[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"detail-sidebar-cat-0-en-105":3,"doc-seo-146141-105":59,"doc-detail-146141-en":130},{"code":4,"msg":5,"data":6},0,"success",[7,13,18,23,28,33,38,43,48,51,55],{"id":8,"doc_module":4,"doc_module_name":9,"category_name":10,"show_sort_weight":11,"slug":12},1,"Document","Story & Novel",90,"story-novel",{"id":14,"doc_module":4,"doc_module_name":9,"category_name":15,"show_sort_weight":16,"slug":17},2,"Literature",80,"literature",{"id":19,"doc_module":4,"doc_module_name":9,"category_name":20,"show_sort_weight":21,"slug":22},4,"Exam",70,"exam",{"id":24,"doc_module":4,"doc_module_name":9,"category_name":25,"show_sort_weight":26,"slug":27},5,"Comic",60,"comic",{"id":29,"doc_module":4,"doc_module_name":9,"category_name":30,"show_sort_weight":31,"slug":32},6,"Technology",50,"technology",{"id":34,"doc_module":4,"doc_module_name":9,"category_name":35,"show_sort_weight":36,"slug":37},7,"Healthcare",40,"healthcare",{"id":39,"doc_module":4,"doc_module_name":9,"category_name":40,"show_sort_weight":41,"slug":42},8,"Research & Report",30,"research-report",{"id":44,"doc_module":4,"doc_module_name":9,"category_name":45,"show_sort_weight":46,"slug":47},9,"Religion & Spirituality",20,"religion-spirituality",{"id":46,"doc_module":4,"doc_module_name":9,"category_name":49,"show_sort_weight":46,"slug":50},"World Cup","world-cup",{"id":52,"doc_module":4,"doc_module_name":9,"category_name":53,"show_sort_weight":52,"slug":54},10,"Lifestyle","lifestyle",{"id":56,"doc_module":4,"doc_module_name":9,"category_name":57,"show_sort_weight":24,"slug":58},19,"General","general",{"code":4,"msg":60,"data":61},"ok",{"site_id":62,"language":63,"slug":64,"title":65,"keywords":66,"description":67,"schema_data":68,"social_meta":123,"head_meta":125,"extra_data":127,"updated_unix":129},105,"en","primordial-black-holes-from-bubble-collisions-during-a-first-order-phase-transition","Primordial black holes from bubble collisions during a first-order phase transition","","Study evaluates whether primordial black holes can be produced by bubble collisions occurring during a first-order phase transition in the early Universe. Typical colliding bubbles are found insufficient, while PBH formation requires a macroscopically thick fluid shell and bubble birth far earlier than the usual nucleation time. Exponential sensitivity to bubble-growth duration and the spacetime metric evolution near the transition end creates major uncertainties. Introducing simulation-extractable parameters in an Abelian Higgs benchmark, the work estimates potentially significant PBH abundance, predicts an approximately monochromatic mass spectrum, and identifies regions matching full dark-matter content or causing overclosure.",{"@graph":69,"@context":122},[70,84,105],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":40,"@type":76,"position":81},"https://docshare.wps.com/document/research-report/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/primordial-black-holes-from-bubble-collisions-during-a-first-order-phase-transition/146141/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/primordial-black-holes-from-bubble-collisions-during-a-first-order-phase-transition/146141.png","ImageObject",300,407,{"name":92,"@type":93},"วิน","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-18","2026-08-26",true,{"@type":102,"interactionType":103,"userInteractionCount":44},"InteractionCounter",{"@type":104},"ViewAction",{"@type":106,"mainEntity":107},"FAQPage",[108,114,118],{"name":109,"@type":110,"acceptedAnswer":111},"What conditions are required for bubble collisions to produce primordial black holes?","Question",{"text":112,"@type":113},"PBH production requires a macroscopically thick fluid shell and bubbles that form much earlier than the typical nucleation time. These conditions make the collision outcome dense enough to trigger black-hole formation.","Answer",{"name":115,"@type":110,"acceptedAnswer":116},"Why are the predictions highly uncertain?",{"text":117,"@type":113},"Uncertainty is dominated by the exponential sensitivity of the PBH-relevant bubble-growth duration. This duration depends on collision details and on how the spacetime metric evolves toward the end of the phase transition.",{"name":119,"@type":110,"acceptedAnswer":120},"How does the paper estimate the PBH abundance and mass spectrum?",{"text":121,"@type":113},"It introduces parameters intended to be obtained from future numerical simulations, evaluates PBH abundance in an Abelian Higgs benchmark model, and predicts an approximately monochromatic PBH mass spectrum. It then identifies parameter-space regions where PBHs could make up all dark matter or overclose the Universe.","https://schema.org",{"og:url":83,"og:type":124,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":126,"canonical":83},"index,follow",{"doc_id":128,"site_id":62},146141,1787737081,{"code":4,"msg":5,"data":131},{"doc_id":128,"user_id":132,"nickname":92,"user_avatar":133,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":134,"file_id":135,"file_url":136,"file_type":137,"file_size":138,"view_count":44,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":139,"language":140,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":141,"faqs":142,"seo_title":143,"seo_description":67,"update_tm":129,"read_time":144},2336475104736,"https://ap-avatar.wpscdn.com/avatar/22000c4c5e0e5b17e70?x-image-process=image/resize,m_fixed,w_180,h_180&k=1786591360781797222","Primordial