The primordial neutrino asymmetry leave profound imprints on the evolution history of the universe, which can be constrained by cosmological observations, including Big Bang Nucleosynthesis (BBN), Cosmic Microwave Background (CMB), and Large-Scale Structure (LSS). We present comprehensive analysis on implications and constraints of the primordial neutrino asymmetry $xi_nu$, based on a precise treatment of neutrino decoupling by solving the complete (anti)neutrino quantum kinetic equations in the Closed-Time-Path formalism. The effective number of neutrinos $ N_{rm eff}$ and (anti)neutrino spectral distortions are calculated, and we find that the non-instantaneous decoupling correction is given by $delta N_{rm eff} = 0.0440 + 0.0102 , xi_nu^2$. Then we perform the state-of-the-art calculation for the abundance of light elements including (anti)neutrino spectral distortions, which indicate a positive asymmetry $0.032 leq xi_nu leq 0.052$ from EMPRESS data. The implications of the neutrino asymmetry for the CMB and LSS are studied in detail, and we find that the Baryon Acoustic Oscillations (BAO) are also significantly affected by $xi_nu$ in addition to the sum of neutrino masses. A combined analysis with EMPRESS BBN, Planck CMB and BOSS BAO data yields a tighter constraint $xi_nu = 0.024 pm 0.013$, which provides constraints on UV models capable of producing large asymmetries.
{"title":"Revisiting primordial neutrino asymmetries, spectral distortions and cosmological constraints with full neutrino transport","authors":"Yuan-Zhen Li, Jiang-Hao Yu","doi":"arxiv-2409.08280","DOIUrl":"https://doi.org/arxiv-2409.08280","url":null,"abstract":"The primordial neutrino asymmetry leave profound imprints on the evolution\u0000history of the universe, which can be constrained by cosmological observations,\u0000including Big Bang Nucleosynthesis (BBN), Cosmic Microwave Background (CMB),\u0000and Large-Scale Structure (LSS). We present comprehensive analysis on\u0000implications and constraints of the primordial neutrino asymmetry $xi_nu$,\u0000based on a precise treatment of neutrino decoupling by solving the complete\u0000(anti)neutrino quantum kinetic equations in the Closed-Time-Path formalism. The\u0000effective number of neutrinos $ N_{rm eff}$ and (anti)neutrino spectral\u0000distortions are calculated, and we find that the non-instantaneous decoupling\u0000correction is given by $delta N_{rm eff} = 0.0440 + 0.0102 , xi_nu^2$.\u0000Then we perform the state-of-the-art calculation for the abundance of light\u0000elements including (anti)neutrino spectral distortions, which indicate a\u0000positive asymmetry $0.032 leq xi_nu leq 0.052$ from EMPRESS data. The\u0000implications of the neutrino asymmetry for the CMB and LSS are studied in\u0000detail, and we find that the Baryon Acoustic Oscillations (BAO) are also\u0000significantly affected by $xi_nu$ in addition to the sum of neutrino masses.\u0000A combined analysis with EMPRESS BBN, Planck CMB and BOSS BAO data yields a\u0000tighter constraint $xi_nu = 0.024 pm 0.013$, which provides constraints on\u0000UV models capable of producing large asymmetries.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"60 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142223496","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We systematically study the 1D charmonium spin-triplet (with the $J^{PC}=1^{--}, 2^{--}, 3^{--}$) and spin-singlet (with the $J^{PC}=2^{-+}$) via the QCD sum rules in comparison with the present experimental results. More experimental data on the D-wave charmonium states will help us to unravel the mass spectrum of the charmonium states near the open-charm thresholds.
