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Electroweak Cogenesis

Cheung, Clifford and Zhang, Yue (2013) Electroweak Cogenesis. Journal of High Energy Physics, 2013 (9). Art. No. 002. ISSN 1126-6708.

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We propose a simple renormalizable model of baryogenesis and asymmetric dark matter generation at the electroweak phase transition. Our setup utilizes the two Higgs doublet model plus two complex gauge singlets, the lighter of which is stable dark matter. The dark matter is charged under a global symmetry that is broken in the early universe but restored during the electroweak phase transition. Because the ratio of baryon and dark matter asymmetries is controlled by model parameters, the dark matter need not be light. Thus, new force carriers are unnecessary and the symmetric dark matter abundance can be eliminated via Higgs portal interactions alone. Our model places a rough upper bound on the dark matter mass, and has implications for direct detection experiments and particle colliders.

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Additional Information:© 2013 SISSA. Published for SISSA by Springer. Received: June 27, 2013; Revised: August 10, 2013; Accepted: August 12, 2013; Published: September 2, 2013. We thank Pavel Fileviez-Perez, Xiangdong Ji, Rabi Mohapatra, Michael Ramsey-Musolf, Shmuel Nussinov, Goran Senjanovic, Jing Shu, Mark Wise, and Kathryn Zurek for valuable comments and discussions. This work is supported by the Gordon and Betty Moore Foundation through Grant #776 to the Caltech Moore Center for Theoretical Cosmology and Physics, and by the DOE Grant DE-FG02-92ER40701.
Group:Caltech Theory, Moore Center for Theoretical Cosmology and Physics
Funding AgencyGrant Number
Gordon and Betty Moore Foundation776
Caltech Moore Center for Theoretical Cosmology and PhysicsUNSPECIFIED
Department of Energy (DOE)DE-FG02-92ER40701
Issue or Number:9
Record Number:CaltechAUTHORS:20130708-081604840
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39236
Deposited By: Tony Diaz
Deposited On:12 Aug 2013 21:30
Last Modified:03 Oct 2019 05:05

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