="normal" font="default" size="100%">Murakami, M.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Thermoelastic Properties of Liquid Fe‐Rich Alloys Under Martian Core Conditions</style></title><secondary-title><style face="normal" font="default" size="100%">Geophysical Research Letters</style></secondary-title></titles><dates><year><style  face="normal" font="default" size="100%">2023</style></year><pub-dates><date><style  face="normal" font="default" size="100%">mar</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://onlinelibrary.wiley.com/doi/10.1029/2022GL102271 https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2022GL102271</style></url></web-urls></urls><number><style face="normal" font="default" size="100%">6</style></number><volume><style face="normal" font="default" size="100%">50</style></volume><pages><style face="normal" font="default" size="100%">1–11</style></pages><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">Seismic measurements made on Mars indicate that the liquid iron‐nickel core is rich in light elements; however, the effects of these light components on the elasticity of Mars&amp;#039; core remain poorly constrained. Here, we calculate elastic properties of various liquid Fe‐X (X = Ni, S, C, O and H) mixtures using ab initio molecular dynamics simulations. We find that, at martian core conditions, the addition of S and O most effectively decreases the density of liquid iron, followed by C and H, while Ni has a minimal effect. As for compressional sound velocity (Vp), C increases Vp of liquid Fe throughout Mars&amp;#039; core, while both S and O reduce Vp, the intensity of which diminishes with increasing pressure. Assuming a martian core made of a binary mixture, the seismically‐inferred density would require the presence of at least 30 wt% S.</style></abstract></record></records></xml>