{"title":"Systematic analysis of the D-wave charmonium states with the QCD sum rules","authors":"Qi Xin, Zhi-Gang Wang","doi":"arxiv-2409.08051","DOIUrl":"https://doi.org/arxiv-2409.08051","url":null,"abstract":"We systematically study the 1D charmonium spin-triplet (with the\u0000$J^{PC}=1^{--}, 2^{--}, 3^{--}$) and spin-singlet (with the $J^{PC}=2^{-+}$)\u0000via the QCD sum rules in comparison with the present experimental results. More\u0000experimental data on the D-wave charmonium states will help us to unravel the\u0000mass spectrum of the charmonium states near the open-charm thresholds.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178490","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We study multi-component dark matter scenarios and the Galactic 511 keV $gamma$-ray emission line signal in the framework of a local, dark $U(1)_D$ extension of the Standard Model. A light vector dark matter particle associated with the dark $U(1)_D$ may decay and annihilate to electron-positron pairs. The produced positrons may in turn form positroniums that subsequently annihilate to two photons, accounting for the observed line signal of the Galactic 511 keV $gamma$-ray emission. Three scenarios are investigated. First, we consider the minimal $U(1)_D$ extension where a dark gauge boson and a dark Higgs boson are newly introduced to the particle content. As a second scenario, we consider WIMP-type dark matter with the introduction of an extra dark fermion which, in addition to the dark gauge boson, may contribute to the dark matter relic abundance. It is thus a multi-component dark matter scenario with a UV-complete dark $U(1)_D$ symmetry. In particular, the vector dark matter may account for a small fraction of the total dark matter relic abundance. Finally, we consider the scenario where the dark matter particles are of the FIMP-type. In this case, both the light vector and fermion dark matter particles may be produced via the freeze-in and super-WIMP mechanisms. Considering theoretical and observational constraints, we explore the allowed parameter space where the Galactic 511 keV $gamma$-ray line signal and the dark matter relic can both be explained. We also discuss possible observational signatures.
{"title":"Multi-component dark matter and Galactic 511 keV $γ$-ray emission","authors":"Sarif Khan, Jinsu Kim, Jongkuk Kim, Pyungwon Ko","doi":"arxiv-2409.07851","DOIUrl":"https://doi.org/arxiv-2409.07851","url":null,"abstract":"We study multi-component dark matter scenarios and the Galactic 511 keV\u0000$gamma$-ray emission line signal in the framework of a local, dark $U(1)_D$\u0000extension of the Standard Model. A light vector dark matter particle associated\u0000with the dark $U(1)_D$ may decay and annihilate to electron-positron pairs. The\u0000produced positrons may in turn form positroniums that subsequently annihilate\u0000to two photons, accounting for the observed line signal of the Galactic 511 keV\u0000$gamma$-ray emission. Three scenarios are investigated. First, we consider the\u0000minimal $U(1)_D$ extension where a dark gauge boson and a dark Higgs boson are\u0000newly introduced to the particle content. As a second scenario, we consider\u0000WIMP-type dark matter with the introduction of an extra dark fermion which, in\u0000addition to the dark gauge boson, may contribute to the dark matter relic\u0000abundance. It is thus a multi-component dark matter scenario with a UV-complete\u0000dark $U(1)_D$ symmetry. In particular, the vector dark matter may account for a\u0000small fraction of the total dark matter relic abundance. Finally, we consider\u0000the scenario where the dark matter particles are of the FIMP-type. In this\u0000case, both the light vector and fermion dark matter particles may be produced\u0000via the freeze-in and super-WIMP mechanisms. Considering theoretical and\u0000observational constraints, we explore the allowed parameter space where the\u0000Galactic 511 keV $gamma$-ray line signal and the dark matter relic can both be\u0000explained. We also discuss possible observational signatures.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178491","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Kyu Jung Bae, Jinn-Ouk Gong, Dong-Won Jung, Kang Young Lee, Chaehyun Yu, Chan Beom Park
We study the phenomenology of the charged Higgs boson, $H^pm$,appearing in the fermionic dark matter model mediated by the dark $Z$ boson. This model is in favor of the light dark $Z$ boson, $Z'$, and the light additional neutral Higgs boson, $h$. We find that $H^pm to W^pm h$ and the $H^pm to W^pm Z'$ are dominant decay channels. Thus the promising final states are trilepton signals, $e mu mu$ or $mu mu mu$ following $Z' to mu^+ mu^-$ decays and leptonic decays of the $W^pm$ boson. The charged Higgs boson will be produced from the top quark decays $t to b H^pm$ following $t bar{t}$ production, if $H^pm$ is light. Whereas $H^pm$ is heavier than the top quark, the dominant production processes are associated productions with either $Z'$ or $h$, $pp to W^star to H^pm h$ and $pp to W^star to H^pm Z'$. We explore the discovery potential of the charged Higgs boson at the LHC. We also discuss the implications of dark matter in relation with the charged Higgs phenomenology.
