Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.015025
A. Drutskoy, E. Vasenin
We study potential contribution of the heavy right-handed neutrino exchange in the process e</a:mi>+</a:mo></a:msup>e</a:mi>−</a:mo></a:msup>→</a:mo>W</a:mi>+</a:mo></a:msup>W</a:mi>−</a:mo></a:msup></a:math>. This process is sensitive to heavy neutrinos with masses larger than <d:math xmlns:d="http://www.w3.org/1998/Math/MathML" display="inline"><d:msqrt><d:mi>s</d:mi></d:msqrt></d:math>. The Monte Carlo simulation of the studied process is performed assuming the seesaw type-I model, where heavy right-handed neutrinos (heavy neutral leptons, HNLs) are introduced in the leptonic sector. Within the Standard Model (SM), the process has a large cross section described by diagrams with <f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mi>s</f:mi></f:math>-channel <h:math xmlns:h="http://www.w3.org/1998/Math/MathML" display="inline"><h:mi>Z</h:mi><h:mo>/</h:mo><h:mi>γ</h:mi></h:math> exchange and <j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"><j:mi>t</j:mi></j:math>-channel active neutrino exchange. Respectively, the <l:math xmlns:l="http://www.w3.org/1998/Math/MathML" display="inline"><l:mi>t</l:mi></l:math>-channel right-handed neutrino exchange amplitude will interfere with these SM amplitudes. However, the angular distributions of the <n:math xmlns:n="http://www.w3.org/1998/Math/MathML" display="inline"><n:mi>W</n:mi></n:math> boson production and decay are different for the right-handed neutrino and SM amplitudes. That can be used to evaluate potential HNL contribution using the extended likelihood method. The simulation of the <p:math xmlns:p="http://www.w3.org/1998/Math/MathML" display="inline"><p:msup><p:mi>e</p:mi><p:mo>+</p:mo></p:msup><p:msup><p:mi>e</p:mi><p:mo>−</p:mo></p:msup><p:mo stretchy="false">→</p:mo><p:msup><p:mi>W</p:mi><p:mo>+</p:mo></p:msup><p:msup><p:mi>W</p:mi><p:mo>−</p:mo></p:msup></p:math> process is performed at the 1 TeV center-of-mass energy and polarization <s:math xmlns:s="http://www.w3.org/1998/Math/MathML" display="inline"><s:msub><s:mi mathvariant="script">P</s:mi><s:mrow><s:msup><s:mi>e</s:mi><s:mo>+</s:mo></s:msup><s:msup><s:mi>e</s:mi><s:mo>−</s:mo></s:msup></s:mrow></s:msub></s:math> of (20%, <v:math xmlns:v="http://www.w3.org/1998/Math/MathML" display="inline"><v:mo>−</v:mo><v:mn>80</v:mn><v:mo>%</v:mo></v:math>), which is a standard option for the future linear <x:math xmlns:x="http://www.w3.org/1998/Math/MathML" display="inline"><x:msup><x:mi>e</x:mi><x:mo>+</x:mo></x:msup><x:msup><x:mi>e</x:mi><x:mo>−</x:mo></x:msup></x:math> International Linear Collider. Both <z:math xmlns:z="http://www.w3.org/1998/Math/MathML" display="inline"><z:mi>W</z:mi></z:math> bosons are reconstructed from two hadronic jets. Simulation of the SM background processes is also done. The beam-induced backgrounds and the initial state radiation effects are taken into account. The majority of background processes are effectively suppressed by the cuts on the invariant masses of two and four
{"title":"Simulation of the process e+e−→W+W− with the heavy right-handed neutrino exchange at 1 TeV future lepton colliders","authors":"A. Drutskoy, E. Vasenin","doi":"10.1103/physrevd.111.015025","DOIUrl":"https://doi.org/10.1103/physrevd.111.015025","url":null,"abstract":"We study potential contribution of the heavy right-handed neutrino exchange in the process e</a:mi>+</a:mo></a:msup>e</a:mi>−</a:mo></a:msup>→</a:mo>W</a:mi>+</a:mo></a:msup>W</a:mi>−</a:mo></a:msup></a:math>. This process is sensitive to heavy neutrinos with masses larger than <d:math xmlns:d=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><d:msqrt><d:mi>s</d:mi></d:msqrt></d:math>. The Monte Carlo simulation of the studied process is performed assuming the seesaw type-I model, where heavy right-handed neutrinos (heavy neutral leptons, HNLs) are introduced in the leptonic sector. Within the Standard Model (SM), the process has a large cross section described by diagrams with <f:math xmlns:f=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><f:mi>s</f:mi></f:math>-channel <h:math xmlns:h=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><h:mi>Z</h:mi><h:mo>/</h:mo><h:mi>γ</h:mi></h:math> exchange and <j:math xmlns:j=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><j:mi>t</j:mi></j:math>-channel