Pub Date : 2025-03-19DOI: 10.1103/physrevd.111.063052
Anna M. Suliga, George M. Fuller
The indirect detection of dark matter (DM) through its annihilation products is one of the primary strategies for DM detection. One of the least constrained classes of models is neutrinophilic DM, because the annihilation products, weakly interacting neutrinos, are challenging to observe. Here, we consider a scenario where MeV-mass DM exclusively annihilates to the third neutrino mass eigenstate, which is predominantly of tau and muon flavor. In such a scenario, the potential detection rate of the neutrinos originating from the DM annihilation in our Galaxy in the conventional detectors would be suppressed by up to approximately two orders of magnitude. This is because the best sensitivity of such detectors for neutrinos with energies below approximately 100 MeV is for electron neutrino flavor. In this work, we highlight the potential of large-scale DM detectors in uncovering such signals in the tens of MeV range of DM masses. In addition, we discuss how coincident signals in direct detection DM experiments and upcoming neutrino detectors such as DUNE, Hyper-Kamiokande, and JUNO could provide new perspectives on the DM problem. Published by the American Physical Society2025
{"title":"Searching for MeV-mass neutrinophilic dark matter with large scale dark matter detectors","authors":"Anna M. Suliga, George M. Fuller","doi":"10.1103/physrevd.111.063052","DOIUrl":"https://doi.org/10.1103/physrevd.111.063052","url":null,"abstract":"The indirect detection of dark matter (DM) through its annihilation products is one of the primary strategies for DM detection. One of the least constrained classes of models is neutrinophilic DM, because the annihilation products, weakly interacting neutrinos, are challenging to observe. Here, we consider a scenario where MeV-mass DM exclusively annihilates to the third neutrino mass eigenstate, which is predominantly of tau and muon flavor. In such a scenario, the potential detection rate of the neutrinos originating from the DM annihilation in our Galaxy in the conventional detectors would be suppressed by up to approximately two orders of magnitude. This is because the best sensitivity of such detectors for neutrinos with energies below approximately 100 MeV is for electron neutrino flavor. In this work, we highlight the potential of large-scale DM detectors in uncovering such signals in the tens of MeV range of DM masses. In addition, we discuss how coincident signals in direct detection DM experiments and upcoming neutrino detectors such as DUNE, Hyper-Kamiokande, and JUNO could provide new perspectives on the DM problem. <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":"42 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143660712","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 : 2025-03-19DOI: 10.1103/physrevd.111.066014
Batoul Banihashemi, Ted Jacobson
The gravitational path integral is usually implemented with a covariant action by analogy with other gauge field theories, but the gravitational case is different in important ways. A key difference is that the integrand has an essential singularity, which occurs at zero lapse where the spacetime metric degenerates. The lapse integration contour required to impose the local time reparametrization constraints must run from −∞ to +∞, yet must not pass through zero. This raises the question: for an application—such as a partition function—where the constraints should be imposed, what is the correct integration contour, and why? We study that question by starting with the reduced phase space path integral, which involves no essential singularity. We observe that if the momenta are to be integrated before the lapse, to obtain a configuration space path integral, the lapse contour should pass below the origin in the complex lapse plane. This contour is also consistent with the requirement that quantum field fluctuation amplitudes have the usual short distance vacuum form, and with obtaining the Bekenstein-Hawking horizon entropy from a Lorentzian path integral. Published by the American Physical Society2025