我们研究了由暗Z$玻色子介导的费米暗物质模型中出现的带电希格斯玻色子$H^pm$的现象学。这个模型支持轻的暗Z$玻色子$Z'$和轻的附加中性希格斯玻色子$h$。我们发现$H^pm to W^pm h$和$H^pm to W^pm Z'$是主要的衰变通道。因此，在 $Z' to mu^+ mu^-$ 衰变和 $W^pm$ 玻色子的leptonic 衰变之后，有希望的终态是三重子信号，即 $e mu mu$ 或 $mu mu mu$ 。如果$H^pm$是轻的，那么带电的希格斯玻色子将从顶夸克衰变$t to b H^pm$产生。而$H^pm$比顶夸克重，主要的产生过程是与$Z'$或$h$相关的产生，即$ppto W^starto Hpm h$和$pp to W^starto H^pm Z'$。我们探讨了在大型强子对撞机上发现带电希格斯玻色子的可能性。我们还讨论了暗物质对带电希格斯现象学的影响。
{"title":"Charged Higgs Boson Phenomenology in the Dark Z mediated Fermionic Dark Matter Model","authors":"Kyu Jung Bae, Jinn-Ouk Gong, Dong-Won Jung, Kang Young Lee, Chaehyun Yu, Chan Beom Park","doi":"arxiv-2409.07688","DOIUrl":"https://doi.org/arxiv-2409.07688","url":null,"abstract":"We study the phenomenology of the charged Higgs boson, $H^pm$,appearing in\u0000the fermionic dark matter model mediated by the dark $Z$ boson. This model is\u0000in favor of the light dark $Z$ boson, $Z'$, and the light additional neutral\u0000Higgs boson, $h$. We find that $H^pm to W^pm h$ and the $H^pm to W^pm Z'$\u0000are dominant decay channels. Thus the promising final states are trilepton\u0000signals, $e mu mu$ or $mu mu mu$ following $Z' to mu^+ mu^-$ decays and\u0000leptonic decays of the $W^pm$ boson. The charged Higgs boson will be produced\u0000from the top quark decays $t to b H^pm$ following $t bar{t}$ production, if\u0000$H^pm$ is light. Whereas $H^pm$ is heavier than the top quark, the dominant\u0000production processes are associated productions with either $Z'$ or $h$, $pp\u0000to W^star to H^pm h$ and $pp to W^star to H^pm Z'$. We explore the\u0000discovery potential of the charged Higgs boson at the LHC. We also discuss the\u0000implications of dark matter in relation with the charged Higgs phenomenology.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178507","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Within the framework of symmetric teleparallel $fleft( Qright) $-gravity for a connection defined in the non-coincidence gauge we derive the Wheeler-DeWitt equation of quantum cosmology. Because the gravitational field equation in $fleft( Qright) $-gravity admits a minisuperspace description the Wheeler-DeWitt equation is a single inhomogeneous partial differential equations. We assume the power-law $fleft( Qright) =f_{0}Q^{mu}$ model and with the application of linear quantum observables we calculate the wavefunction of the universe. Finally, we investigate the effects of the quantum correction terms in the semi-classical limit.
{"title":"Semi-Classical limit and quantum corrections in noncoincidence power-law $f(Q)$-Cosmology","authors":"Andronikos Paliathanasis","doi":"arxiv-2409.07755","DOIUrl":"https://doi.org/arxiv-2409.07755","url":null,"abstract":"Within the framework of symmetric teleparallel $fleft( Qright) $-gravity\u0000for a connection defined in the non-coincidence gauge we derive the\u0000Wheeler-DeWitt equation of quantum cosmology. Because the gravitational field\u0000equation in $fleft( Qright) $-gravity admits a minisuperspace description the\u0000Wheeler-DeWitt equation is a single inhomogeneous partial differential\u0000equations. We assume the power-law $fleft( Qright) =f_{0}Q^{mu}$ model and\u0000with the application of linear quantum observables we calculate the\u0000wavefunction of the universe. Finally, we investigate the effects of the\u0000quantum correction terms in the semi-classical limit.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"60 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178497","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Rouzbeh Allahverdi, Adrian Thompson, Mohammadreza Zakeri
Rare processes in laboratory and within astrophysical environments can be highly sensitive probes of baryon-number violating interactions at the TeV scale. We demonstrate the power of neutron stars to constrain baryon number violation by considering a minimal extension of the standard model involving a TeV-mass scalar mediator and a GeV scale Majorana fermion $psi$. We find that a $Delta B = 2$ mass-loss process in binary pulsar systems via $n to gamma psi$ and the subsequent scattering $psi n to pi^- K^+$ places stringent constraints on the model parameter space. These limits will become much stronger, due to the possibility of $Lambda rightarrow gamma psi$ decays at the tree level, if the neutron star equation of state is hyperonic. We compare these constraints with ongoing and future collider experiments, $n-bar{n}$ oscillations, and dinucleon decay searches at future large-scale neutrino experiments, finding that the binary pulsars bounds on couplings are significantly tighter for specific flavor combinations.
