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contents/kmhd.html

@@ -394,7 +394,10 @@ <h2 id="toc-title">Table of contents</h2>
 
   <ul>
   <li><a href="#sec-firehose" id="toc-sec-firehose" class="nav-link active" data-scroll-target="#sec-firehose"><span class="header-section-number">14.1</span> Firehose Instability: Linear Theory</a></li>
-  <li><a href="#sec-mirror" id="toc-sec-mirror" class="nav-link" data-scroll-target="#sec-mirror"><span class="header-section-number">14.2</span> Mirror Instability: Linear Theory</a></li>
+  <li><a href="#sec-mirror" id="toc-sec-mirror" class="nav-link" data-scroll-target="#sec-mirror"><span class="header-section-number">14.2</span> Mirror Instability: Linear Theory</a>
+  <ul class="collapse">
+  <li><a href="#comparison-with-slow-mode" id="toc-comparison-with-slow-mode" class="nav-link" data-scroll-target="#comparison-with-slow-mode"><span class="header-section-number">14.2.1</span> Comparison With Slow Mode</a></li>
+  </ul></li>
   <li><a href="#origin-of-pressure-anisotropy" id="toc-origin-of-pressure-anisotropy" class="nav-link" data-scroll-target="#origin-of-pressure-anisotropy"><span class="header-section-number">14.3</span> Origin of Pressure Anisotropy</a></li>
   <li><a href="#remarks" id="toc-remarks" class="nav-link" data-scroll-target="#remarks"><span class="header-section-number">14.4</span> Remarks</a>
   <ul class="collapse">
@@ -788,6 +791,26 @@ <h2 data-number="14.2" class="anchored" data-anchor-id="sec-mirror"><span class=
 </figcaption>
 </figure>
 </div>
+<section id="comparison-with-slow-mode" class="level3" data-number="14.2.1">
+<h3 data-number="14.2.1" class="anchored" data-anchor-id="comparison-with-slow-mode"><span class="header-section-number">14.2.1</span> Comparison With Slow Mode</h3>
+<ul>
+<li>Driving Mechanism
+<ul>
+<li>Mirror Mode: Driven primarily by pressure anisotropy (<span class="math inline">\(T_\perp/T_\parallel &gt; 1\)</span>) in high-beta plasmas.</li>
+<li>MHD Slow Mode: Driven by pressure gradients and magnetic field line curvature in low- to moderate-beta plasmas.</li>
+</ul></li>
+<li>Propagation Characteristics
+<ul>
+<li>Mirror Mode: Primarily propagates parallel to the background magnetic field, but can have a small perpendicular component. It is a non-propagating mode in the fluid limit (zero frequency), but it can acquire a finite frequency due to kinetic effects.</li>
+<li>MHD Slow Mode: Propagates obliquely to the magnetic field, with both parallel and perpendicular components. It is a propagating mode with a finite frequency.</li>
+</ul></li>
+<li>Plasma Conditions
+<ul>
+<li>Mirror Mode: Typically found in high-beta (<span class="math inline">\(\gtrsim 1\)</span>) plasmas, such as the Earth’s magnetosheath and the solar wind.</li>
+<li>MHD Slow Mode: More common in low- to moderate-beta (<span class="math inline">\(\ll 1\)</span>) plasmas, such as the solar corona and the Earth’s magnetosphere, where the magnetic pressure dominates.</li>
+</ul></li>
+</ul>
+</section>
 </section>
 <section id="origin-of-pressure-anisotropy" class="level2" data-number="14.3">
 <h2 data-number="14.3" class="anchored" data-anchor-id="origin-of-pressure-anisotropy"><span class="header-section-number">14.3</span> Origin of Pressure Anisotropy</h2>