{"title":"On the lapse contour in the gravitational path integral","authors":"Batoul Banihashemi, Ted Jacobson","doi":"10.1103/physrevd.111.066014","DOIUrl":"https://doi.org/10.1103/physrevd.111.066014","url":null,"abstract":"The gravitational path integral is usually implemented with a covariant action by analogy with other gauge field theories, but the gravitational case is different in important ways. A key difference is that the integrand has an essential singularity, which occurs at zero lapse where the spacetime metric degenerates. The lapse integration contour required to impose the local time reparametrization constraints must run from −</a:mo>∞</a:mi></a:mrow></a:math> to <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mo>+</c:mo><c:mi>∞</c:mi></c:math>, yet must not pass through zero. This raises the question: for an application—such as a partition function—where the constraints should be imposed, what is the correct integration contour, and why? We study that question by starting with the reduced phase space path integral, which involves no essential singularity. We observe that if the momenta are to be integrated before the lapse, to obtain a configuration space path integral, the lapse contour should pass below the origin in the complex lapse plane. This contour is also consistent with the requirement that quantum field fluctuation amplitudes have the usual short distance vacuum form, and with obtaining the Bekenstein-Hawking horizon entropy from a Lorentzian path integral. <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":"214 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143653732","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}
We discuss a mechanism of primordial black hole (PBH) formation that does not require specific features in the inflationary potential, revisiting previous literature. In this mechanism, a light spectator field evolves stochastically during inflation and remains subdominant during the post-inflationary era. Even though the curvature power spectrum stays small at all scales, rare perturbations of the field probe a local maximum in its potential, leading to non-Gaussian tails in the distribution of curvature fluctuations, and to copious PBH production. For a concrete axionlike particle (ALP) scenario we analytically determine the distribution of the compaction function for perturbations, showing that it is characterized by a heavy tail, which produces an extended PBH mass distribution. We find the ALP mass and decay constant to be correlated with the PBH mass, for instance, an ALP with a mass ma=5.4×1014eV and a decay constant fa=4.6×10−5MPl can lead to PBHs of mass MPBH=1021g as the entire dark matter of the universe, and is testable in future PBH observations via lensing in the Nancy Grace Roman Space Telescope and mergers detectable in the Laser Interferometer Space Antenna and Einstein Telescope gravitational wave detectors. We then extend our analysis to mixed ALP and PBH dark matter and Higgs-like spectator fields. We find that PBHs cluster strongly over all cosmological scales, clashing with cosmic microwave background isocurvature bounds. We argue that this problem is shared by all PBH production from inflationary models that depend solely on large non-Gaussianity without a peak in the curvature power spectrum and discuss possible remedies. Published by the American Physical Society2025
我们讨论了一种原始黑洞（PBH）的形成机制，它不需要暴胀势中的特定特征，并对以前的文献进行了重温。在这一机制中，一个轻的旁观者场在膨胀过程中随机演化，并在后膨胀时代保持次主导地位。尽管曲率功率谱在所有尺度上都保持较小，但该场的罕见扰动会探测到其势能的局部最大值，从而导致曲率波动分布中的非高斯尾，并产生大量 PBH。对于一个具体的类轴子粒子（ALP）情景，我们分析测定了扰动的压实函数分布，结果表明它的特点是有一个重尾，从而产生了一个扩展的 PBH 质量分布。我们发现 ALP 的质量和衰变常数与 PBH 的质量相关，例如，质量 ma=5.4×1014eV 和衰变常数 fa=4.6×10-5 MPl 的 ALP 可以导致质量 MPBH=1021 g 的 PBH，作为整个宇宙的暗物质，并且可以在未来的 PBH 观测中通过南希-格雷斯-罗曼太空望远镜的透镜以及激光干涉仪太空天线和爱因斯坦望远镜引力波探测器探测到的合并进行检验。然后，我们将分析扩展到混合 ALP 和 PBH 暗物质以及类希格斯谱场。我们发现，PBH 在所有宇宙学尺度上都有强烈的聚类，这与宇宙微波背景等曲率边界相冲突。我们认为这个问题与所有仅依赖于大非高斯性而没有曲率功率谱峰值的暴胀模型产生的 PBH 都有相同之处，并讨论了可能的补救措施。 美国物理学会出版 2025
{"title":"Stochastic axionlike curvaton: Non-Gaussianity and primordial black holes without a large power spectrum","authors":"Chao Chen, Anish Ghoshal, Gianmassimo Tasinato, Eemeli Tomberg","doi":"10.1103/physrevd.111.063539","DOIUrl":"https://doi.org/10.1103/physrevd.111.063539","url":null,"abstract":"We discuss a mechanism of primordial black hole (PBH) formation that does not require specific features in the inflationary potential, revisiting previous literature. In this mechanism, a light spectator field evolves stochastically during inflation and remains subdominant during the post-inflationary era. Even though the curvature power spectrum stays small at all scales, rare perturbations of the field probe a local maximum in its potential, leading to non-Gaussian tails in the distribution of curvature fluctuations, and to copious PBH production. For