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<section id="flaring-variables-fla">
<h1>Flaring variables (fla)<a class="headerlink" href="#flaring-variables-fla" title="Link to this heading">¶</a></h1>
<p>The phenomelogical classification of <code class="docutils literal notranslate"><span class="pre">flaring</span></code> is any kind of outbursting source, where a variable star (or binary system) dramatically increases in brightness for minutes to hours before returning to quiescence. Most flare stars are red dwarfs, while RS Canum Venaticorum variables (RS CVn) are also known to flare due to a companion star in the binary system. Other possible sources of flaring include dwarf novae, which arise from accretion disk activity in a cataclysmic variable star.</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>
</ul>
</li>
<li><p>Occurrence rate: very common, for a given red dwarf, flares 10³¹ - 10³² ergs occur about once per day, and flares 10³³ - 10³⁴ ergs occur about once per 10-100 days.</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 flaring_dwarfnova" src="_images/flaring_dwarfnova.png" /></p>
<p><img alt="ZTF flaring_mdwarf" src="_images/flaring_mdwarf.png" /></p>
<section id="description">
<h3>Description<a class="headerlink" href="#description" title="Link to this heading">¶</a></h3>
<p>Flaring stars are easy to recognise by their increase in brightness from quiescent levels, rapidly returning to that same level shortly thereafter.</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>variable</p></li>
<li><p>increase in brightness before returning to quiescence.</p></li>
<li><p>amplitude: at the bright end, flares can be many magnitudes, while at the dim end, flare detection is limited by survey photometric precision.</p></li>
</ul>
<p><img alt="HR diagram of Flaring" src="_images/hr__flaring.png" /></p>
<p><img alt="RA/Dec diagram of Flaring" src="_images/radec__flaring.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>Taichi Kato, WZ Sge-type dwarf novae, Publications of the Astronomical Society of Japan, Volume 67, Issue 6, December 2015, 108 <a class="reference external" href="https://arxiv.org/pdf/1507.07659.pdf">arxiv:1507.07659</a></p></li>
<li><p>Maximilian N. Günther et al 2020 AJ 159 60, <a class="reference external" href="https://arxiv.org/pdf/1901.00443.pdf">arxiv:1901.00443</a></p></li>
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