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space_weather/SSA/index.html

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 <h1 id="solar-synoptic-analysis">Solar Synoptic Analysis</h1>
 <p>Synoptic maps of the solar surface are drawn each day by SWPC forecasters, providing forecasters with a broad outline of solar surface features. These maps were started on June 2, 1972 and have been produced daily since then.</p>
+<p><img alt="hmib" src="../../assets/ssa_1.webp" /></p>
 <div class="admonition quote">
 <p class="admonition-title">Source</p>
 <p>The Solar Synoptic Analysis is courtesy of the Space Weather Prediction Center (SWPC) part of the National Oceanic and Atmospheric Administration (NOAA), located in Boulder, Colorado.</p>
 </div>
 <h2 id="how-to-read">How to Read</h2>
 <h3 id="active-regions">Active Regions</h3>
-<p>Active regions are localized magnetic fields on the Sun. Areas with strong or intense magnetic fields provide energy for solar flares and coronal mass ejections (CMEs), so accurate forecasting of space weather activity requires an accurate picture of these regions.. Active regions are given official numbers by SWPC, and the drawings include the probabilities of C, M, and X class flares for the next 24 hours associated with each active region, along with a proton event probability.</p>
+<p>Active regions are localized magnetic fields on the Sun. Areas with strong or intense magnetic fields provide energy for solar flares and coronal mass ejections (CMEs), so accurate forecasting of space weather activity requires an accurate picture of these regions.
+<strong>Active regions are given official numbers by SWPC, and the drawings include the probabilities of C, M, and X class flares for the next 24 hours associated with each active region, along with a proton event probability.</strong></p>
 <h3 id="coronal-holes">Coronal Holes</h3>
-<p>Coronal holes are single polarity magnetic regions that are the source of high speed solar winds which drive magnetospheric activity. Coronal holes are the most common cause of geomagnetic storms. Coronal holes have historically been identified from He I 10830A ground-based observations. The boundaries of coronal holes are shown on the synoptic drawings as lines with hash marks on the coronal hole side of the boundary line.</p>
+<p>Coronal holes are single polarity magnetic regions that are the source of high speed solar winds which drive magnetospheric activity. Coronal holes are the most common cause of geomagnetic storms. Coronal holes have historically been identified from He I 10830A ground-based observations. <strong>The boundaries of coronal holes are shown on the synoptic drawings as lines with hash marks on the coronal hole side of the boundary line.</strong></p>
 <h3 id="neutral-lines">Neutral Lines</h3>
-<p>Large magnetic field structures of one magnetic polarity have a ‘neutral line’ at the boundary of the different magnetic polarities of the fields. Neutral lines are associated with flaring in active regions, and filaments/prominences are often associated with the neutral lines on a quiet sun. Neutral lines appear as dashed lines on the synoptic drawings and the forecaster indicates the polarity of the magnetic field on either side of the neutral line with + (positive) and – (negative) signs.</p>
+<p>Large magnetic field structures of one magnetic polarity have a ‘neutral line’ at the boundary of the different magnetic polarities of the fields. Neutral lines are associated with flaring in active regions, and filaments/prominences are often associated with the neutral lines on a quiet sun. <strong>Neutral lines appear as dashed lines on the synoptic drawings and the forecaster indicates the polarity of the magnetic field on either side of the neutral line with + (positive) and – (negative) signs.</strong></p>
 <h3 id="plages">Plages</h3>
-<p>Plages make up most of an Active Region, and appear bright in conjunction with the dark sunspots. Plages have strong magnetic fields but disorganized magnetic fields, unlike the highly organized fields of sunspots. In the synoptic drawings, plages are colored red. It is quite normal to have regions of plage with no sunspots, which do not receive an official number since they are not considered active regions and are unlikely to produce solar flares. Plage regions are the chief source of UV variability from the sun, however.</p>
+<p>Plages make up most of an Active Region, and appear bright in conjunction with the dark sunspots. Plages have strong magnetic fields but disorganized magnetic fields, unlike the highly organized fields of sunspots. <strong>In the synoptic drawings, plages are colored red.</strong> It is quite normal to have regions of plage with no sunspots, which do not receive an official number since they are not considered active regions and are unlikely to produce solar flares.</p>
 <h3 id="filaments-and-prominences">Filaments and Prominences</h3>
-<p>Highly-stable regions of high density gas in the low density corona are called filaments. When these occur near the limb and can be seen protruding from the corona, often in spectacular fashion, they are called prominences. When they erupt they can be a geomagnetic storm threat, but the eruptions are usually slow and don’t often drive large storms. The filaments and prominences are drawn as outlines with hash marks.</p>
+<p>Highly-stable regions of high density gas in the low density corona are called filaments. When these occur near the limb and can be seen protruding from the corona, often in spectacular fashion, they are called prominences. When they erupt they can be a geomagnetic storm threat, but the eruptions are usually slow and don’t often drive large storms. <strong>The filaments and prominences are drawn as outlines with hash marks.</strong></p>
 <h2 id="solar-coordinates">Solar Coordinates</h2>
 <ul>
 <li>Lt: The current Carrington longitude line (north to south) at solar center disk.</li>

space_weather/imagers/index.html

@@ -967,9 +967,9 @@
 </li>
         
           <li class="md-nav__item">
-  <a href="#303-a" class="md-nav__link">
+  <a href="#304-a" class="md-nav__link">
     <span class="md-ellipsis">
-      303 Å
+      304 Å
     </span>
   </a>
   
