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@@ -204,7 +204,7 @@ <h2 class="animated-heading">Searching For Light Knights in the Dark</h2>
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 <p> How do massive stars die? What triggers these cataclysmic catastrophes? 
 
-My research has centered around the first detection of <a href="https://ui.adsabs.harvard.edu/abs/2020PhRvD.101h4002A/abstract">GWs</a> from <a href="https://ui.adsabs.harvard.edu/abs/2016PhRvD..93d2002G/abstract">core-collapse supernovae (CCSNe)</a> using both terrestrial and <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240513211G/abstract">proposed lunar-based interferometers</a>. Detecting GWs from a CCSN would mark the next watershed moment in the nascent field of GW astronomy. GWs, generated by the quadrupole distribution of energy and mass, are intricately linked to the inner dynamics of the explosion mechanism triggering a core-collapse supernova. They provide unprecedented insights into the degrees of asymmetry at the moment of explosion and the underlying mechanisms causing the explosion of a massive star.
+My research has centered around the first detection of <a href="https://ui.adsabs.harvard.edu/abs/2020PhRvD.101h4002A/abstract">gravitational waves (GWs)</a> from <a href="https://ui.adsabs.harvard.edu/abs/2016PhRvD..93d2002G/abstract">core-collapse supernovae (CCSNe)</a> using both terrestrial and <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240513211G/abstract">proposed lunar-based interferometers</a>. Detecting GWs from a CCSN would mark the next watershed moment in the nascent field of GW astronomy. GWs, generated by the quadrupole distribution of energy and mass, are intricately linked to the inner dynamics of the explosion mechanism triggering a core-collapse supernova. They provide unprecedented insights into the degrees of asymmetry at the moment of explosion and the underlying mechanisms causing the explosion of a massive star.
 
 Recent neutrino-driven CCSN simulations have begun to converge on the essential phases and signatures of the GW signal and their origin in supernova microphysics. GW astronomy for CCSNe presents unique challenges compared to detecting GWs from compact binary systems: while the waveforms are expected to be predominantly stochastic, critical deterministic features carry imprints of the underlying physics. Additionally, the energy conversion into GWs varies depending on the progenitor and the detailed explosion mechanism. Even the most favorable GW emission mechanisms suggest detectability with current and proposed laser interferometers does not extend beyond the local Universe (a few tens of megaparsecs). For many models, the expected detection range is within our galaxy, where the rate of CCSNe is about 1 in 50 years. Therefore, performing GW science with CCSNe requires concerted efforts across multiple fields. This includes improving GW detector sensitivities, continuing the development of reliable CCSNe simulations, incorporating progenitor physics along with using <a href="https://ui.adsabs.harvard.edu/abs/2022ApJ...931..159G/abstract">optical data from telescopes around the world</a>, and advancing data analysis techniques to establish a true multi-messenger approach by combining all available observations.</p>    </div>