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added SEOBNR-PM and links to AEI and Humboldt webpages
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images/SEOBNR-PM_waveform.png

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index.html

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@@ -46,6 +46,8 @@ <h1 id="title">Raj Patil</h1>
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<div id="logo">
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<!-- <h2><a href=''>Curriculum Vitae</a></h2> -->
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<h2>&nbsp</h2>
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<h2>Webpage &nbsp <a href="https://www.aei.mpg.de/person/124916/138766" target="_blank">[AEI]</a> &nbsp <a href="https://www2.hu-berlin.de/rtg2575/members/doctoral-students/" target="_blank">[Humboldt]</a></h2>
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<h2>&nbsp</h2>
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<h2><a href="https://inspirehep.net/authors/1829940" target="_blank">[iNSPIRE]</a></h2>
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<h2>&nbsp</h2>
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<h2><a href="https://github.com/raj-physics" target="_blank">[GitHub]</a></h2>
@@ -242,7 +244,20 @@ <h2>Research</h2> <h4>(Details)</h4>
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</p>
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<div id="floatedR">
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<figure>
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<img class="image fit" src="./images/SEOBNR-PM_waveform.png" />
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<figcaption><font style="font-size:12px;" >q is the mass ratio (m1/m2) and chi1 and chi2 are the spins </a> </font></figcaption>
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</figure>
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<p> I am also working on developing SEOBNR-PM <a href="https://arxiv.org/abs/2405.19181" target="_blank"> [arXiv:2405.19181] </a> which is a bound-orbit waveform model that uses the post-Minkowskian (PM) results in the effective one body (EOB) formalism. A typical time-domain waveform model uses the Hamiltonian (for conservative effects) and Fluxes (for dissipative effects) to evolve the dynamics of the binary system in the inspiral phase when the orbital radius is slowly decaying due to gravitational wave emission. Then when two compact objects collide on each other, a numerical relativity (NR) and black hole perturbation theory informed templated is used to model the merger and the ringdown. In SEOBNR-PM we use the PM scattering angle (upto 4PM for non-spinning and 5PM for spinning) to construct a PM Hamiltonian, which is a new feature of this model. Here is one example of a waveform generated using the model and its comparison to the corresponding NR waveform.
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