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<section id="w-uma-wuma">
<h1>W Uma (wuma)<a class="headerlink" href="#w-uma-wuma" title="Link to this heading">¶</a></h1>
<p>W UMa stars are main-sequence overcontact binaries. In overcontact binaries both stars are too large for their Roche lobe share a common envelope and can exchange mass and energy. The mass-ratio of the system ranges from 1 to 10 in extreme cases. Components can have different raddii and surface brightness with temperatures ranging from 4000 to 9000K.</p>
<section id="classification-and-numbers">
<h2>Classification and numbers<a class="headerlink" href="#classification-and-numbers" title="Link to this heading">¶</a></h2>
<ul class="simple">
<li><p>Supertypes</p>
<ul>
<li><p>variable</p></li>
<li><p>periodic</p></li>
<li><p>binary</p></li>
<li><p>eclipsing</p></li>
</ul>
</li>
<li><p>Occurrence rate: very common, about 10<sup>5</sup> expected in ZTF data</p></li>
</ul>
</section>
<section id="ztf-light-curves">
<h2>ZTF light curves<a class="headerlink" href="#ztf-light-curves" title="Link to this heading">¶</a></h2>
<p><img alt="ZTF wuma" src="_images/w_uma.png" /></p>
<section id="description">
<h3>Description<a class="headerlink" href="#description" title="Link to this heading">¶</a></h3>
<p>Contact binary lightcurves show a distinctive shape that shows two eclipses which do smoothly transition over. Eclipses can have a flat bottom. The eclipse depth is often identical, but can be show slightly different depths. In rare cases there can be differences in the maxima of the lightcurves (e.g. due to starspots).</p>
</section>
<section id="light-curve-characteristics">
<h3>Light curve characteristics<a class="headerlink" href="#light-curve-characteristics" title="Link to this heading">¶</a></h3>
<ul class="simple">
<li><p>periodic variable</p></li>
<li><p>period range: 0.22-0.8 days</p></li>
<li><p>amplitude: up to 0.75 mag</p></li>
<li><p>light curve shape: EW, two ‘V’-shaped eclipses with smooth transitions</p></li>
<li><p>eclipses often equal depth, within 0.1mag</p></li>
</ul>
</section>
<section id="other-characteristics-and-selection-methods">
<h3>Other characteristics and selection methods<a class="headerlink" href="#other-characteristics-and-selection-methods" title="Link to this heading">¶</a></h3>
<ul class="simple">
<li><p>g-r = -0.1 – 1.0. Short period systems are typically redder.</p></li>
<li><p>absolute magnitudes are similar to main-sequence stars</p></li>
</ul>
<p><img alt="HR diagram of W Uma" src="_images/hr__w_uma.png" /></p>
<p><img alt="RA/Dec diagram of W Uma" src="_images/radec__w_uma.png" /></p>
</section>
</section>
<section id="references-and-further-reading">
<h2>References and further reading:<a class="headerlink" href="#references-and-further-reading" title="Link to this heading">¶</a></h2>
<ul class="simple">
<li><p>Sterken & Jasschek: Light curves of variable stars</p></li>
<li><p>Marsh et al, MNRAS 465, 4678–4689, 2017</p></li>
</ul>
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