a concrete axionlike particle (ALP) scenario we analytically determine the distribution of the compaction function for perturbations, showing that it is characterized by a heavy tail, which produces an extended PBH mass distribution. We find the ALP mass and decay constant to be correlated with the PBH mass, for instance, an ALP with a mass m</a:mi></a:mrow>a</a:mi></a:mrow></a:msub>=</a:mo>5.4</a:mn>×</a:mo>10</a:mn></a:mrow>14</a:mn></a:mrow></a:msup></a:mtext></a:mtext>eV</a:mi></a:mrow></a:mrow></a:math> and a decay constant <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mrow><c:msub><c:mrow><c:mi>f</c:mi></c:mrow><c:mrow><c:mi>a</c:mi></c:mrow></c:msub><c:mo>=</c:mo><c:mrow><c:mn>4.6</c:mn><c:mo>×</c:mo><c:msup><c:mrow><c:mn>10</c:mn></c:mrow><c:mrow><c:mo>−</c:mo><c:mn>5</c:mn></c:mrow></c:msup><c:mtext> </c:mtext></c:mrow><c:msub><c:mrow><c:mi>M</c:mi></c:mrow><c:mrow><c:mi>Pl</c:mi></c:mrow></c:msub></c:mrow></c:math> can lead to PBHs of mass <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:mrow><e:msub><e:mrow><e:mi>M</e:mi></e:mrow><e:mrow><e:mi>PBH</e:mi></e:mrow></e:msub><e:mo>=</e:mo><e:msup><e:mrow><e:mn>10</e:mn></e:mrow><e:mrow><e:mn>21</e:mn></e:mrow></e:msup><e:mtext> </e:mtext><e:mtext> </e:mtext><e:mi mathvariant=\"normal\">g</e:mi></e:mrow></e:math> as the entire dark matter of the universe, and is testable in future PBH observations via lensing in the Nancy Grace Roman Space Telescope and mergers detectable in the Laser Interferometer Space Antenna and Einstein Telescope gravitational wave detectors. We then extend our analysis to mixed ALP and PBH dark matter and Higgs-like spectator fields. We find that PBHs cluster strongly over all cosmological scales, clashing with cosmic microwave background isocurvature bounds. We argue that this problem is shared by all PBH production from inflationary models that depend solely on large non-Gaussianity without a peak in the curvature power spectrum and discuss possible remedies. <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":"34 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143660581","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 : 2025-03-18DOI: 10.1103/physrevd.111.056023
Ziyue Wang, Shu Lin
Motivated by the key role of shear induced polarization in understanding the local spin polarization puzzle of Λ hyperons in heavy ion collisions, we perform a complete analysis of spin polarization of massive fermion in a quantum electrodynamic plasma with shear flow. Apart from the well-known spin-shear coupling in free theory, we include two more collision dependent contributions: one is a nondynamical contribution fixed by shifted spin-averaged distribution in steady state; the other is a dynamical contribution following from spin evolution. Despite of the dependencies on collision, we find the dependencies on coupling drop out in the final results. These contributions can lead to significant enhancement of the spin-shear coupling in phenomenologically interesting regime. Published by the American Physical Society2025
{"title":"Spin polarization for massive fermion in a shear flow: Complete results at O(∂)","authors":"Ziyue Wang, Shu Lin","doi":"10.1103/physrevd.111.056023","DOIUrl":"https://doi.org/10.1103/physrevd.111.056023","url":null,"abstract":"Motivated by the key role of shear induced polarization in understanding the local spin polarization puzzle of Λ</a:mi></a:math> hyperons in heavy ion collisions, we perform a complete analysis of spin polarization of massive fermion in a quantum electrodynamic plasma with shear flow. Apart from the well-known spin-shear coupling in free theory, we include two more collision dependent contributions: one is a nondynamical contribution fixed by shifted spin-averaged distribution in steady state; the other is a dynamical contribution following from spin evolution. Despite of the dependencies on collision, we find the dependencies on coupling drop out in the final results. These contributions can lead to significant enhancement of the spin-shear coupling in phenomenologically interesting regime. <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":"33 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143653778","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 : 2025-03-18DOI: 10.1103/physrevd.111.065017
Chiang-Mei Chen, Chun-Chih Huang, Sang Pyo Kim, Chun-Yu Wei