active neutrino exchange. Respectively, the <l:math xmlns:l=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><l:mi>t</l:mi></l:math>-channel right-handed neutrino exchange amplitude will interfere with these SM amplitudes. However, the angular distributions of the <n:math xmlns:n=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><n:mi>W</n:mi></n:math> boson production and decay are different for the right-handed neutrino and SM amplitudes. That can be used to evaluate potential HNL contribution using the extended likelihood method. The simulation of the <p:math xmlns:p=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><p:msup><p:mi>e</p:mi><p:mo>+</p:mo></p:msup><p:msup><p:mi>e</p:mi><p:mo>−</p:mo></p:msup><p:mo stretchy=\"false\">→</p:mo><p:msup><p:mi>W</p:mi><p:mo>+</p:mo></p:msup><p:msup><p:mi>W</p:mi><p:mo>−</p:mo></p:msup></p:math> process is performed at the 1 TeV center-of-mass energy and polarization <s:math xmlns:s=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><s:msub><s:mi mathvariant=\"script\">P</s:mi><s:mrow><s:msup><s:mi>e</s:mi><s:mo>+</s:mo></s:msup><s:msup><s:mi>e</s:mi><s:mo>−</s:mo></s:msup></s:mrow></s:msub></s:math> of (20%, <v:math xmlns:v=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><v:mo>−</v:mo><v:mn>80</v:mn><v:mo>%</v:mo></v:math>), which is a standard option for the future linear <x:math xmlns:x=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><x:msup><x:mi>e</x:mi><x:mo>+</x:mo></x:msup><x:msup><x:mi>e</x:mi><x:mo>−</x:mo></x:msup></x:math> International Linear Collider. Both <z:math xmlns:z=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><z:mi>W</z:mi></z:math> bosons are reconstructed from two hadronic jets. Simulation of the SM background processes is also done. The beam-induced backgrounds and the initial state radiation effects are taken into account. The majority of background processes are effectively suppressed by the cuts on the invariant masses of two and four ","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"30 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030856","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.015026
Dhruv Ringe
Recent evidence of a stochastic gravitational wave (GW) background found by NANOGrav and other pulsar timing array (PTA) collaborations has inspired many studies looking for possible sources. We consider the hypothesis that the GW signature is produced by domain walls (DWs) arising in the doublet left-right symmetric model (DLRSM) due to the spontaneous breaking of the discrete parity symmetry. We show that the DW network consists of two types of DWs, namely Z2 and LR DWs, and solve the kink equations to obtain the parametric dependence of the surface tension in the two cases. We argue that the Z2 DWs are unstable due to higher surface tension, leading to a stable network consisting only of LR DWs. Considering the GW signal from the DLRSM DW model with and without the contribution from supermassive black hole binaries, we perform a Bayesian analysis using the PTA data to estimate the posterior distribution and identify best-fit parameter ranges. The PTA data favors a parity-breaking scale of O(105)GeV, and a biased potential Vbias∼(O(100)MeV)4. The model with only DLRSM DWs is slightly favored over the model where additional supermassive black hole binaries contribution is considered. Published by the American Physical Society2025
{"title":"Domain wall constraints on the doublet left-right symmetric model from pulsar timing array data","authors":"Dhruv Ringe","doi":"10.1103/physrevd.111.015026","DOIUrl":"https://doi.org/10.1103/physrevd.111.015026","url":null,"abstract":"Recent evidence of a stochastic gravitational wave (GW) background found by NANOGrav and other pulsar timing array (PTA) collaborations has inspired many studies looking for possible sources. We consider the hypothesis that the GW signature is produced by domain walls (DWs) arising in the doublet left-right symmetric model (DLRSM) due to the spontaneous breaking of the discrete parity symmetry. We show that the DW network consists of two types of DWs, namely Z</a:mi>2</a:mn></a:msub></a:math> and <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mi>L</c:mi><c:mi>R</c:mi></c:math> DWs, and solve the kink