We study the new $Z'$ boson as a portal for the production of Higgs bosons $h_0$ and $H_0$ predicted by the Bestest Little Higgs Model through Higgs-strahlung processes $\mu^+\mu^- \to (Z, Z') \to Zh_0, ZH_0$ . We focus on the resonant and nonresonant effects of the $Zh_0, ZH_0$ signals. In our analysis, we consider the center-of-mass energies of $\sqrt{s}=3, 4, 6, 10, 30$ TeV and integrated luminosities of ${\cal{L}}=2, 4, 6, 10, 30$ ${ {\rm{ab}}^{-1}}$ projected for a future muon collider. The possibility of performing precision measurements for Higgs bosons $h_0$ and $H_0$ is very promising for the future muon collider. Furthermore, our results may be useful to the High Energy Physics community. Complementarily, we generate and provide the Feynman rules necessary for studying processes $\mu^+\mu^- \to (Z, Z') \to Zh_0, ZH_0$ .

J.M. Martínez-Martínez

A. Gutiérrez-Rodríguez

E. Cruz-Albaro

M.A. Hernández-Ruíz

New $\textit{Z}$' boson of the bestest little Higgs model as a portal to signatures of Higgs bosons $\textit{h}$ $_{0}$ and $\textit{H}$ $_{0}$ at the future muon collider

The so-called metastability bound on the Higgs mass suggests that the smallness of the Higgs mass may be a by-product of the metastability of the electroweak vacuum. A significantly strong bound requires new physics capable of lowering the scale where the Higgs quartic coupling turns negative through renormalization group effects, without destabilizing the electroweak vacuum entirely. We analyze in this context the low-scale Majoron model of neutrino masses, which automatically contains two key elements for a viable scenario: heavy fermions to lower the instability scale and a extended scalar sector to stabilize the potential and achieve realistic lifetimes for the electroweak vacuum. We show how the metastability bound can be generalized to theories with multiple scalars and present an efficient way of calculating the tunneling rate in such potentials. We also demonstrate that FCC will probe regions of the parameter space relevant for metastability: large regions of the fermionic sector at FCC-ee and some reach to the scalar sector at FCC-hh.

Spain

V. Enguita

B. Gavela

United States

T. Steingasser

Higgs near-criticality at future colliders

It is a long-standing puzzle why the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi>C</mi><mi>P</mi></mrow></math> violation (CPV) in the baryon system has not yet been definitively established as in the meson one. We demonstrate that individual partial-wave CPV in the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi mathvariant="normal">Λ</mi><mi>b</mi></msub><mo stretchy="false">→</mo><mi>p</mi><msup><mi>π</mi><mo>−</mo></msup></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>p</mi><msup><mi>K</mi><mo>−</mo></msup></math> decays can exceed 10%, but the destruction between the partial waves (the suppression by the small partial-wave weight) results in a small net direct CPV in the former (the latter) as measured currently. Our finding highlights the different dynamics responsible for CPVs in baryon and meson decays. We propose to probe the CPV observables associated with the angular distributions of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi mathvariant="normal">Λ</mi></mrow><mrow><mi>b</mi></mrow></msub><mo stretchy="false">→</mo><mi>p</mi><msub><mrow><mi>a</mi></mrow><mrow><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>1260</mn><mo stretchy="false">)</mo></mrow></math>, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi>p</mi><msub><mrow><mi>K</mi></mrow><mrow><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>1270</mn><mo stretchy="false">)</mo></mrow></math> decay products, which are large enough for being identified experimentally.

China

Jia-Jie Han

Ji-Xin Yu

Ya Li

Hsiang-nan Li

Jian-Peng Wang

Zhen-Jun Xiao

Fu-Sheng Yu

Establishing <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>C</mi><mi>P</mi></math> Violation in <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>b</mi></math>-Baryon Decays

I present a highly efficient integration method for scattering calculations, and a “partial rate matrix” that encodes the scattering rate as a function of the SO(3) orientation of the detector. This replaces the original multidimensional rate integral with a simple exercise in vector multiplication, speeding up the rate calculation by a factor of around <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>10</mn><mn>8</mn></msup></math>. I include a scheme to fully factorize the dark matter particle model, its astrophysical velocity distribution, and the properties of the target material from each other, enabling efficient calculation of the partial rate matrix even in studies comparing large sets of these input functions. This is now the only sensible way to evaluate the dark matter scattering rate in anisotropic detector materials. It is straightforward to generalize this method to other difficult but linear problems.

Benjamin Lillard

Partial Rate Matrix for Dark Matter Scattering

Neutrino telescopes, including IceCube, can detect galactic supernova events by observing the collective rise in photomultiplier count rates with a subsecond time resolution. Leveraging precise timing, we demonstrate for the first time the ability of neutrino telescopes to explore new weakly coupled states emitted from supernovae and subsequently decaying to neutrinos. Our approach utilizes publicly available packages, asteria and snewpy, for simulating detector responses and parametrizing neutrino fluxes originating from the standard model and new physics. We present results for two beyond-the-standard model scenarios and introduce the tool developed for testing a diverse range of new physics models.

