[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"doc-detail-43232-en":3,"doc-seo-43232-105":30,"detail-sidebar-cat-0-en-105":95},{"code":4,"msg":5,"data":6},0,"success",{"doc_id":7,"user_id":8,"nickname":9,"user_avatar":10,"doc_module":4,"category_id":11,"category_name":12,"doc_title":13,"doc_description":14,"doc_content":15,"file_id":16,"file_url":17,"file_type":18,"file_size":19,"view_count":20,"is_deleted":4,"is_public":21,"is_downloadable":21,"audit_status":21,"page_count":22,"language":23,"language_code":24,"site_id":25,"html_lang":24,"table_of_contents":26,"faqs":27,"seo_title":13,"seo_description":14,"update_tm":28,"read_time":29},43232,7971461740909,"Levi","https://ap-avatar.wpscdn.com/davatar_155a257f0dc6eb9ab79c44ca47cae57d",8,"Research & Report","Direct detection of dark energy: The XENON1T excess and future prospects","We investigate how upcoming and current terrestrial dark matter direct detection experiments could probe dark energy through new light degrees of freedom. If dark energy couples to matter and photons, solar dark-energy quanta stream to Earth and interact in detector chambers. Screening suppresses production in stellar cores, while photon coupling enables production in the Sun’s tachocline via a Primakoff-like mechanism. The XENON1T electron-recoil excess can be fit by chameleon-screened dark energy at 2.0σ and tested by future detectors.","Direct detection of dark energy: The XENON1T excess and future prospects  \nSunny Vagnozzi, 1,2,*,¶ Luca Visinelli,3,4,5,†,¶ Philippe Brax,6,‡ Anne-Christine Davis,7,1,§ and Jeremy Sakstein8, ∥ 1Kavli Institute for Cosmology (KICC), University of Cambridge, Madingley Road,  \nCambridge CB3 0HA, United Kingdom  \n2Institute of Astronomy (IoA), University of Cambridge, Madingley Road,  \nCambridge CB3 0HA, United Kingdom  \n3Istituto Nazionale di Fisica Nucleare (INFN), Laboratori Nazionali di Frascati,  \nC.P. 13, I-100044 Frascati, Italy  \n4Tsung-Dao Lee Institute (TDLI), Shanghai Jiao Tong University, 200240 Shanghai, China  \n5Gravitation Astroparticle Physics Amsterdam (GRAPPA), University of Amsterdam,  \nScience Park 904, 1098 XH Amsterdam, Netherlands  \n6Institute de Physique Theórique (IPhT), Universite´ Paris-Saclay, CNRS, CEA, F-91191,  \nGif-sur-Yvette Cedex, France  \n7Department of Applied Mathematics and Theoretical Physics (DAMTP),  \nCenter for Mathematical Sciences, University of Cambridge, CB3 0WA, United Kingdom  \n8Department of Physics & Astronomy, University of Hawai ’i, Watanabe Hall,  \n2505 Correa Road, Honolulu, Hawaii, 96822, USA  \n (Received 7 April 2021; accepted 20 August 2021; published 15 September 2021)  \nWe explore the prospects for direct detection of dark energy by current and upcoming terrestrial dark matter direct detection experiments. If dark energy is driven by a new light degree of freedom coupled to matter and photons then dark energy quanta are predicted to be produced in the Sun. These quanta free-stream toward Earth where they can interact with Standard Model particles in the detection chambers of direct detection experiments, presenting the possibility that these experiments could be used to test dark energy. Screening mechanisms, which suppress fifth forces associated with new light particles, and are a necessary feature of many dark energy models, prevent production processes from occurring in the core of the Sun, and similarly, in the cores of red giant, horizontal branch, and white dwarf stars. Instead, the coupling of dark energy to photons leads to production in the strong magnetic field of the solar tachocline via a mechanism analogous to the Primakoff process. This then allows for detectable signals on Earth while evading the strong constraints that would typically result from stellar probes of new light particles. As an example, we examine whether the electron recoil excess recently reported by the XENON1T collaboration can be explained by chameleon-screened dark energy, and find that such a model is preferred over the background-only hypothesis at the 2.0σ level, in a large range of parameter space not excluded by stellar (or other) probes. This raises the tantalizing possibility that XENON1T may have achieved the first direct detection of dark energy. Finally, we study the prospects for confirming this scenario using planned future detectors such as XENONnT, PandaX-4T, and LUX-ZEPLIN.  \nDOI: 10.1103/PhysRevD.104.063023  \n*[sunny.vagnozzi@ast.cam.ac.uk](sunny.vagnozzi@ast.cam.ac.uk)[ ](sunny.vagnozzi@ast.cam.ac.uk)†[luca.visinelli@sjtu.edu.cn](luca.visinelli@sjtu.edu.cn)[ ](luca.visinelli@sjtu.edu.cn)‡[philippe.brax@cea.fr](philippe.brax@cea.fr)  \n§[ad107@cam.ac.uk](ad107@cam.ac.uk)[ ](ad107@cam.ac.uk)∥[sakstein@hawaii.edu](sakstein@hawaii.edu)  \n¶These authors contributed equally to this work.  \nPublished by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3.  \nI. INTRODUCTION  \nMore than two decades after the discovery that the expansion of the Universe is accelerating [1,2], the nature of the dark energy (D) component driving this phenome  \nnon and making up 70% of the energy budget of the Universe remains a mystery [3–7] . What is perhaps the simplest theoretical DE cand","cbCaidQnATv1MM2J","https://ap.wps.com/l/cbCaidQnATv1MM2J","pdf",1022805,2,1,24,"English","en",105,"# Introduction\n## Dark energy and the cosmological constant problem\n## Modified gravity and screening mechanisms\n## Prospects for direct detection\n## XENON1T explanation and statistical preference\n## Future experimental confirmation","[{\"question\":\"How can dark energy be tested using dark matter direct detection experiments?\",\"answer\":\"The work proposes that dark energy may be realized by new light degrees of freedom produced in the Sun, then reaching Earth and interacting within the detection chambers of terrestrial experiments.\"},{\"question\":\"Why doesn’t dark-energy production occur in the Sun’s core in these models?\",\"answer\":\"Screening mechanisms suppress the associated fifth-force interactions, preventing the production channels from operating efficiently in dense stellar interiors such as the solar core.\"},{\"question\":\"What mechanism enables detectable production when dark energy couples to photons?\",\"answer\":\"Photon coupling leads to production in the solar tachocline through a Primakoff-like process driven by the Sun’s strong magnetic field.\"},{\"question\":\"What do the authors conclude about the XENON1T electron-recoil excess and future verification?\",\"answer\":\"A chameleon-screened dark energy scenario is preferred over a background-only explanation at the 2.0σ level over substantial parameter space, and the scenario can be tested using planned detectors such as XENONnT, PandaX-4T, and LUX-ZEPLIN.\"}]",1783378883,60,{"code":4,"msg":31,"data":32},"ok",{"site_id":25,"language":24,"slug":33,"title":13,"keywords":34,"description":14,"schema_data":35,"social_meta":90,"head_meta":92,"extra_data":94,"updated_unix":28},"direct-detection-of-dark-energy-the-xenon1t-excess-and-future-prospects","",{"@graph":36,"@context":89},[37,53,68],{"@type":38,"itemListElement":39},"BreadcrumbList",[40,44,47,50],{"item":41,"name":42,"@type":43,"position":21},"https://docshare.wps.com","Home","ListItem",{"item":45,"name":46,"@type":43,"position":20},"https://docshare.wps.com/document/","Document",{"item":48,"name":12,"@type":43,"position":49},"https://docshare.wps.com/document/research-report/",3,{"item":51,"name":13,"@type":43,"position":52},"https://docshare.wps.com/document/direct-detection-of-dark-energy-the-xenon1t-excess-and-future-prospects/43232/",4,{"url":51,"name":13,"@type":54,"author":55,"headline":13,"publisher":57,"fileFormat":60,"inLanguage":24,"description":14,"dateModified":61,"datePublished":62,"encodingFormat":60,"isAccessibleForFree":63,"interactionStatistic":64},"DigitalDocument",{"name":9,"@type":56},"Person",{"url":41,"name":58,"@type":59},"DocShare","Organization","application/pdf","2026-07-13","2026-07-06",true,{"@type":65,"interactionType":66,"userInteractionCount":20},"InteractionCounter",{"@type":67},"ViewAction",{"@type":69,"mainEntity":70},"FAQPage",[71,77,81,85],{"name":72,"@type":73,"acceptedAnswer":74},"How can dark energy be tested using dark matter direct detection experiments?","Question",{"text":75,"@type":76},"The work proposes that dark energy may be realized by new light degrees of freedom produced in the Sun, then reaching Earth and interacting within the detection chambers of terrestrial experiments.","Answer",{"name":78,"@type":73,"acceptedAnswer":79},"Why doesn’t dark-energy production occur in the Sun’s core in these models?",{"text":80,"@type":76},"Screening mechanisms suppress the associated fifth-force interactions, preventing the production channels from operating efficiently in dense stellar interiors such as the solar core.",{"name":82,"@type":73,"acceptedAnswer":83},"What mechanism enables detectable production when dark energy couples to photons?",{"text":84,"@type":76},"Photon coupling leads to production in the solar tachocline through a Primakoff-like process driven by the Sun’s strong magnetic field.",{"name":86,"@type":73,"acceptedAnswer":87},"What do the authors conclude about the XENON1T electron-recoil excess and future verification?",{"text":88,"@type":76},"A chameleon-screened dark energy scenario is preferred over a background-only explanation at the 2.0σ level over substantial parameter space, and the scenario can be tested using planned detectors such as XENONnT, PandaX-4T, and LUX-ZEPLIN.","https://schema.org",{"og:url":51,"og:type":91,"og:title":13,"og:site_name":58,"og:description":14},"article",{"robots":93,"canonical":51},"index,follow",{"doc_id":7,"site_id":25},{"code":4,"msg":5,"data":96},[97,101,105,109,113,118,123,126,131,134,138],{"id":21,"doc_module":4,"doc_module_name":46,"category_name":98,"show_sort_weight":99,"slug":100},"Story & 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