<?xml version="1.0" encoding="utf-8" standalone="yes"?><rss version="2.0" xmlns:atom="http://www.w3.org/2005/Atom"><channel><title>research on zhi</title><link>https://zhichen3.github.io/research/</link><description>Recent content in research on zhi</description><generator>Hugo</generator><language>en-us</language><lastBuildDate>Sun, 02 Feb 2025 00:00:00 -0500</lastBuildDate><atom:link href="https://zhichen3.github.io/research/index.xml" rel="self" type="application/rss+xml"/><item><title>Sensitivity of He Flames in X-ray Bursts to Nuclear Physics</title><link>https://zhichen3.github.io/research/xrb-sensitivity/</link><pubDate>Sun, 02 Feb 2025 00:00:00 -0500</pubDate><guid>https://zhichen3.github.io/research/xrb-sensitivity/</guid><description>&lt;figure class="resource-copy">&lt;img src="https://zhichen3.github.io/research/xrb-sensitivity/network_abar_50ms.png">
&lt;/figure>

&lt;h2 id="introduction">Introduction&lt;/h2> &lt;p>Millisecond burst oscillation phenomenon is often observed during the rise time
of the X-ray burst light curve, where the oscillation frequency matches with the
X-ray emission pulsation of the neutron star within few Hz.
The modulation of asymmetrical burning on the surface of the neutron star
due to the spreading of the initial local hotspot is the current contender theory
that explains this behavior.
Many have attempted to model the laterally flame propagation on the neutron star surface,
with successes at studying the flame front and calculating the flame speed.
In this project, I conducted a sensitivity test on how choices of nuclear reaction network,
plasma screening routines, and integration coupling methods can influence the He flame dynamics.
Details of the work is published in &lt;a href="https://iopscience.iop.org/article/10.3847/1538-4357/acec72" target="_blank" rel="noopener">ApJ&lt;/a> .
&lt;strong>Here I&amp;rsquo;ll just summarize the most important finding on the effect of nuclear reaction network
on flame dynamics and nucleosynthesis&lt;/strong>.&lt;/p></description></item><item><title>Interferometry</title><link>https://zhichen3.github.io/research/interferometry/</link><pubDate>Sun, 02 Feb 2025 00:00:00 -0500</pubDate><guid>https://zhichen3.github.io/research/interferometry/</guid><description>&lt;figure class="resource-copy">&lt;img src="https://zhichen3.github.io/research/interferometry/interferometry_setup.png">
&lt;/figure>

&lt;p>This was my research project during my &lt;a href="https://science.osti.gov/wdts/suli" target="_blank" rel="noopener">SULI&lt;/a> internship in 2021.
I was interested in estimating the precision of the
&lt;a href="https://astro.theoj.org/article/39641-two-photon-amplitude-interferometry-for-precision-astrometry" target="_blank" rel="noopener">two-photon interferometry&lt;/a> technique
for measuring the relative separation between two light-sources (i.e. stars)
using Markov-Chain Monte Carlos (MCMC) simulation.&lt;/p>
&lt;h2 id="two-photon-interferometer-overview">Two-photon Interferometer Overview&lt;/h2> &lt;p>Assume there are two sources which can be observed simultaneously from two stations,
&lt;strong>L&lt;/strong> and &lt;strong>R&lt;/strong> , with single spatial mode inputs &lt;em>a&lt;/em>, &lt;em>b&lt;/em> and &lt;em>e&lt;/em>, &lt;em>f&lt;/em>.
Both sources send out photons in the form of plane wave, the path length difference
between the two stations yielding phase delays \(\delta_1\) and \(\delta_2\) between the photons observed
at channels &lt;em>a&lt;/em>, &lt;em>e&lt;/em> from source 1 and &lt;em>b&lt;/em>, &lt;em>f&lt;/em> from source 2, respectively.
If the two detected photons are close enough in frequency and arrival time,
then the pattern of coincidences measured at the outputs &lt;em>c&lt;/em>, &lt;em>d&lt;/em> and &lt;em>g&lt;/em>, &lt;em>h&lt;/em>
will be sensitive to the difference in phase delays
after interference at the symmetric beam splitter in each station.&lt;/p></description></item></channel></rss>