https://www.laurynewilliams.com/categories/published/Recent content in Published on Lauryn E. WilliamsHugoen-usMon, 27 Jul 2026 00:00:00 +0000https://www.laurynewilliams.com/project/hydro/Mon, 27 Jul 2026 00:00:00 +0000https://www.laurynewilliams.com/project/hydro/<hr> <h2 id="simulating-tżo-formation">Simulating TŻO Formation <a href="#simulating-t%c5%bco-formation"><svg class="anchor-symbol" aria-hidden="true" height="26" width="26" viewBox="0 0 22 22" xmlns="http://www.w3.org/2000/svg"> <path d="M0 0h24v24H0z" fill="currentColor"></path> <path d="M3.9 12c0-1.71 1.39-3.1 3.1-3.1h4V7H7c-2.76.0-5 2.24-5 5s2.24 5 5 5h4v-1.9H7c-1.71.0-3.1-1.39-3.1-3.1zM8 13h8v-2H8v2zm9-6h-4v1.9h4c1.71.0 3.1 1.39 3.1 3.1s-1.39 3.1-3.1 3.1h-4V17h4c2.76.0 5-2.24 5-5s-2.24-5-5-5z"></path> </svg></a> </h2> <p>A TŻO can be created when a newly formed neutron star (NS) gets &ldquo;kicked&rdquo; into its companion star, which we call the &ldquo;impact scenario&rdquo;.</p> <p>Using a moving mesh solver (MANGA) on top of the smooth particle hydrodynamics (SPH) code, Charm N-body GrAvity solver (ChaNGa), we simulated 5 main sequences (MS) masses spanning 5 - 15 solar masses, with three different periastron distances (<code>$r_p$</code>).</p>https://www.laurynewilliams.com/project/amnh/Sun, 26 Jul 2026 00:00:00 +0000https://www.laurynewilliams.com/project/amnh/<hr> <h3 id="identifying-dynamical-masses-of-long-period-companions-using-orbit-fitting-code-with-hgca-astrometry">Identifying Dynamical Masses of Long Period Companions Using Orbit Fitting code with HGCA Astrometry <a href="#identifying-dynamical-masses-of-long-period-companions-using-orbit-fitting-code-with-hgca-astrometry"><svg class="anchor-symbol" aria-hidden="true" height="26" width="26" viewBox="0 0 22 22" xmlns="http://www.w3.org/2000/svg"> <path d="M0 0h24v24H0z" fill="currentColor"></path> <path d="M3.9 12c0-1.71 1.39-3.1 3.1-3.1h4V7H7c-2.76.0-5 2.24-5 5s2.24 5 5 5h4v-1.9H7c-1.71.0-3.1-1.39-3.1-3.1zM8 13h8v-2H8v2zm9-6h-4v1.9h4c1.71.0 3.1 1.39 3.1 3.1s-1.39 3.1-3.1 3.1h-4V17h4c2.76.0 5-2.24 5-5s-2.24-5-5-5z"></path> </svg></a> </h3> <h2 id="background">Background <a href="#background"><svg class="anchor-symbol" aria-hidden="true" height="26" width="26" viewBox="0 0 22 22" xmlns="http://www.w3.org/2000/svg"> <path d="M0 0h24v24H0z" fill="currentColor"></path> <path d="M3.9 12c0-1.71 1.39-3.1 3.1-3.1h4V7H7c-2.76.0-5 2.24-5 5s2.24 5 5 5h4v-1.9H7c-1.71.0-3.1-1.39-3.1-3.1zM8 13h8v-2H8v2zm9-6h-4v1.9h4c1.71.0 3.1 1.39 3.1 3.1s-1.39 3.1-3.1 3.1h-4V17h4c2.76.0 5-2.24 5-5s-2.24-5-5-5z"></path> </svg></a> </h2> <p>The Hipparcos-Gaia Catalog of Accelerations contains a subset of stars that appeared to be accelerating during a cross calibration between the High Precision PARallax Collecting Satellite (HIPPARCOS) catalog and Gaia. ( <a href="https://ui.adsabs.harvard.edu/abs/2021ApJS..254...42B/abstract" target="_blank" rel="noopener">Brandt 2021</a>)</p>