black holes from bubble collisions during a first-order  \nphase transition  \nTae Hyun Jung1,2,* and Takemichi Okui1,3,†  \n1Department of Physics, Florida State University, Tallahassee, Florida 32306, USA 2Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34126, Korea 3Theory Center, High Energy Accelerator Research Organization (KEK), Tsukuba 305-0801, Japan  \n (Received 5 January 2024; accepted 18 November 2024; published 11 December 2024)  \nWe study the possibility of production of primordial black holes (PBHs) from bubble collisions during a first-order phase transition. While typical colliding bubbles are small and irrelevant for PBH production, we find that those that can produce PBHs must have a macroscopically thick fluid shell and have been born much before the typical nucleation time. Particularly large uncertainties arise from an exponential sensitivity of the nucleation rate on the required duration ofbubble growth which depends on the details ofthe collisionsand the evolution of the spacetime metric toward the end of the phase transition. We introduce a few parameters to be obtained from future numerical simulation to represent those unknowns, and estimate the PBH abundance inan Abelian Higgs benchmark model and show that it can be significant. We predict an approximately monochromatic PBH mass spectrum, and find regions in the parameter space where the PBHs can constitute entire dark matter or even overclose the Universe. Our result thus shows that models with a first-order phase transition can be constrained by overabundant PBHs or null results of other PBH searches.  \nDOI: 10.1103/PhysRevD.110.115014  \nI. INTRODUCTION  \nFirst-order phase transition in the early Universe is a well motivated field of study both theoretically and experimentally. Since a generic quantum field theory has multiple phases, it is natural to expect the early Universe to undergo various stages of phase transitions, some of which may well be at first order. A first-order phase transition necessarily leads to nucleation of true-vacuum bubbles and their subsequent expansions, and they must eventually collide to fill the Universe with the true vacuum. This can result in many cosmological implications such as dark matter [1–6] and baryogenesis [7–12] . Since gravitational wave production from bubble collisions during a first-order phase transition is generically expected [13–20], these ideas may be testable by near-future gravitational wave experiments [21–60](see Refs. [19,20] for reviews) .  \nSince every first-order phase transition must end with bubble collisions, it is important to seek other significant outcomes of bubble collisions. In particular, given many PBH bounds and searches [61–90], we would like to know  \n*Contact author: [thjung0720@gmail.com](thjung0720@gmail.com)  \n†Contact author: [tokui@fsu.edu](tokui@fsu.edu)  \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.  \nwhether or not bubble collisions can produce an observationally significant abundance of PBHs, a subject initiated by [91] . One might be tempted to disregard this possibility and favor other PBH formation mechanisms [92–96][97,98][99–102][103–110] as it seems highly improbable for a large amount of energy to be compressed into a small volume by bubble collisions. In fact, the number of PBHs per Hubble volume at the time of their formation must be extremely small  \nnPBH3H ∼ 10−15fPBH 􀀁~~ ~~10−M1P1BMH⊙~~ ~~ 􀀃􀀁~~ ~~105GT~~ ~~􀀁eV􀀃 3 􀀁~~ ~~10g􀀁0􀀃 12 ; ð1Þ  \nwhere fPBH ≡ ρPBH =ρDM , and H, T􀀁 and g􀀁 are respectively the Hubble rate at the formation time, the temperature and radiation degrees of freedom at the reheating after the phase transition. Here, we have assumed that the reheating is inst","cbCaibpXBZst6vSg","https://ap.wps.com/l/cbCaibpXBZst6vSg","pdf",2533354,18,"English","# I. INTRODUCTION\n## Bubble collisions and PBH motivation\n# II. THE HOOP CONJECTURE AND ITS IMPLICATIONS\n## A. The hoop conjecture\n## B. Necessity for large bubbles with a thick fluid shell","[{\"question\":\"What conditions are required for bubble collisions to produce primordial black holes?\",\"answer\":\"PBH production requires a macroscopically thick fluid shell and bubbles that form much earlier than the typical nucleation time. These conditions make the collision outcome dense enough to trigger black-hole formation.\"},{\"question\":\"Why are the predictions highly uncertain?\",\"answer\":\"Uncertainty is dominated by the exponential sensitivity of the PBH-relevant bubble-growth duration. This duration depends on collision details and on how the spacetime metric evolves toward the end of the phase transition.\"},{\"question\":\"How does the paper estimate the PBH abundance and mass spectrum?\",\"answer\":\"It introduces parameters intended to be obtained from future numerical simulations, evaluates PBH abundance in an Abelian Higgs benchmark model, and predicts an approximately monochromatic PBH mass spectrum. It then identifies parameter-space regions where PBHs could make up all dark matter or overclose the Universe.\"}]","Primordial black holes from bubble collisions during a first-order phase transition | PDF",45]