Can QCD axion stars explain Subaru HSC microlensing?
| dc.contributor.author | Schiappacasse, Enrico D. | |
| dc.contributor.author | Yanagida, Tsutomu T. | |
| dc.date.accessioned | 2022-01-11T07:29:34Z | |
| dc.date.available | 2022-01-11T07:29:34Z | |
| dc.date.issued | 2021 | |
| dc.identifier.citation | Schiappacasse, E. D., & Yanagida, T. T. (2021). Can QCD axion stars explain Subaru HSC microlensing?. <i>Physical Review D</i>, <i>104</i>(10), Article 103020. <a href="https://doi.org/10.1103/PhysRevD.104.103020" target="_blank">https://doi.org/10.1103/PhysRevD.104.103020</a> | |
| dc.identifier.other | CONVID_103594782 | |
| dc.identifier.uri | https://jyx.jyu.fi/handle/123456789/79273 | |
| dc.description.abstract | A non-negligible fraction of the QCD axion dark matter may form gravitationally bound Bose Einstein condensates, which are commonly known as axion stars or axion clumps. Such astrophysical objects have been recently proposed as the cause for the single candidate event reported by Subaru Hyper Suprime-Cam (HSC) microlensing search in the Andromeda galaxy. Depending on the breaking scale of the Peccei-Quinn symmetry and the details of the dark matter scenario, QCD axion clumps may form via gravitational condensation during radiation domination, in the dense core of axion miniclusters, or within axion minihalos around primordial black holes. We analyze all these scenarios and conclude that the microlensing candidate detected by the Subaru HSC survey is likely not caused by QCD axion stars. | en |
| dc.format.mimetype | application/pdf | |
| dc.language.iso | eng | |
| dc.publisher | American Physical Society (APS) | |
| dc.relation.ispartofseries | Physical Review D | |
| dc.rights | CC BY 4.0 | |
| dc.title | Can QCD axion stars explain Subaru HSC microlensing? | |
| dc.type | article | |
| dc.identifier.urn | URN:NBN:fi:jyu-202201111051 | |
| dc.contributor.laitos | Fysiikan laitos | fi |
| dc.contributor.laitos | Department of Physics | en |
| dc.type.uri | http://purl.org/eprint/type/JournalArticle | |
| dc.type.coar | http://purl.org/coar/resource_type/c_2df8fbb1 | |
| dc.description.reviewstatus | peerReviewed | |
| dc.relation.issn | 2470-0010 | |
| dc.relation.numberinseries | 10 | |
| dc.relation.volume | 104 | |
| dc.type.version | publishedVersion | |
| dc.rights.copyright | © 2021 the Authors | |
| dc.rights.accesslevel | openAccess | fi |
| dc.relation.grantnumber | 318319 | |
| dc.subject.yso | kosmologia | |
| dc.subject.yso | hiukkasfysiikka | |
| dc.subject.yso | kvanttiväridynamiikka | |
| dc.subject.yso | astrofysiikka | |
| dc.subject.yso | pimeä aine | |
| dc.format.content | fulltext | |
| jyx.subject.uri | http://www.yso.fi/onto/yso/p7160 | |
| jyx.subject.uri | http://www.yso.fi/onto/yso/p15576 | |
| jyx.subject.uri | http://www.yso.fi/onto/yso/p39318 | |
| jyx.subject.uri | http://www.yso.fi/onto/yso/p20188 | |
| jyx.subject.uri | http://www.yso.fi/onto/yso/p14101 | |
| dc.rights.url | https://creativecommons.org/licenses/by/4.0/ | |
| dc.relation.doi | 10.1103/PhysRevD.104.103020 | |
| dc.relation.funder | Research Council of Finland | en |
| dc.relation.funder | Suomen Akatemia | fi |
| jyx.fundingprogram | Academy Project, AoF | en |
| jyx.fundingprogram | Akatemiahanke, SA | fi |
| jyx.fundinginformation | This work was supported by the Academy of Finland Grant No. 318319. T. T. Y. is supported in part by the China Grant for Talent Scientific Start-Up Project and the JSPS Grant-in-Aid for Scientific Research Grants No. 16H02176, No. 17H02878, and No. 19H05810 and by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. | |
| dc.type.okm | A1 |
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