实验室和天体物理环境中的罕见过程可以成为TeV尺度重子数违反相互作用的高灵敏探测器。我们通过考虑标准模型的一个最小扩展（涉及一个TeV质量的标量中介和一个GeV尺度的马约拉纳费米子$psi$），证明了中子星在约束重子数违反方面的能力。我们发现，双脉冲星系统中通过 $n to gammapsi$ 和随后的散射 $psi n to pi^- K^+$ 的 $Delta B = 2$ 质量损失过程对模型参数空间施加了严格的限制。如果中子星的状态方程是超音速的，那么由于树级上可能存在$Lambda rightarrow gamma psi$衰变，这些限制就会变得更强。我们将这些约束与正在进行的和未来的对撞机实验、$n-bar{n}$振荡以及未来大规模中微子实验中的二核子衰变搜索进行了比较，发现双脉冲星的耦合约束在特定的味道组合中明显更紧。
{"title":"Insights from Binary Pulsars and Laboratories into Baryon Number Violation: Implications for GeV Dark Matter","authors":"Rouzbeh Allahverdi, Adrian Thompson, Mohammadreza Zakeri","doi":"arxiv-2409.08178","DOIUrl":"https://doi.org/arxiv-2409.08178","url":null,"abstract":"Rare processes in laboratory and within astrophysical environments can be\u0000highly sensitive probes of baryon-number violating interactions at the TeV\u0000scale. We demonstrate the power of neutron stars to constrain baryon number\u0000violation by considering a minimal extension of the standard model involving a\u0000TeV-mass scalar mediator and a GeV scale Majorana fermion $psi$. We find that\u0000a $Delta B = 2$ mass-loss process in binary pulsar systems via $n to gamma\u0000psi$ and the subsequent scattering $psi n to pi^- K^+$ places stringent\u0000constraints on the model parameter space. These limits will become much\u0000stronger, due to the possibility of $Lambda rightarrow gamma psi$ decays at\u0000the tree level, if the neutron star equation of state is hyperonic. We compare\u0000these constraints with ongoing and future collider experiments, $n-bar{n}$\u0000oscillations, and dinucleon decay searches at future large-scale neutrino\u0000experiments, finding that the binary pulsars bounds on couplings are\u0000significantly tighter for specific flavor combinations.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"80 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178488","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The expected improvements in the precision of inflationary physics observables including the scalar spectral index $n_{s}$ and the tensor-to-scalar ratio $r$ will reveal more than just the viability of a particular model of inflation. In the presence of a curvaton field $chi$, supposedly dead models of inflation can be resurrected as these observables are affected by curvaton perturbations. For currently successful models, improved constraints will enable us to constrain the properties of extra decaying scalar degrees of freedom produced during inflation. In this work, we demonstrate these diverse uses of a curvaton field with the most recent constraints on ($n_{s},r$) and two exemplary inflation models, the Starobinsky model, and a model of new inflation. Our analysis invokes three free parameters: the curvaton mass $m_{chi}$, its decay rate $Gamma_{chi}$ the reheating temperature $T_{rm RH}$ produced by inflaton decays. We systematically analyze possible post-inflationary era scenarios of a curvaton field. By projecting the most recent CMB data on ($n_{s},r$) into this parameter space, we can either set constraints on the curvaton parameters from successful models of inflation (so that the success is not spoiled) or determine the parameters which are able to save a model for which $n_{s}$ is predicted to be below the experimental data. We emphasize that the initial value of $langle chi^2 rangle propto H^4/m_chi^2$ produced during inflation is determined from a stochastic approach and thus not a free parameter in our analysis. We also investigate the production of local non-Gaussianity $f_{NL}^{(rm loc)}$ and apply current CMB constraints to the parameter space. Intriguingly, we find that a large value of $f_{NL}^{(rm loc)}$ of $mathcal{O}(1)$ can be produced for both of the two representative inflation models.