equations to obtain the parametric dependence of the surface tension in the two cases. We argue that the <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:msub><e:mi>Z</e:mi><e:mn>2</e:mn></e:msub></e:math> DWs are unstable due to higher surface tension, leading to a stable network consisting only of <g:math xmlns:g=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><g:mi>L</g:mi><g:mi>R</g:mi></g:math> DWs. Considering the GW signal from the DLRSM DW model with and without the contribution from supermassive black hole binaries, we perform a Bayesian analysis using the PTA data to estimate the posterior distribution and identify best-fit parameter ranges. The PTA data favors a parity-breaking scale of <i:math xmlns:i=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><i:mi mathvariant=\"script\">O</i:mi><i:mo stretchy=\"false\">(</i:mo><i:msup><i:mn>10</i:mn><i:mn>5</i:mn></i:msup><i:mo stretchy=\"false\">)</i:mo><i:mtext> </i:mtext><i:mtext> </i:mtext><i:mi>GeV</i:mi></i:math>, and a biased potential <n:math xmlns:n=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><n:msub><n:mi>V</n:mi><n:mrow><n:mi>bias</n:mi></n:mrow></n:msub><n:mo>∼</n:mo><n:mo stretchy=\"false\">(</n:mo><n:mi mathvariant=\"script\">O</n:mi><n:mo stretchy=\"false\">(</n:mo><n:mn>100</n:mn><n:mo stretchy=\"false\">)</n:mo><n:mtext> </n:mtext><n:mtext> </n:mtext><n:mi>MeV</n:mi><n:msup><n:mo stretchy=\"false\">)</n:mo><n:mn>4</n:mn></n:msup></n:math>. The model with only DLRSM DWs is slightly favored over the model where additional supermassive black hole binaries contribution is considered. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"45 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030858","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.l021903
Matti Järvinen, Dorin Weissman
We establish a new tool for studying strongly coupled matter: an effective theory of black holes in gravity, which maps to a hydrodynamic description of field theories via the gauge-gravity duality. Our approach is inspired by previously known effective theories found in the limit of a high number of dimensions. We argue that the new approach can accurately describe phase transitions in a wide class of theories, such as the Yang-Mills and other nearly critical field theories. As an application to a previously unsolved problem, we analyze the interface between confining and deconfining phases in holographic Yang-Mills theory. Published by the American Physical Society2025
{"title":"Black hole effective theory for strongly interacting matter","authors":"Matti Järvinen, Dorin Weissman","doi":"10.1103/physrevd.111.l021903","DOIUrl":"https://doi.org/10.1103/physrevd.111.l021903","url":null,"abstract":"We establish a new tool for studying strongly coupled matter: an effective theory of black holes in gravity, which maps to a hydrodynamic description of field theories via the gauge-gravity duality. Our approach is inspired by previously known effective theories found in the limit of a high number of dimensions. We argue that the new approach can accurately describe phase transitions in a wide class of theories, such as the Yang-Mills and other nearly critical field theories. As an application to a previously unsolved problem, we analyze the interface between confining and deconfining phases in holographic Yang-Mills theory. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"35 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030857","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.015023
M. A. Arroyo-Ureña, E. A. Herrera-Chacón, S. Rosado-Navarro, Humberto Salazar
We explore the production and possible detection of a charged scalar Higgs pair H−H+ decaying into the final state μνμcb in proton-proton collisions at the LHC and its next step, the high luminosity LHC (HL-LHC). The charged scalars are predicted within the theoretical framework of the two-Higgs doublet model of type III (2HDM-III). As a test and validation of the model, we identify regions of the 2HDM-III parameter space that accommodate the current excess of events at 3σ in the process BR(t→H±b)×BR(H±→cb) for MH±=130GeV, as reported by ATLAS Collaboration. Theoretical and additional experimental constraints are also included. Based on this, we propose realistic scenarios that could be brought under experimental scrutiny at the HL-LHC. Assuming the most favorable scenario, we predict a signal significance at the level of 5σ for a charged scalar boson mass MH± in the 100–350 GeV range. Published by the American Physical Society2025
