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saturnaxis · Aug 7, 2023 · 409551a · 409551a
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diff --git a/Tutorials/planet-packing-stability.ipynb b/Tutorials/planet-packing-stability.ipynb
diff --git a/Tutorials/three-body-stability.ipynb b/Tutorials/three-body-stability.ipynb
@@ -658,7 +658,7 @@
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diff --git a/docs/Tutorials/planet-packing-stability.html b/docs/Tutorials/planet-packing-stability.html
diff --git a/docs/Tutorials/three-body-stability.html b/docs/Tutorials/three-body-stability.html
@@ -790,7 +790,7 @@ <h3><span class="section-number">3.3.1. </span>A sample simulation (Kepler-16b)<
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 <p>The above figures show the evolution of the planet’s eccentricity and inclination vectors.  The planetary eccentricity vector illustrates how the shape of the orbit changes over time <strong>and</strong> how the orbit can rotate relative to the binary orbital plane.  The inclination vector represents how the planetary orbit can tilt and wobble with time (i.e., like a plate on a table).  Each of these vectors can have two components: <strong>free</strong> and <strong>forced</strong>.  The forced component shifts the mean value of the vectors away from the origin.</p>
-<p>The top-left panel shows the planetary eccentricity  <span class="math notranslate nohighlight">\(e_p\)</span> changing over 100 years, while the top-middle panel shows the evolution of the planetary argument of periapse <span class="math notranslate nohighlight">\(\omega_p\)</span>.  The forced component increases the mean eccentricity to <span class="math notranslate nohighlight">\(0.034\)</span>, while the argument of periapse is <span class="math notranslate nohighlight">\({\sim}278^\circ\)</span>.  The top-right panel shows how the direction of the eccentricity vector changes over the simulation.  The red dot marks the origin, where in the absence of a forced component it would lie in the center.  Instead, all the points appear to orbit a fixed point with a radius equal to the forced eccentricity <span class="math notranslate nohighlight">\(e_F\)</span> and rotated by an angle equal to the forced argument of periapsis <span class="math notranslate nohighlight">\(\omega_F\)</span>, in polar coordinates.</p>
+<p>The top-left panel shows the planetary eccentricity  <span class="math notranslate nohighlight">\(e_p\)</span> changing over 100 years, while the top-middle panel shows the evolution of the planetary argument of periapse <span class="math notranslate nohighlight">\(\omega_p\)</span>.  The forced component increases the mean eccentricity to <span class="math notranslate nohighlight">\(0.034\)</span>, while the argument of periapse is <span class="math notranslate nohighlight">\({\sim}278^\circ\)</span>.  The top-right panel shows how the direction of the eccentricity vector changes over the simulation.  The red dot marks the origin, where in the absence of a forced component it would lie in the center.  Instead, all the points appear to orbit a fixed point with a radius equal to the forced eccentricity <span class="math notranslate nohighlight">\(e_F\)</span> and rotated by an angle equal to the forced argument of periapse <span class="math notranslate nohighlight">\(\omega_F\)</span>, in polar coordinates.</p>
 <p>The bottom row represents similar panels, but using the planetary inclination <span class="math notranslate nohighlight">\(i_p\)</span> and longitude of ascending node <span class="math notranslate nohighlight">\(\Omega_p\)</span>. The planetary orbit appears to couple tightly with the binary orbit.  Naively, this would suggest that the system will continue to transit indefinitely.  However, we must consider that the inclination shown here is the <strong>mutual inclination</strong> and if the binary orbital plane tilts relative to our line-of-sight, then the planetary orbit will also tilt along with it.  As a result, our ability to view Kepler-16b transiting its host star is temporary and will only occur when the alignment is just right (e.g., the transit of Venus or Mercury across our Sun).  More broadly, the circumbinary planet community has dubbed this ability to transit as <em>transitability</em> (see <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2015MNRAS.449..781M/abstract">Martin &amp; Triaud (2015)</a> and <a class="reference external" href="https://ui.adsabs.harvard.edu/abs/2017MNRAS.465.3235M/abstract">Martin (2017)</a> for more details).</p>
 </section>
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diff --git a/docs/_sources/Tutorials/planet-packing-stability.ipynb b/docs/_sources/Tutorials/planet-packing-stability.ipynb
diff --git a/docs/_sources/Tutorials/three-body-stability.ipynb b/docs/_sources/Tutorials/three-body-stability.ipynb
@@ -658,7 +658,7 @@
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diff --git a/docs/searchindex.js b/docs/searchindex.js