{"title":"The Role of the Curvaton Post-Planck","authors":"Gongjun Choi, Wenqi Ke, Keith A. Olive","doi":"arxiv-2409.08279","DOIUrl":"https://doi.org/arxiv-2409.08279","url":null,"abstract":"The expected improvements in the precision of inflationary physics\u0000observables including the scalar spectral index $n_{s}$ and the\u0000tensor-to-scalar ratio $r$ will reveal more than just the viability of a\u0000particular model of inflation. In the presence of a curvaton field $chi$,\u0000supposedly dead models of inflation can be resurrected as these observables are\u0000affected by curvaton perturbations. For currently successful models, improved\u0000constraints will enable us to constrain the properties of extra decaying scalar\u0000degrees of freedom produced during inflation. In this work, we demonstrate\u0000these diverse uses of a curvaton field with the most recent constraints on\u0000($n_{s},r$) and two exemplary inflation models, the Starobinsky model, and a\u0000model of new inflation. Our analysis invokes three free parameters: the\u0000curvaton mass $m_{chi}$, its decay rate $Gamma_{chi}$ the reheating\u0000temperature $T_{rm RH}$ produced by inflaton decays. We systematically analyze\u0000possible post-inflationary era scenarios of a curvaton field. By projecting the\u0000most recent CMB data on ($n_{s},r$) into this parameter space, we can either\u0000set constraints on the curvaton parameters from successful models of inflation\u0000(so that the success is not spoiled) or determine the parameters which are able\u0000to save a model for which $n_{s}$ is predicted to be below the experimental\u0000data. We emphasize that the initial value of $langle chi^2 rangle propto\u0000H^4/m_chi^2$ produced during inflation is determined from a stochastic\u0000approach and thus not a free parameter in our analysis. We also investigate the\u0000production of local non-Gaussianity $f_{NL}^{(rm loc)}$ and apply current CMB\u0000constraints to the parameter space. Intriguingly, we find that a large value of\u0000$f_{NL}^{(rm loc)}$ of $mathcal{O}(1)$ can be produced for both of the two\u0000representative inflation models.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142223497","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Peter W. Graham, Harikrishnan Ramani, Samuel S. Y. Wong
While much supersymmetric WIMP parameter space has been ruled out, one remaining important candidate is Higgsino dark matter. The Higgsino can naturally realize the ``inelastic dark matter" scenario, where the scattering off a nucleus occurs between two nearly-degenerate states, making it invisible to WIMP direct detection experiments if the splitting is too large to be excited. It was realized that a ``luminous dark matter" detection process, where the Higgsino upscatters in the Earth and subsequently decays into a photon in a large neutrino detector, offers the best sensitivity to such a scenario. We consider the possibility of adding a large volume of a heavy element, such as Pb or U, around the detector. We also consider the presence of U and Th in the Earth itself, and the effect of an enhanced high-velocity tail of the dark matter distribution due to the presence of the Large Magellanic Cloud. These effects can significantly improve the sensitivity of detectors such as JUNO, SNO+, and Borexino, potentially making it possible in the future to cover much of the remaining parameter space for this classic SUSY WIMP dark matter.
{"title":"Enhancing Direct Detection of Higgsino Dark Matter","authors":"Peter W. Graham, Harikrishnan Ramani, Samuel S. Y. Wong","doi":"arxiv-2409.07768","DOIUrl":"https://doi.org/arxiv-2409.07768","url":null,"abstract":"While much supersymmetric WIMP parameter space has been ruled out, one\u0000remaining important candidate is Higgsino dark matter. The Higgsino can\u0000naturally realize the ``inelastic dark matter\" scenario, where the scattering\u0000off a nucleus occurs between two nearly-degenerate states, making it invisible\u0000to WIMP direct detection experiments if the splitting is too large to be\u0000excited. It was realized that a ``luminous dark matter\" detection process,\u0000where the Higgsino upscatters in the Earth and subsequently decays into a\u0000photon in a large neutrino detector, offers the best sensitivity to such a\u0000scenario. We consider the possibility of adding a large volume of a heavy\u0000element, such as Pb or U, around the detector. We also consider the presence of\u0000U and Th in the Earth itself, and the effect of an enhanced high-velocity tail\u0000of the dark matter distribution due to the presence of the Large Magellanic\u0000Cloud. These effects can significantly improve the sensitivity of detectors\u0000such as JUNO, SNO+, and Borexino, potentially making it possible in the future\u0000to cover much of the remaining parameter space for this classic SUSY WIMP dark\u0000matter.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"12 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178493","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Significant efforts have been made in recent years to measure the properties of charmed baryons. In this work, we study the $Xi_{c}'$ and $Omega_{c}$ baryons in the relativistic flux tube model with a quark-diquark picture of a baryon. The modified Regge relation between mass and angular momentum is used to predict the spin-average masses. The spin-dependent interactions are also included to compute the spin-dependent splitting. We calculate the masses of states belonging to the $1F$-wave and $1G$-wave of $Xi_{c}'$ and $Omega_{c}$ baryons, which are not yet detected experimentally. Our mass predictions can offer valuable insights to experimental facilities in their search to discover the higher excited states of $Xi_{c}'$ and $Omega_{c}$ baryons.