@@ -1324,9 +1324,9 @@
 </li>
         
           <li class="md-nav__item">
-  <a href="#303-a" class="md-nav__link">
+  <a href="#304-a" class="md-nav__link">
     <span class="md-ellipsis">
-      303 Å
+      304 Å
     </span>
   </a>
   
@@ -1469,6 +1469,7 @@
 <h1 id="sun-imagers">Sun Imagers</h1>
 <h2 id="atmospheric-imagery-assembly">Atmospheric Imagery Assembly</h2>
 <h3 id="94-a">94 Å</h3>
+<p><img alt="aia_0094" src="../../assets/aia_0094.webp" /></p>
 <p>This channel (as well as AIA 131) is designed to study solar flares. It measures extremely hot temperatures around 6 million Kelvin (10.8 million F). It can take images every 2 seconds (instead of 10) in a reduced field of view in order to look at flares in more detail.</p>
 <ul>
 <li><strong>Where:</strong> Flaring regions of the corona</li>
@@ -1477,6 +1478,7 @@
 <li><strong>Characteristic temperature:</strong> 6 million K (10.8 million F)</li>
 </ul>
 <h3 id="131-a">131 Å</h3>
+<p><img alt="aia_0131" src="../../assets/aia_0131.webp" /></p>
 <p>This channel (as well as AIA 094) is designed to study solar flares. It measures extremely hot temperatures around 10 million K (18 million F), as well as cool plasmas around 400,000 K (720,000 F). It can take images every 2 seconds (instead of 10) in a reduced field of view in order to look at flares in more detail.</p>
 <ul>
 <li><strong>Where:</strong> Flaring regions of the corona</li>
@@ -1485,6 +1487,7 @@
 <li><strong>Characteristic temperatures:</strong> 10 million K (18 million F)</li>
 </ul>
 <h3 id="171-a">171 Å</h3>
+<p><img alt="aia_0171" src="../../assets/aia_0171.webp" /></p>
 <p>This channel is especially good at showing coronal loops - the arcs extending off of the Sun where plasma moves along magnetic field lines. The brightest spots seen here are locations where the magnetic field near the surface is exceptionally strong.</p>
 <ul>
 <li><strong>Where:</strong> Quiet corona and upper transition region</li>
@@ -1493,6 +1496,7 @@
 <li><strong>Characteristic temperature:</strong> 1 million K (1.8 million F)</li>
 </ul>
 <h3 id="193-a">193 Å</h3>
+<p><img alt="aia_0193" src="../../assets/aia_0193.webp" /></p>
 <p>This channel highlights the outer atmosphere of the Sun - called the corona - as well as hot flare plasma. Hot active regions, solar flares, and coronal mass ejections will appear bright here. The dark areas - called coronal holes - are places where very little radiation is emitted, yet are the main source of solar wind particles.</p>
 <ul>
 <li><strong>Where:</strong> Corona and hot flare plasma</li>
@@ -1500,7 +1504,8 @@
 <li><strong>Primary ions seen:</strong> 11 times ionized iron (Fe XII)</li>
 <li><strong>Characteristic temperature:</strong> 1.25 million K (2.25 million F)</li>
 </ul>
-<h3 id="303-a">303 Å</h3>
+<h3 id="304-a">304 Å</h3>
+<p><img alt="aia_0304" src="../../assets/aia_0304.webp" /></p>
 <p>This channel is especially good at showing areas where cooler dense plumes of plasma (filaments and prominences) are located above the visible surface of the Sun. Many of these features either can't be seen or appear as dark lines in the other channels. The bright areas show places where the plasma has a high density.</p>
 <ul>
 <li><strong>Where:</strong> Upper chromosphere and lower transition region</li>
@@ -1509,6 +1514,7 @@
 <li><strong>Characteristic temperature:</strong> 50,000 K (90,000 F)</li>
 </ul>
 <h3 id="335-a">335 Å</h3>
+<p><img alt="aia_0335" src="../../assets/aia_0335.webp" /></p>
 <p>This channel (as well as AIA 211) highlights the active region of the outer atmosphere of the Sun - the corona. Active regions, solar flares, and coronal mass ejections will appear bright here. The dark areas - or coronal holes - are places where very little radiation is emitted, yet are the main source of solar wind particles.</p>
 <ul>
 <li><strong>Where:</strong> Active regions of the corona</li>
@@ -1517,6 +1523,7 @@
 <li><strong>Characteristic temperature:</strong> 2.8 million K (5 million F)</li>
 </ul>
 <h3 id="1600-a">1600 Å</h3>
+<p><img alt="aia_1600" src="../../assets/aia_1600.webp" /></p>
 <p>This channel (as well as AIA 1700) often shows a web-like pattern of bright areas that highlight places where bundles of magnetic fields lines are concentrated. However, small areas with a lot of field lines will appear black, usually near sunspots and active regions.</p>