{"title":"Hunting for a charged Higgs boson pair in proton-proton collisions","authors":"M. A. Arroyo-Ureña, E. A. Herrera-Chacón, S. Rosado-Navarro, Humberto Salazar","doi":"10.1103/physrevd.111.015023","DOIUrl":"https://doi.org/10.1103/physrevd.111.015023","url":null,"abstract":"We explore the production and possible detection of a charged scalar Higgs pair H</a:mi>−</a:mo></a:msup>H</a:mi>+</a:mo></a:msup></a:math> decaying into the final state <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mi>μ</c:mi><c:msub><c:mi>ν</c:mi><c:mi>μ</c:mi></c:msub><c:mi>c</c:mi><c:mi>b</c:mi></c:math> in proton-proton collisions at the LHC and its next step, the high luminosity LHC (HL-LHC). The charged scalars are predicted within the theoretical framework of the two-Higgs doublet model of type III (2HDM-III). As a test and validation of the model, we identify regions of the 2HDM-III parameter space that accommodate the current excess of events at <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:mn>3</e:mn><e:mi>σ</e:mi></e:math> in the process <g:math xmlns:g=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><g:mi mathvariant=\"script\">B</g:mi><g:mi mathvariant=\"script\">R</g:mi><g:mo stretchy=\"false\">(</g:mo><g:mi>t</g:mi><g:mo stretchy=\"false\">→</g:mo><g:msup><g:mi>H</g:mi><g:mo>±</g:mo></g:msup><g:mi>b</g:mi><g:mo stretchy=\"false\">)</g:mo><g:mo>×</g:mo><g:mi mathvariant=\"script\">B</g:mi><g:mi mathvariant=\"script\">R</g:mi><g:mo stretchy=\"false\">(</g:mo><g:msup><g:mi>H</g:mi><g:mo>±</g:mo></g:msup><g:mo stretchy=\"false\">→</g:mo><g:mi>c</g:mi><g:mi>b</g:mi><g:mo stretchy=\"false\">)</g:mo></g:math> for <s:math xmlns:s=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><s:msub><s:mi>M</s:mi><s:msup><s:mi>H</s:mi><s:mo>±</s:mo></s:msup></s:msub><s:mo>=</s:mo><s:mn>130</s:mn><s:mtext> </s:mtext><s:mtext> </s:mtext><s:mi>GeV</s:mi></s:math>, as reported by ATLAS Collaboration. Theoretical and additional experimental constraints are also included. Based on this, we propose realistic scenarios that could be brought under experimental scrutiny at the HL-LHC. Assuming the most favorable scenario, we predict a signal significance at the level of <u:math xmlns:u=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><u:mn>5</u:mn><u:mi>σ</u:mi></u:math> for a charged scalar boson mass <w:math xmlns:w=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><w:msub><w:mi>M</w:mi><w:msup><w:mi>H</w:mi><w:mo>±</w:mo></w:msup></w:msub></w:math> in the 100–350 GeV range. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"14 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030862","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.024060
Michael L. Katz, Nikolaos Karnesis, Natalia Korsakova, Jonathan R. Gair, Nikolaos Stergioulas
The large-scale analysis task of deciphering gravitational-wave signals in the LISA data stream will be difficult, requiring a large amount of computational resources and extensive development of computational methods. Its high dimensionality, multiple model types, and complicated noise profile require a global fit to all parameters and input models simultaneously. In this work, we detail our global fit algorithm, called “Erebor,” designed to accomplish this challenging task. It is capable of analyzing current state-of-the-art datasets and then growing into the future as more pieces of the pipeline are completed and added. We describe our pipeline strategy, the algorithmic setup, and the results from our analysis of the LDC2A Sangria dataset, which contains massive black hole binaries, compact galactic binaries, and a parametrized noise spectrum whose parameters are unknown to the user. The Erebor algorithm includes three unique and very useful contributions: GPU acceleration for enhanced computational efficiency; ensemble Markov Chain Monte Carlo (MCMC) sampling with multiple MCMC walkers per temperature for better mixing and parallelized sample creation; and special online updates to reversible-jump (or transdimensional) sampling distributions to ensure sampler mixing and accurate initial estimates for detectable sources in the data. We recover posterior distributions for all 15 (6) of the injected massive black hole binaries (MBHB) in the LDC2A training (hidden) dataset. We catalog ∼12000 galactic binaries (∼8000 as high confidence detections) for both the training and hidden datasets. All of the sources and their posterior distributions are provided in publicly available catalogs. Published by the American Physical Society2025