Kerr-Newman black holes in a de Sitter (dS) space have the limit of rotating Nariai black holes with the near-horizon geometry of a warped dS3×S1/Z2 when the black hole horizon and the cosmological horizon coincide or approach close to each other. We study the rotation effect on the spontaneous emission of charges in the near-extremal rotating charged Nariai black hole and compare it to those from the near-extremal Nariai black hole in [C.-M. Chen , ] and near-extremal Kerr-Newman black hole in de Sitter space in [C.-M. Chen and S. P. Kim, ]. In strong contrast to the near-extremal Kerr-Newman black hole in dS space, the near-extremal rotating Nariai black hole also has an exponential amplification for the emission of high-energy charges, which becomes catastrophic regardless of angular momentum when two horizons coincide. The radius of rotating Nariai black holes monotonically increases as the angular momentum and charge of black holes increase, which gives a weaker electric field on the horizon than Nariai black holes. Thus, the angular momentum of black holes that drags particles on the horizon decreases the mean number of charges by a factor not by an order. We observe a catastrophic emission of boson condensation for charges with an effective energy equal to the chemical potential in the spacelike outer region of the cosmological horizon. Remarkably, the Schwinger emission of charges in the standard particle model may prevent the rotating Nariai black holes from evolving into spacetimes with a naked singularity when the angular momentum is close to the allowed maximum, which Nariai black holes cannot avoid. Published by the American Physical Society2025
{"title":"Catastrophic emission of charges from near-extremal charged Nariai black holes. II. Rotation effect","authors":"Chiang-Mei Chen, Chun-Chih Huang, Sang Pyo Kim, Chun-Yu Wei","doi":"10.1103/physrevd.111.065017","DOIUrl":"https://doi.org/10.1103/physrevd.111.065017","url":null,"abstract":"Kerr-Newman black holes in a de Sitter (dS) space have the limit of rotating Nariai black holes with the near-horizon geometry of a warped dS</a:mi>3</a:mn></a:msub>×</a:mo>S</a:mi>1</a:mn></a:msup>/</a:mo>Z</a:mi>2</a:mn></a:msub></a:math> when the black hole horizon and the cosmological horizon coincide or approach close to each other. We study the rotation effect on the spontaneous emission of charges in the near-extremal rotating charged Nariai black hole and compare it to those from the near-extremal Nariai black hole in [C.-M. Chen , ] and near-extremal Kerr-Newman black hole in de Sitter space in [C.-M. Chen and S. P. Kim, ]. In strong contrast to the near-extremal Kerr-Newman black hole in dS space, the near-extremal rotating Nariai black hole also has an exponential amplification for the emission of high-energy charges, which becomes catastrophic regardless of angular momentum when two horizons coincide. The radius of rotating Nariai black holes monotonically increases as the angular momentum and charge of black holes increase, which gives a weaker electric field on the horizon than Nariai black holes. Thus, the angular momentum of black holes that drags particles on the horizon decreases the mean number of charges by a factor not by an order. We observe a catastrophic emission of boson condensation for charges with an effective energy equal to the chemical potential in the spacelike outer region of the cosmological horizon. Remarkably, the Schwinger emission of charges in the standard particle model may prevent the rotating Nariai black holes from evolving into spacetimes with a naked singularity when the angular momentum is close to the allowed maximum, which Nariai black holes cannot avoid. <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":"125 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143653733","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 : 2025-03-18DOI: 10.1103/physrevd.111.054510
Peter Boyle, Felix Erben, Vera Gülpers, Maxwell T. Hansen, Fabian Joswig, Michael Marshall, Nelson Pitanga Lachini, Antonin Portelli