 <ul>
 <li><strong>Where:</strong> Transition region and upper photosphere</li>
@@ -1525,6 +1532,7 @@
 <li><strong>Characteristic temperatures:</strong> 6,000 K (11,000 F), and 100,000 K (180,000 F)</li>
 </ul>
 <h3 id="1700-a">1700 Å</h3>
+<p><img alt="aia_1700" src="../../assets/aia_1700.webp" /></p>
 <p>This channel (as well as AIA 1600) often shows a web-like pattern of bright areas that highlight places where bundles of magnetic fields lines are concentrated. However, small areas with a lot of field lines will appear black, usually near sunspots and active regions.</p>
 <ul>
 <li><strong>Where:</strong> Temperature minimum and photosphere</li>
@@ -1532,19 +1540,26 @@
 <li><strong>Primary ions seen:</strong> Continuum</li>
 <li><strong>Characteristic temperature:</strong> 6,000 K (11,000 F)</li>
 </ul>
+<hr />
 <h2 id="helioseismic-and-magnetic-imager">Helioseismic and Magnetic Imager</h2>
 <h3 id="magnetogram">Magnetogram</h3>
+<p><img alt="hmib" src="../../assets/HMIB.webp" /></p>
 <p>Magnetograms show maps of the magnetic field on the Sun’s surface. The HMI instrument uses the Zeeman effect to measure the intensity of the magnetic field component along the line of sight by making use of the circularly polarized spectral line. The color chart of the magnetic field along the line of sight is designed to visually show both high and low values. Intensities less than 24G are shades of gray. Positive values of the field are green and blue. Negative values are yellow and red. Regions with a weak field appear mainly in yellow or green. Progressively positive values range from dark green to light green (at 236 G). Negative values range from light yellow to orange (at -236G). There is a strong discontinuity in the coloration at 236G. Positive or negative sunspots and other regions with an intense field appear blue or red with dark umbrae. There are 254 colors arranged symmetrically around 0. The 127 positive values include 2 grays tending toward dark, 13 greens toward light, and 110 blues toward dark. The 127 negative values include 2 grays tending toward light, 18 yellows toward dark, and 107 reds toward dark. Nominally, each color indicates a range of about 11.81 G, and the coloration altogether spans the range between -1500 G and 1500 G</p>
 <h3 id="intensitygram">Intensitygram</h3>
+<p><img alt="hmii" src="../../assets/HMII.webp" /></p>
 <p>HMI samples the Fe I absorption line at 6173.3 Å at six points, assuming that the "pure" profile of the Fe I line is Gaussian and the transmission profiles are delta functions, the first and second Fourier coefficients of the Fe I line profile can be calculated, and Doppler velocity estimation can be performed. An estimate of the intensity in the continuum is obtained by "reconstructing" the solar line from the Doppler offset and the thickness and depth of the line.</p>
 <h3 id="dopplergram">Dopplergram</h3>
+<p><img alt="hmid" src="../../assets/HMID.webp" /></p>
 <p>HMI camera 2 takes 72 images to construct a single Doppler diagram. Six images are taken at six positions across the spectral line at 6173.3 Å. Each image is taken in two polarization states, circularly polarized to the right (RCP or Stokes I-V) and circularly polarized to the left (LCP or Stokes I+V). Assuming that the absorption line is Gaussian and the transmission profiles of the HMI filter are delta functions, Fourier coefficients are calculated and then used to estimate the magnetic field B along the line of sight.</p>
+<hr />
 <h2 id="large-angle-and-spectrometric-coronagraph">Large Angle and Spectrometric Coronagraph</h2>
 <h3 id="lasco-c1-not-available">LASCO C1 (NOT AVAILABLE)</h3>
 <p>A Fabry–Pérot interferometer coronagraph imaging from 1.1 to 3 solar radii, non-functional since the 24 June 1998 SOHO Mission Interruption</p>
 <h3 id="lasco-c2-orange">LASCO C2 (orange)</h3>
-<p>A white light coronagraph imaging from 1.5 to 6 solar radii</p>
+<p><img alt="lasco_c2" src="../../assets/lasco_c2.webp" /></p>
+<p>A white light coronagraph imaging from 1.5 to 6 solar radii. The LASCO camera is equipped with an occulting disk that blocks out the Sun to be able to study the faint details in the corona.</p>
 <h3 id="lasco-c3-blue">LASCO C3 (blue)</h3>
+<p><img alt="lasco_c3" src="../../assets/lasco_c3.webp" /></p>
 <p>A white light coronagraph imaging from 3.7 to 30 solar radii</p>