Solar chameleons: Novel channels

We revisit the flux of chameleons (light scalar particles which could play a role in the dark energy phenomenon) produced in the interior of the Sun. Our novel analysis incorporates various important details and new processes that have previously been overlooked, including the impact of the bulk magnetic field profile, as well as Primakoff production of chameleons in the electric fields of electrons and ions. In this paper we consider only the contributions of transverse photons. The production of chameleons from longitudinal electromagnetic excitations will be presented in a dedicated follow-up work. Demanding that the total flux of chameleons does not exceed 3% of the solar luminosity leads to the stringent upper limit on the chameleon-photon conformal coupling <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msub><a:mi>β</a:mi><a:mi>γ</a:mi></a:msub><a:mo>≲</a:mo><a:msup><a:mn>10</a:mn><a:mn>10</a:mn></a:msup></a:math>, assuming that the height of the chameleon potential is set to the dark energy scale <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mi mathvariant="normal">Λ</c:mi><c:mo>=</c:mo><c:mn>2.4</c:mn><c:mtext> </c:mtext><c:mtext> </c:mtext><c:mi>meV</c:mi></c:math>, and independently of other couplings to matter. Although this bound is tighter than current upper limits on <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:msub><f:mi>β</f:mi><f:mi>γ</f:mi></f:msub></f:math> from the CAST helioscope, these limits will have to be reassessed in terms of the updated solar chameleon flux we have computed. We argue that solar chameleons, potentially detectable in next-generation helioscopes such as IAXO, can be used to probe a region of chameleon parameter space that has yet to be covered. Published by the American Physical Society 2024