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            <idno type="halRefHtml">&lt;i&gt;Comptes Rendus. Physique&lt;/i&gt;, 2015, 16, pp.661-673. &lt;a target="_blank" href="https://dx.doi.org/10.1016/j.crhy.2015.08.014"&gt;&amp;#x27E8;10.1016/j.crhy.2015.08.014&amp;#x27E9;&lt;/a&gt;</idno>
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                <term xml:lang="en">supernova</term>
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                <term xml:lang="en">Radiation mechanisms: non-thermal</term>
                <term xml:lang="en">Binaries: general</term>
                <term xml:lang="en">Gamma-rays: stars</term>
                <term xml:lang="en">Accélération de particules</term>
                <term xml:lang="en">Mécanismes de rayonnement non thermiques</term>
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                <term xml:lang="en">accretion</term>
                <term xml:lang="en">Étoiles binaires</term>
                <term xml:lang="en">black hole</term>
                <term xml:lang="en">white dwarf</term>
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                <term xml:lang="en">energy: high</term>
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              <p>More than a dozen binary systems are now established as sources of variable, high-energy (HE, 0.1–100 GeV ) gamma rays. Five are also established sources of very-high-energy (VHE, ⩾100 GeV ) gamma rays. The mechanisms behind gamma-ray emission in binaries are very diverse. My current understanding is that they divide up into four types of systems: gamma-ray binaries, powered by pulsar rotation; microquasars, powered by accretion onto a black hole or neutron star; novae, powered by thermonuclear runaway on a white dwarf; colliding wind binaries, powered by stellar winds from massive stars. Some of these types had long been suspected to emit gamma rays (microquasars), others have taken the community by surprise (novae). My purpose here is to provide a brief review of the current status of gamma-ray emission from binaries, in the context of related objects where similar mechanisms are at work (pulsar wind nebulae, active galactic nuclei, supernova remnants).</p>
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