K. Barth, A. Belov, B. Beltran, H. Brauninger, J. M. Carmona, J. I. Collar, T. Dafni, M. Davenport, L. Di Lella, C. Eleftheriadis, J. Englhauser, G. Fanourakis, E. Ferrer Ribas, H. Fischer, J. Franz, P. Friedrich, J. Galan, J. A. Garcia, T. Geralis, I. Giomataris, S. Gninenko, H. Gomez, M. D. Hassinoff, F. H. Heinsius, D. H. H. Hoffmann, I. G. Irastorza, J. Jacoby, K. Jakovcic, D. Kang, K. Konigsmann, R. Kotthaus, K. Kousouris, M. Krcmar, M. Kuster, B. Lakic, A. Liolios, A. Ljubicic, G. Lutz, G. Luzon, D. W. Miller, T. Papaevangelou, M. J. Pivovaroff, G. Raffelt, J. Redondo, H. Riege, A. Rodriguez, J. Ruz, I. Savvidis, Y. Semertzidis, L. Stewart, K. Van Bibber, J. D. Vieira, J. A. Villar, J. K. Vogel, L. Walckiers, K. Zioutas
In non-hadronic axion models, which have a tree-level axion-electron interaction, the Sun produces a strong axion flux by bremsstrahlung, Compton scattering, and axio-recombination, the "BCA processes." Based on a new calculation of this flux, including for the first time axio-recombination, we derive limits on the axion-electron Yukawa coupling g_ae and axion-photon interaction strength g_ag using the CAST phase-I data (vacuum phase). For m_a < 10 meV/c2 we find g_ag x g_ae< 8.1 x 10^-23 GeV^-1 at 95% CL. We stress that a next-generation axion helioscope such as the proposed IAXO could push this sensitivity into a range beyond stellar energy-loss limits and test the hypothesis that white-dwarf cooling is dominated by axion emission.
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http://arxiv.org/abs/1302.6283
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