{"title":"Efficient GPU-accelerated multisource global fit pipeline for LISA data analysis","authors":"Michael L. Katz, Nikolaos Karnesis, Natalia Korsakova, Jonathan R. Gair, Nikolaos Stergioulas","doi":"10.1103/physrevd.111.024060","DOIUrl":"https://doi.org/10.1103/physrevd.111.024060","url":null,"abstract":"The large-scale analysis task of deciphering gravitational-wave signals in the LISA data stream will be difficult, requiring a large amount of computational resources and extensive development of computational methods. Its high dimensionality, multiple model types, and complicated noise profile require a global fit to all parameters and input models simultaneously. In this work, we detail our global fit algorithm, called “Erebor,” designed to accomplish this challenging task. It is capable of analyzing current state-of-the-art datasets and then growing into the future as more pieces of the pipeline are completed and added. We describe our pipeline strategy, the algorithmic setup, and the results from our analysis of the LDC2A Sangria dataset, which contains massive black hole binaries, compact galactic binaries, and a parametrized noise spectrum whose parameters are unknown to the user. The Erebor algorithm includes three unique and very useful contributions: GPU acceleration for enhanced computational efficiency; ensemble Markov Chain Monte Carlo (MCMC) sampling with multiple MCMC walkers per temperature for better mixing and parallelized sample creation; and special online updates to reversible-jump (or transdimensional) sampling distributions to ensure sampler mixing and accurate initial estimates for detectable sources in the data. We recover posterior distributions for all 15 (6) of the injected massive black hole binaries (MBHB) in the LDC2A training (hidden) dataset. We catalog ∼</a:mo>12000</a:mn></a:math> galactic binaries (<c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mo>∼</c:mo><c:mn>8000</c:mn></c:math> as high confidence detections) for both the training and hidden datasets. All of the sources and their posterior distributions are provided in publicly available catalogs. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"30 11 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030855","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.015024
Luis A. Anchordoqui, Ignatios Antoniadis, Dieter Lüst, Karem Peñaló Castillo
We reexamine a dynamical dark matter model with Kaluza-Klein (KK) towers of gravitons and neutrinos fitting together in the dark dimension. We show that even though gravitational decays of neutrino KK towers have little impact in cosmology, the weak decay channel could have significant cosmological effects. Taking conservative upper bounds on the dark matter decay rate into two photons before reionization and on the number of effective extra neutrino species ΔNeff, we derive constraints on the conversion rate from active to sterile species despite the dependence of the mixing angle on the KK mode mass. We also provide counterarguments to a recent claim suggesting that the bounds on ΔNeff rule out micron-sized extra dimensions. Published by the American Physical Society2025
{"title":"Cosmological constraints on dark neutrino towers","authors":"Luis A. Anchordoqui, Ignatios Antoniadis, Dieter Lüst, Karem Peñaló Castillo","doi":"10.1103/physrevd.111.015024","DOIUrl":"https://doi.org/10.1103/physrevd.111.015024","url":null,"abstract":"We reexamine a dynamical dark matter model with Kaluza-Klein (KK) towers of gravitons and neutrinos fitting together in the dark dimension. We show that even though gravitational decays of neutrino KK towers have little impact in cosmology, the weak decay channel could have significant cosmological effects. Taking conservative upper bounds on the dark matter decay rate into two photons before reionization and on the number of effective extra neutrino species Δ</a:mi>N</a:mi>eff</a:mi></a:msub></a:math>, we derive constraints on the conversion rate from active to sterile species despite the dependence of the mixing angle on the KK mode mass. We also provide counterarguments to a recent claim suggesting that the bounds on <d:math xmlns:d=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><d:mi mathvariant=\"normal\">Δ</d:mi><d:msub><d:mi>N</d:mi><d:mi>eff</d:mi></d:msub></d:math> rule out micron-sized extra dimensions. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"67 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030859","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.023042
Yann Cado, Christoph Englert, Tanmoy Modak, Mariano Quirós
We investigate the impact of preheating on baryogenesis in R2-Higgs inflation. In this scenario, the inclusion of a dimension-six operator (R/Λ2)BμνB˜μν abundantly generates helical hypermagnetic fields during inflation, leading to a baryon asymmetric Universe at the electroweak crossover. Focusing on the R2-like regime, we first derive the relevant dynamics of preheating using a doubly covariant formalism. We find that preheating can happen for the Higgs, transverse gauge, and Goldstone bosons, however, it is dependent on the value of the nonminimal coupling ξH between the Standard Model Higgs field and the Ricci scalar. We identify the preheating temperature to determine the appropriate scale Λ for driving baryogenesis, which is around Λ∼2.2(2.6)×10−5MP for ξH∼1(10). Our results represent the most accurate estimation of the scale of gravity induced baryogenesis in R2-Higgs inflation to date. Areas for further improvement are identified. Published by the American Physical Society2025
{"title":"Implication of preheating on gravity assisted baryogenesis in R2 -Higgs inflation","authors":"Yann Cado, Christoph Englert, Tanmoy Modak, Mariano Quirós","doi":"10.1103/physrevd.111.023042","DOIUrl":"https://doi.org/10.1103/physrevd.111.023042","url":null,"abstract":"We investigate the impact of preheating on baryogenesis in R</a:mi>2</a:mn></a:msup></a:math>-Higgs inflation. In this scenario, the inclusion of a dimension-six operator <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mrow><c:mo stretchy=\"false\">(</c:mo><c:mi>R</c:mi><c:mo>/</c:mo><c:msup><c:mi mathvariant=\"normal\">Λ</c:mi><c:mn>2</c:mn></c:msup><c:mo stretchy=\"false\">)</c:mo></c:mrow><c:msub><c:mi>B</c:mi><c:mrow><c:mi>μ</c:mi><c:mi>ν</c:mi></c:mrow></c:msub><c:msup><c:mover accent=\"true\"><c:mi>B</c:mi><c:mo stretchy=\"false\">˜</c:mo></c:mover><c:mrow><c:mi>μ</c:mi><c:mi>ν</c:mi></c:mrow></c:msup></c:math> abundantly generates helical hypermagnetic fields during inflation, leading to a baryon asymmetric Universe at the electroweak crossover. Focusing on the <j:math xmlns:j=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><j:msup><j:mi>R</j:mi><j:mn>2</j:mn></j:msup></j:math>-like regime, we first derive the relevant dynamics of preheating using a doubly covariant formalism. We find that preheating can happen for the Higgs, transverse gauge, and Goldstone bosons, however, it is dependent on the value of the nonminimal coupling <l:math xmlns:l=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><l:msub><l:mi>ξ</l:mi><l:mi>H</l:mi></l:msub></l:math> between the Standard Model Higgs field and the Ricci scalar. We identify the preheating temperature to determine the appropriate scale <n:math xmlns:n=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><n:mi mathvariant=\"normal\">Λ</n:mi></n:math> for driving baryogenesis, which is around <q:math xmlns:q=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><q:mrow><q:mi mathvariant=\"normal\">Λ</q:mi><q:mo>∼</q:mo><q:mn>2.2</q:mn><q:mo stretchy=\"false\">(</q:mo><q:mn>2.6</q:mn><q:mo stretchy=\"false\">)</q:mo><q:mo>×</q:mo><q:msup><q:mrow><q:mn>10</q:mn></q:mrow><q:mrow><q:mo>−</q:mo><q:mn>5</q:mn></q:mrow></q:msup><q:msub><q:mrow><q:mi>M</q:mi></q:mrow><q:mrow><q:mi mathvariant=\"normal\">P</q:mi></q:mrow></q:msub></q:mrow></q:math> for <w:math xmlns:w=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><w:msub><w:mi>ξ</w:mi><w:mi>H</w:mi></w:msub><w:mo>∼</w:mo><w:mn>1</w:mn><w:mo stretchy=\"false\">(</w:mo><w:mn>10</w:mn><w:mo stretchy=\"false\">)</w:mo></w:math>. Our results represent the most accurate estimation of the scale of gravity induced baryogenesis in R</ab:mi>2</ab:mn></ab:msup></ab:math>-Higgs inflation to date. Areas for further improvement are identified. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"52 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030861","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.025020
