Solar constraints on hidden photons re-visited

By J. Redondo, G. Raffelt. 2013

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We re-examine solar emission of hidden photons γ' (mass m) caused by kinetic γ–γ' mixing. We calculate the emission rate with thermal field theory methods and with a kinetic equation that includes γ–γ' ''flavor oscillations'' and γ absorption and emission by the thermal medium. In the resonant case both methods yield identical emission rates which, in the longitudinal channel, are enhanced by a factor ωP2/m2 (plasma frequency ωP) in agreement with An, Pospelov and Pradler (2013). The Sun must not emit more energy in a ``dark channel'' than allowed by solar neutrino measurements, i.e., not more than 10% of its photon luminosity. Together with the revised emission rate, this conservative requirement implies χ < 4 × 10−12(eV/m) for the kinetic mixing parameter. This is the most restrictive stellar limit below m ~ 3eV, whereas for larger masses the transverse channel dominates together with limits from other stars. A recent analysis of XENON10 data marginally improves the solar limit, leaving open the opportunity to detect solar hidden photons with future large-scale dark matter experiments. Detecting low-mass hidden photons with the ALPS-II photon-regeneration experiment also remains possible.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4b8ad6ee81bb20b5911f2f111c1bb43aada44827

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In Nuclear and High Energy Physics

Citations in the corpus

Any Light Particle Search II -- Technical Design Report (2013, background): “s the reach of ALPS-IIb, with and without gas, respectively. For the parameter choices with gas, see main text. The black dashed lines enclose the HP Dark Radiation hint [64], however recent analyses [68, 69] exclude the parameter range above the line labeled “Longitudinal, thus disfavoring this int”
Solar axion flux from the axion-electron coupling (2013, background): “Recent papers also showed that in some cases the emission of longitudinally polarized modes can dominate [94, 115].”
Cool WISPs for stellar cooling excesses (2015, background): “In the case of low mass, the emission rate of longitudinal HPs is [35]”
Stellar cooling bounds on new light particles: plasma mixing effects (2016, background): “With modern solar models, novel forms of energy loss can be constrained down to around 10% of the measured solar luminosity [7, 15] (global modelling using specific energy loss profiles can improve this limit to the few percent level [16]).”
Constraining light dark matter with diffuse X-ray and gamma-ray observations (2013, background): “Assuming mγd ' mγ̃d , additional constraints exist from beam-dump [82, 83], fixedtarget [84, 85], and colliding-beam experiments [86]; precision measurements [87]; stars [88, 89]; and from the intergalactic diffuse photon background (IDPB).”
New axion and hidden photon constraints from a solar data global fit (2015, methodology): “We only take into account the dominant process of resonant emission of longitudinal hidden photons (details in [9, 54]) for which the energy loss rate is given by”
Dark matter models and direct detection (2019, background): “[92, 89, 91, 119, 90] for the Sun, red giants, horizontal branch stars, and SN1987a.”