We present our study of the ρ</a:mi>(</a:mo>770</a:mn>)</a:mo></a:math> and <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:msup><e:mi>K</e:mi><e:mo>*</e:mo></e:msup><e:mo stretchy="false">(</e:mo><e:mn>892</e:mn><e:mo stretchy="false">)</e:mo></e:math> resonances from lattice quantum chromodynamics (QCD) employing domain-wall fermions at physical quark masses. We determine the finite-volume energy spectrum in various momentum frames and obtain phase-shift parametrizations via the Lüscher formalism and as a final step the complex resonance poles of the <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:mi>π</i:mi><i:mi>π</i:mi></i:math> and <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:mi>K</k:mi><k:mi>π</k:mi></k:math> elastic scattering amplitudes via an analytical continuation of the models. By sampling a large number of representative sets of underlying energy-level fits, we also assign a systematic uncertainty to our final results. This is a significant extension to data-driven analysis methods that have been used in lattice QCD to date, due to the two-step nature of the formalism. Our final pole positions, <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:mi>M</m:mi><m:mo>+</m:mo><m:mi>i</m:mi><m:mi mathvariant="normal">Γ</m:mi><m:mo>/</m:mo><m:mn>2</m:mn></m:math>, with all statistical and systematic errors exposed, are <p:math xmlns:p="http://www.w3.org/1998/Math/MathML" display="inline"><p:mrow><p:msub><p:mrow><p:mi>M</p:mi></p:mrow><p:mrow><p:msup><p:mrow><p:mi>K</p:mi></p:mrow><p:mrow><p:mo>*</p:mo></p:mrow></p:msup></p:mrow></p:msub><p:mo>=</p:mo><p:mn>893</p:mn><p:mo stretchy="false">(</p:mo><p:mn>2</p:mn><p:mo stretchy="false">)</p:mo><p:mo stretchy="false">(</p:mo><p:mn>8</p:mn><p:mo stretchy="false">)</p:mo><p:mo stretchy="false">(</p:mo><p:mn>54</p:mn><p:mo stretchy="false">)</p:mo><p:mo stretchy="false">(</p:mo><p:mn>2</p:mn><p:mo stretchy="false">)</p:mo><p:mtext> </p:mtext><p:mtext> </p:mtext><p:mi>MeV</p:mi></p:mrow></p:math> and <z:math xmlns:z="http://www.w3.org/1998/Math/MathML" display="inline"><z:msub><z:mi mathvariant="normal">Γ</z:mi><z:msup><z:mi>K</z:mi><z:mo>*</z:mo></z:msup></z:msub><z:mo>=</z:mo><z:mn>51</z:mn><z:mo stretchy="false">(</z:mo><z:mn>2</z:mn><z:mo stretchy="false">)</z:mo><z:mo stretchy="false">(</z:mo><z:mn>11</z:mn><z:mo stretchy="false">)</z:mo><z:mo stretchy="false">(</z:mo><z:mn>3</z:mn><z:mo stretchy="false">)</z:mo><z:mo stretchy="false">(</z:mo><z:mn>0</z:mn><z:mo stretchy="false">)</z:mo><z:mtext> </z:mtext><z:mtext> </z:mtext><z:mi>MeV</z:mi></z:math> for the <kb:math xmlns:kb="http://www.w3.org/1998/Math/MathML" display="inline"><kb:msup><kb:mi>K</kb:mi><kb:mo>*</kb:mo></kb:msup><kb:mo stretchy="false">(</kb:mo><kb:mn>892</kb:mn><kb:mo stretchy="false">)</kb:mo></kb:math> resonance and <ob:math xmlns:ob="http://www.w3.org/1998/Math/MathML" display="inline"><ob:mrow><ob:msub><ob:mrow><ob:mi>M</ob
{"title":"Physical-mass calculation of ρ(770) and K*(892) resonance parameters via ππ and Kπ scattering amplitudes from lattice QCD","authors":"Peter Boyle, Felix Erben, Vera Gülpers, Maxwell T. Hansen, Fabian Joswig, Michael Marshall, Nelson Pitanga Lachini, Antonin Portelli","doi":"10.1103/physrevd.111.054510","DOIUrl":"https://doi.org/10.1103/physrevd.111.054510","url":null,"abstract":"We present our study of the ρ</a:mi>(</a:mo>770</a:mn>)</a:mo></a:math> and <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:msup><e:mi>K</e:mi><e:mo>*</e:mo></e:msup><e:mo stretchy=\"false\">(</e:mo><e:mn>892</e:mn><e:mo stretchy=\"false\">)</e:mo></e:math> resonances from lattice quantum chromodynamics (QCD) employing domain-wall fermions at physical quark masses. We determine the finite-volume energy spectrum in various momentum frames and obtain phase-shift parametrizations via the Lüscher formalism and as a final step the complex resonance poles of the <i:math xmlns:i=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><i:mi>π</i:mi><i:mi>π</i:mi></i:math> and <k:math xmlns:k=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><k:mi>K</k:mi><k:mi>π</k:mi></k:math> elastic scattering amplitudes via an analytical continuation of the models. By sampling a large number of representative sets of underlying energy-level fits, we also assign a systematic uncertainty to our final results. This is a significant extension to data-driven analysis methods that have been used in lattice QCD to date, due to the two-step nature of the formalism. Our final pole positions, <m:math xmlns:m=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><m:mi>M</m:mi><m:mo>+</m:mo><m:mi>i</m:mi><m:mi mathvariant=\"normal\">Γ</m:mi><m:mo>/</m:mo><m:mn>2</m:mn></m:math>, with all statistical and systematic errors exposed, are <p:math xmlns:p=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><p:mrow><p:msub><p:mrow><p:mi>M</p:mi></p:mrow><p:mrow><p:msup><p:mrow><p:mi>K</p:mi></p:mrow><p:mrow><p:mo>*</p:mo></p:mrow></p:msup></p:mrow></p:msub><p:mo>=</p:mo><p:mn>893</p:mn><p:mo stretchy=\"false\">(</p:mo><p:mn>2</p:mn><p:mo