Y. Ageeva, P. Petrov, M. Shaposhnikov
In this paper, we show how the finite formulation of quantum field theory based on Callan-Symanzik equations can be generalized to the case of nonrenormalizable theories. We derive an equation for effective action for an arbitrary single scalar field theory, allowing us to perform computations without running in intermediate divergencies. We illustrate the method with the use of λϕ4+ϕ6/M2 theory by the explicit (and fully finite) calculations of the effective potential as well as two-, four- and six-point correlation functions at one-loop level and demonstrate that no quantum corrections to scalar mass m2, depending on M2 scale, are generated. Published by the American Physical Society2025
{"title":"Nonrenormalizable theories and finite formulation of QFT","authors":"Y. Ageeva, P. Petrov, M. Shaposhnikov","doi":"10.1103/physrevd.111.025020","DOIUrl":"https://doi.org/10.1103/physrevd.111.025020","url":null,"abstract":"In this paper, we show how the finite formulation of quantum field theory based on Callan-Symanzik equations can be generalized to the case of nonrenormalizable theories. We derive an equation for effective action for an arbitrary single scalar field theory, allowing us to perform computations without running in intermediate divergencies. We illustrate the method with the use of λ</a:mi>ϕ</a:mi></a:mrow>4</a:mn></a:mrow></a:msup>+</a:mo>ϕ</a:mi></a:mrow>6</a:mn></a:mrow></a:msup>/</a:mo>M</a:mi></a:mrow>2</a:mn></a:mrow></a:msup></a:mrow></a:math> theory by the explicit (and fully finite) calculations of the effective potential as well as two-, four- and six-point correlation functions at one-loop level and demonstrate that no quantum corrections to scalar mass <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:msup><c:mi>m</c:mi><c:mn>2</c:mn></c:msup></c:math>, depending on <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:msup><e:mi>M</e:mi><e:mn>2</e:mn></e:msup></e:math> scale, are generated. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"206 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143031340","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.023041
David E. Kaplan, Xuheng Luo, Ngan H. Nguyen, Surjeet Rajendran, Erwin H. Tanin
Dark matter may exist today in the form of ultraheavy composite bound states. Collisions between such dark matter states can release intense bursts of radiation that include γ-rays among the final products. Thus, indirect detection signals of dark matter may include unconventional γ-ray bursts. Such bursts may have been missed not necessarily because of their low arriving γ-ray fluxes, but rather their briefness and rareness. We point out that intense bursts whose nondetection thus far are due to the latter can be detected in the near future with existing and planned facilities. In particular, we propose that, with slight experimental adjustments and suitable data analyses, imaging atmospheric Cherenkov telescopes (IACTs) and Pulsed All-Sky Near-Infrared and Optical Search for Extra-Terrestrial Intelligence (PANOSETI) are promising tools for detecting such rare, brief, but intense bursts. We also show that, if we assume these bursts originate from collisions of dark matter states, IACTs and PANOSETI can probe a large dark matter parameter space beyond existing limits. Additionally, we present a concrete model of dark matter that produces bursts potentially detectable in these instruments. Published by the American Physical Society2025