{"title":"Masses of higher excited states of $Ξ_{c}'$ and $Ω_{c}$ baryons","authors":"Pooja Jakhad, Juhi Oudichhya, Ajay Kumar Rai","doi":"arxiv-2409.07789","DOIUrl":"https://doi.org/arxiv-2409.07789","url":null,"abstract":"Significant efforts have been made in recent years to measure the properties\u0000of charmed baryons. In this work, we study the $Xi_{c}'$ and $Omega_{c}$\u0000baryons in the relativistic flux tube model with a quark-diquark picture of a\u0000baryon. The modified Regge relation between mass and angular momentum is used\u0000to predict the spin-average masses. The spin-dependent interactions are also\u0000included to compute the spin-dependent splitting. We calculate the masses of\u0000states belonging to the $1F$-wave and $1G$-wave of $Xi_{c}'$ and $Omega_{c}$\u0000baryons, which are not yet detected experimentally. Our mass predictions can\u0000offer valuable insights to experimental facilities in their search to discover\u0000the higher excited states of $Xi_{c}'$ and $Omega_{c}$ baryons.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"56 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178492","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We propose a new channel to search for millicharged particles at the future Super Tau Charm Facility (STCF) via mono-$pi^0$ signature. For the first time, we compute the mono-$pi^0$ signal events at the future STCF due to millicharged particle production, as well as due to standard model irreducible/reducible backgrounds. By utilizing the assumed 20 ab$^{-1}$ luminosity for each running energy with $sqrt{s}= 2$ GeV, 4 GeV and 7 GeV, we derive the corresponding upper limits on millicharge, respectively. Via mono-$pi^0$ searches at the future STCF with $sqrt{s}=2$ GeV, the upper limits on millicharge can be improved than ArgoNeuT when the mass of millicharged particle is less than about 500 MeV, but are not very competitive compared to a latest derivation from a past BEBC experiment and a new SENSEI experiment. Regardless, the mono-$pi^0$ searches could be an important complement to investigate the invisible particles, such as dark matter.
{"title":"Can millicharge be probed at future Super Tau Charm Facility via mono-$π^0$ searches?","authors":"Yu Zhang","doi":"arxiv-2409.08129","DOIUrl":"https://doi.org/arxiv-2409.08129","url":null,"abstract":"We propose a new channel to search for millicharged particles at the future\u0000Super Tau Charm Facility (STCF) via mono-$pi^0$ signature. For the first time,\u0000we compute the mono-$pi^0$ signal events at the future STCF due to\u0000millicharged particle production, as well as due to standard model\u0000irreducible/reducible backgrounds. By utilizing the assumed 20 ab$^{-1}$\u0000luminosity for each running energy with $sqrt{s}= 2$ GeV, 4 GeV and 7 GeV, we\u0000derive the corresponding upper limits on millicharge, respectively. Via\u0000mono-$pi^0$ searches at the future STCF with $sqrt{s}=2$ GeV, the upper\u0000limits on millicharge can be improved than ArgoNeuT when the mass of\u0000millicharged particle is less than about 500 MeV, but are not very competitive\u0000compared to a latest derivation from a past BEBC experiment and a new SENSEI\u0000experiment. Regardless, the mono-$pi^0$ searches could be an important\u0000complement to investigate the invisible particles, such as dark matter.","PeriodicalId":501067,"journal":{"name":"arXiv - PHYS - High Energy Physics - Phenomenology","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178489","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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