stretchy=\"false\">)</p:mo><p:mo stretchy=\"false\">(</p:mo><p:mn>8</p:mn><p:mo stretchy=\"false\">)</p:mo><p:mo stretchy=\"false\">(</p:mo><p:mn>54</p:mn><p:mo stretchy=\"false\">)</p:mo><p:mo stretchy=\"false\">(</p:mo><p:mn>2</p:mn><p:mo stretchy=\"false\">)</p:mo><p:mtext> </p:mtext><p:mtext> </p:mtext><p:mi>MeV</p:mi></p:mrow></p:math> and <z:math xmlns:z=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><z:msub><z:mi mathvariant=\"normal\">Γ</z:mi><z:msup><z:mi>K</z:mi><z:mo>*</z:mo></z:msup></z:msub><z:mo>=</z:mo><z:mn>51</z:mn><z:mo stretchy=\"false\">(</z:mo><z:mn>2</z:mn><z:mo stretchy=\"false\">)</z:mo><z:mo stretchy=\"false\">(</z:mo><z:mn>11</z:mn><z:mo stretchy=\"false\">)</z:mo><z:mo stretchy=\"false\">(</z:mo><z:mn>3</z:mn><z:mo stretchy=\"false\">)</z:mo><z:mo stretchy=\"false\">(</z:mo><z:mn>0</z:mn><z:mo stretchy=\"false\">)</z:mo><z:mtext> </z:mtext><z:mtext> </z:mtext><z:mi>MeV</z:mi></z:math> for the <kb:math xmlns:kb=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><kb:msup><kb:mi>K</kb:mi><kb:mo>*</kb:mo></kb:msup><kb:mo stretchy=\"false\">(</kb:mo><kb:mn>892</kb:mn><kb:mo stretchy=\"false\">)</kb:mo></kb:math> resonance and <ob:math xmlns:ob=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><ob:mrow><ob:msub><ob:mrow><ob:mi>M</ob","PeriodicalId":20167,"journal":{"name":"Physical Review D","volume":"44 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143653779","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 : 2025-03-17DOI: 10.1103/physrevd.111.056020
Orkash Amat, Hong-Hao Fan, Suo Tang, Yong-Feng Huang, Bai-Song Xie
We have formulated a generalized two level model for studying the vacuum electron-positron pair production in strong classical background fields via slowly varying envelope approximation. It can provide momentum spectra with fully spin resolved components for all possible combined spin states of the particle and antiparticle simultaneously in multidimensional time-dependent electric fields. Moreover, we have also investigated the validity of the two level model for fermions (scalar particles) by comparing the results with those by equal-time Dirac-Heisenberg-Wigner (Feshbach-Villars-Heisenberg-Wigner) formalism in different regimes of pair creation, i.e., multiphoton and tunneling dominated mechanisms. It is found that the results are consistent with each other, indicating the good approximation of the two level model. In particular, in terms of the two level model, we found that the contribution of the particle momentum spectra is the greatest when the spin states of the particle and antiparticle are parallel with S=1. It is believed that by this two level model one can extend researches on pair production for more different background fields, such as a slowly varying spatial-temporal one. Significantly, we demonstrate that the generalized two level model is equivalent to the spin resolved quantum kinetic theory. In comparison to the equal-time Dirac-Heisenberg-Wigner and Feshbach-Villars-Heisenberg-Wigner methods, the two-level model is simpler and has the potential to deliver faster computational performance. Published by the American Physical Society2025
{"title":"Spin resolved momentum spectra for vacuum pair production via a generalized two level model","authors":"Orkash Amat, Hong-Hao Fan, Suo Tang, Yong-Feng Huang, Bai-Song Xie","doi":"10.1103/physrevd.111.056020","DOIUrl":"https://doi.org/10.1103/physrevd.111.056020","url":null,"abstract":"We have formulated a generalized two level model for studying the vacuum electron-positron pair production in strong classical background fields via slowly varying envelope approximation. It can provide momentum spectra with fully spin resolved components for all possible combined spin states of the particle and antiparticle simultaneously in multidimensional time-dependent electric fields. Moreover, we have also investigated the validity of the two level model for fermions (scalar particles) by comparing the results with those by equal-time Dirac-Heisenberg-Wigner (Feshbach-Villars-Heisenberg-Wigner) formalism in different regimes of pair creation, i.e., multiphoton and tunneling dominated mechanisms. It is found that the results are consistent with each other, indicating the good approximation of the two level model. In particular, in terms of the two level model, we found that the contribution of the particle momentum spectra is the greatest when the spin states of the particle and antiparticle are parallel