{"title":"Indirect searches for ultraheavy dark matter in the time domain","authors":"David E. Kaplan, Xuheng Luo, Ngan H. Nguyen, Surjeet Rajendran, Erwin H. Tanin","doi":"10.1103/physrevd.111.023041","DOIUrl":"https://doi.org/10.1103/physrevd.111.023041","url":null,"abstract":"Dark matter may exist today in the form of ultraheavy composite bound states. Collisions between such dark matter states can release intense bursts of radiation that include γ</a:mi></a:math>-rays among the final products. Thus, indirect detection signals of dark matter may include unconventional <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mi>γ</c:mi></c:math>-ray bursts. Such bursts may have been missed not necessarily because of their low arriving <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:mi>γ</e:mi></e:math>-ray fluxes, but rather their briefness and rareness. We point out that intense bursts whose nondetection thus far are due to the latter can be detected in the near future with existing and planned facilities. In particular, we propose that, with slight experimental adjustments and suitable data analyses, imaging atmospheric Cherenkov telescopes (IACTs) and Pulsed All-Sky Near-Infrared and Optical Search for Extra-Terrestrial Intelligence (PANOSETI) are promising tools for detecting such rare, brief, but intense bursts. We also show that, if we assume these bursts originate from collisions of dark matter states, IACTs and PANOSETI can probe a large dark matter parameter space beyond existing limits. Additionally, we present a concrete model of dark matter that produces bursts potentially detectable in these instruments. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"2 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143030860","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-01-24DOI: 10.1103/physrevd.111.023535
Rayne Liu, Wayne Hu, Huangyu Xiao
Wave or fuzzy dark matter that is produced with relativistic wave numbers exhibits free-streaming effects analogous to warm or hot particle dark matter with relativistic momenta. Axions produced after inflation provide such a warm or mildly relativistic candidate, where the enhanced suppression and observational bounds are only moderately stronger than that from wave propagation of initially cold axions. More generally, the free-streaming damping also impacts isocurvature fluctuations from generation in causally disconnected patches. As coherent spatial fluctuations free stream away they leave incoherent and transient superpositions in their wakes. These multiple wave momentum streams are the wave analog of particle phase space fluctuations or directional collisionless damping of massive neutrinos or hot dark matter. The observable impact on both adiabatic and isocurvature fluctuations of fuzzy dark matter can differ from their cold dark matter counterparts due to free streaming depending on how warm or hot is their momentum distribution. Published by the American Physical Society2025
{"title":"Warm and fuzzy dark matter: Free streaming of wave dark matter","authors":"Rayne Liu, Wayne Hu, Huangyu Xiao","doi":"10.1103/physrevd.111.023535","DOIUrl":"https://doi.org/10.1103/physrevd.111.023535","url":null,"abstract":"Wave or fuzzy dark matter that is produced with relativistic wave numbers exhibits free-streaming effects analogous to warm or hot particle dark matter with relativistic momenta. Axions produced after inflation provide such a warm or mildly relativistic candidate, where the enhanced suppression and observational bounds are only moderately stronger than that from wave propagation of initially cold axions. More generally, the free-streaming damping also impacts isocurvature fluctuations from generation in causally disconnected patches. As coherent spatial fluctuations free stream away they leave incoherent and transient superpositions in their wakes. These multiple wave momentum streams are the wave analog of particle phase space fluctuations or directional collisionless damping of massive neutrinos or hot dark matter. The observable impact on both adiabatic and isocurvature fluctuations of fuzzy dark matter can differ from their cold dark matter counterparts due to free streaming depending on how warm or hot is their momentum distribution. <jats:supplementary-material> <jats:copyright-statement>Published by the American Physical Society</jats:copyright-statement> <jats:copyright-year>2025</jats:copyright-year> </jats:permissions> </jats:supplementary-material>","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"8 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143031339","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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