with S</a:mi>=</a:mo>1</a:mn></a:math>. It is believed that by this two level model one can extend researches on pair production for more different background fields, such as a slowly varying spatial-temporal one. Significantly, we demonstrate that the generalized two level model is equivalent to the spin resolved quantum kinetic theory. In comparison to the equal-time Dirac-Heisenberg-Wigner and Feshbach-Villars-Heisenberg-Wigner methods, the two-level model is simpler and has the potential to deliver faster computational performance. <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":"24 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143635221","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 : 2025-03-17DOI: 10.1103/physrevd.111.063049
Garv Chauhan
The cosmic neutrino background (CνB) constitutes the last observable prediction of the standard cosmological model, which has yet to be detected directly. In this work, we show how the coherent scattering of neutrinos off dense neutron matter can lead to an additional cooling channel in neutron stars (NSs). We also include the effects of gravitational capture and boosting, but find that the cooling is efficient only in the presence of large overdensities. We further discuss the prediction of a boosted CνB flux on Earth from nearby NSs and the potential detection prospects in the case of a future nearby galactic supernova. Although currently these ideas do not offer any detection prospects, they can be used to constrain overdensities η≲1011–1014 on short length scales O(10km). We also discuss the impact of new physics scenarios, such as long-range forces, on NS cooling through the CνB. Published by the American Physical Society2025
{"title":"Neutron stars as a probe of the cosmic neutrino background","authors":"Garv Chauhan","doi":"10.1103/physrevd.111.063049","DOIUrl":"https://doi.org/10.1103/physrevd.111.063049","url":null,"abstract":"The cosmic neutrino background (C</a:mi>ν</a:mi>B</a:mi></a:mrow></a:math>) constitutes the last observable prediction of the standard cosmological model, which has yet to be detected directly. In this work, we show how the coherent scattering of neutrinos off dense neutron matter can lead to an additional cooling channel in neutron stars (NSs). We also include the effects of gravitational capture and boosting, but find that the cooling is efficient only in the presence of large overdensities. We further discuss the prediction of a boosted <e:math xmlns:e=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><e:mrow><e:mi mathvariant=\"normal\">C</e:mi><e:mi>ν</e:mi><e:mi mathvariant=\"normal\">B</e:mi></e:mrow></e:math> flux on Earth from nearby NSs and the potential detection prospects in the case of a future nearby galactic supernova. Although currently these ideas do not offer any detection prospects, they can be used to constrain overdensities <i:math xmlns:i=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><i:mi>η</i:mi><i:mo>≲</i:mo><i:msup><i:mn>10</i:mn><i:mn>11</i:mn></i:msup><i:mi>–</i:mi><i:msup><i:mn>10</i:mn><i:mn>14</i:mn></i:msup></i:math> on short length scales <k:math xmlns:k=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><k:mi mathvariant=\"script\">O</k:mi><k:mo stretchy=\"false\">(</k:mo><k:mn>10</k:mn><k:mtext> </k:mtext><k:mtext> </k:mtext><k:mi>km</k:mi><k:mo stretchy=\"false\">)</k:mo></k:math>. We also discuss the impact of new physics scenarios, such as long-range forces, on NS cooling through the <p:math xmlns:p=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><p:mrow><p:mi mathvariant=\"normal\">C</p:mi><p:mi>ν</p:mi><p:mi mathvariant=\"normal\">B</p:mi></p:mrow></p:math>. <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":"7 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143640048","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 : 2025-03-17DOI: 10.1103/physrevd.111.054019
Yan-Ke Chen, Liang-Zhen Wen, Lu Meng, Shi-Lin Zhu
We calculate the electromagnetic polarizabilities of the spin-12 singly heavy baryons in the heavy baryon chiral perturbation theory up to O(p3). We estimate the low-energy constants using the magnetic moments of singly charmed baryons from lattice QCD simulations and the experimental decay widths of Σc and Σc*. Our results indicate that the long-range chiral corrections make significant contributions to the polarizabilities. Additionally, the magnetic dipole transitions B6*→B6+γ also provide large contribution to the magnetic polarizabilities. Published by the American Physical Society2025
{"title":"Electromagnetic polarizabilities of the spin- 12 singly heavy baryons in heavy baryon chiral perturbation theory","authors":"Yan-Ke Chen, Liang-Zhen Wen, Lu Meng, Shi-Lin Zhu","doi":"10.1103/physrevd.111.054019","DOIUrl":"https://doi.org/10.1103/physrevd.111.054019","url":null,"abstract":"We calculate the electromagnetic polarizabilities of the spin-1</a:mn>2</a:mn></a:mfrac></a:math> singly heavy baryons in the heavy baryon chiral perturbation theory up to <c:math xmlns:c=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><c:mi mathvariant=\"script\">O</c:mi><c:mo stretchy=\"false\">(</c:mo><c:msup><c:mi>p</c:mi><c:mn>3</c:mn></c:msup><c:mo stretchy=\"false\">)</c:mo></c:math>. We estimate the low-energy constants using the magnetic moments of singly charmed baryons from lattice QCD simulations and the experimental decay widths of <h:math xmlns:h=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><h:msub><h:mi mathvariant=\"normal\">Σ</h:mi><h:mi>c</h:mi></h:msub></h:math> and <k:math xmlns:k=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><k:msubsup><k:mi mathvariant=\"normal\">Σ</k:mi><k:mi>c</k:mi><k:mo>*</k:mo></k:msubsup></k:math>. Our results indicate that the long-range chiral corrections make significant contributions to the polarizabilities. Additionally, the magnetic dipole transitions <n:math xmlns:n=\"http://www.w3.org/1998/Math/MathML\" display=\"inline\"><n:msubsup><n:mi mathvariant=\"script\">B</n:mi><n:mn>6</n:mn><n:mo>*</n:mo></n:msubsup><n:mo stretchy=\"false\">→</n:mo><n:msub><n:mi mathvariant=\"script\">B</n:mi><n:mn>6</n:mn></n:msub><n:mo>+</n:mo><n:mi>γ</n:mi></n:math> also provide large contribution to the magnetic polarizabilities. <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":"37 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143640046","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 : 2025-03-17DOI: 10.1103/physrevd.111.063045
Daniel J. Heimsoth, Rebecca Kowalski, Danielle H. Speller, Calvin W. Johnson, A. Baha Balantekin, Susan N. Coppersmith
Using tellurium dioxide as a target, we calculate uncertainties on 90% upper confidence limits of Galilean effective field theory (Galilean EFT) couplings to a weakly interacting massive particle (WIMP) dark matter candidate due to uncertainties in nuclear shell models. We find that these uncertainties in naturally occurring tellurium isotopes are comparable across the different Galilean EFT couplings to uncertainties in xenon, with some reaching over 100%. We also consider the effect these nuclear uncertainties have on estimates of the annual modulation of dark matter from these searches, finding that the uncertainties in the modulation amplitude are proportional to the nonmodulating upper confidence limit uncertainties. We also show that the determination of the modulation phase is insensitive to changes in the nuclear model for a given isotope. Published by the American Physical Society2025
{"title":"Uncertainties in tellurium-based dark matter searches stemming from nuclear structure uncertainties","authors":"Daniel J. Heimsoth, Rebecca Kowalski, Danielle H. Speller, Calvin W. Johnson, A. Baha Balantekin, Susan N. Coppersmith","doi":"10.1103/physrevd.111.063045","DOIUrl":"https://doi.org/10.1103/physrevd.111.063045","url":null,"abstract":"Using tellurium dioxide as a target, we calculate uncertainties on 90% upper confidence limits of Galilean effective field theory (Galilean EFT) couplings to a weakly interacting massive particle (WIMP) dark matter candidate due to uncertainties in nuclear shell models. We find that these uncertainties in naturally occurring tellurium isotopes are comparable across the different Galilean EFT couplings to uncertainties in xenon, with some reaching over 100%. We also consider the effect these nuclear uncertainties have on estimates of the annual modulation of dark matter from these searches, finding that the uncertainties in the modulation amplitude are proportional to the nonmodulating upper confidence limit uncertainties. We also show that the determination of the modulation phase is insensitive to changes in the nuclear model for a given isotope. <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":"40 1","pages":""},"PeriodicalIF":5.0,"publicationDate":"2025-03-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143635227","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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