Carlos A. Argüelles

Vedran Brdar

Belgium

Jeffrey Lazar

Ying-Ying Li

Supernovae Time Profiles as a Probe of New Physics at Neutrino Telescopes

A new integration method drastically improves the efficiency of the dark matter direct detection calculation. In this work I introduce a complete, orthogonal basis of spherical wavelet-harmonic functions, designed for the new vector space integration method. This factorizes the numeric calculation into a “vector” that depends only on the astrophysical velocity distribution; a second vector, depending only on the detector form factor; and a scattering matrix defined on the basis functions, which depends on the details of the dark matter (DM) particle model (e.g. its mass). For common spin-independent DM–Standard Model interactions, this scattering matrix can be evaluated analytically in the wavelet-harmonic basis. This factorization is particularly helpful for the more complicated analyses that have become necessary in recent years, especially those involving anisotropic detector materials or more realistic models of the local DM velocity distribution. With the new method, analyses studying large numbers of detector orientations and DM particle models can be performed more than 10 million times faster. This paper derives several analytic results for the spherical wavelets, including an extrapolation in the space of wavelet coefficients, and a generalization of the vector space method to a much broader class of linear functional integrals. Both results are highly relevant outside the field of DM direct detection.

Wavelet-harmonic integration methods

We present static axially symmetric fluid distributions not producing gravitational field outside their boundaries (i.e. fluid sources which match smoothly on the boundary surface to Minkowski space–time). These solutions provide further examples of ghost stars. A specific model is fully described, and its physical and geometrical properties are analyzed in detail. This includes the multipole moment structure of the source and its complexity factors, both of which vanish for our solution.

L. Herrera

J. Hernández–Pastora

J. Ospino

Venezuela

A. Prisco

Axially symmetric ghost stars

We study the $$\Lambda _{b}\rightarrow \Lambda _{c}\bar{D}^{0}K^{-}$$ and $$\Lambda _{b}\rightarrow \Lambda _{c}D^{-}\bar{K}^{0}$$ decays which proceed via a Cabibbo and $$N_c$$ favored process of external emission, and we determine the $$\bar{D}^{0}K^{-}$$ and $$D^{-}\bar{K}^{0}$$ mass distributions close to the $$\bar{D} \bar{K}$$ threshold. For this, we use the tree level contribution plus the rescattering of the meson-meson components, using the extension of the local hidden gauge approach to the charm sector that produces the $$D^*_{s0}(2317)$$ resonance. We observe a large enhancement of the mass distributions close to threshold due to the presence of this resonance below threshold. Next we undertake the inverse problem of extracting the maximum information on the interaction of the $$\bar{D} \bar{K}$$ channels from these distributions, and using the resampling method we find that from these data one can obtain precise values of the scattering lengths and effective ranges, the existence of an $$I=0$$ bound state with a precision of about $$4 \;\mathrm MeV$$ in the mass, plus the $$\bar{D} \bar{K}$$ molecular probability of this state with reasonable precision. Given the fact that the $$\Lambda _{b}\rightarrow \Lambda _{c}\bar{D}^{0}K^{-}$$ decay is already measured by the LHCb collaboration, it is expected that in the next runs with more statistics of the decay, these mass distributions can be measured with precision and the method proposed here can be used to determine the nature of the $$D^*_{s0}(2317)$$ , which is still an issue of debate.

Hai-Peng Li

Wei-Hong Liang

Chu-Wen Xiao

Ju-Jun Xie

Eulogio Oset

Determination of the binding and $\textit{DK}$ probability of the $$D^{*}_{s0}(2317)$$ from the $$(\bar{D}\bar{K})^-$$ mass distributions in $$\Lambda _{b}\rightarrow \Lambda _{c} (\bar{D}\bar{K})^-$$ decays

In this paper, we would like to examine whether the Sáez–Ballester theory admits stable and attractive Bianchi type I inflationary solutions in the presence of a non-minimal coupling between scalar and vector fields such as $$f^2(\phi )F_{\mu \nu }F^{\mu \nu }$$ . As a result, such a solution will be shown to exist within this theory for a suitable setup of fields. Interestingly, the considered Sáez–Ballester theory can be shown to be equivalent to the standard scalar–vector theory via a suitable field redefinition. This means that the obtained solution can be reduced to that derived in an original anisotropic inflation model proposed by Kanno, Soda, and Watanabe. Consequently, the corresponding tensor-to-scalar ratio of this solution turns out to be higher than the latest observational value of the Planck satellite (Planck 2018) due to the fact that $$c_s$$ , the corresponding speed of sound of scalar perturbations of the Sáez–Ballester theory, turns out to be one. This result indicates an important hint that the speed of sound, $$c_s$$ , could play an important role in making the corresponding non-canonical anisotropic inflation cosmologically viable in the light of the Planck 2018 data. To be more specific, we will point out that any modifications of the Sáez–Ballester theory having $$c_s \sim 0.1$$ will have a great potential to be highly consistent with the Planck 2018 data. For heuristic reasons, a simple modified version of the Sáez–Ballester theory will be proposed as a specific demonstration. As a result, we will show that this modified model admits an anisotropic power-law inflationary solution as expected.

Vietnam

Tuan Do

Phung Dong

Duy Nguyen

India

J. Singh

Anisotropic power-law inflation for the Sáez–Ballester theory non-minimally coupled to a vector field

It is generally believed that quantum entanglement in the maximally entangled states is greater than quantum entanglement in the non-maximally entangled states under a relativistic setting. In this paper, we study quantum entanglement for four different types of Bell-like states of the fermionic modes near the event horizon of a Schwarzschild black hole. It is interesting to find that quantum entanglement in the maximally entangled states is less than quantum entanglement in the non-maximally entangled states in Schwarzschild spacetime. From the perspective of quantum resources, the non-maximally entangled states may have more advantages in curved spacetime compared to the maximally entangled states. This is obviously different from the conclusions in previous paper. For two types of Bell-like states, quantum entanglement suffers sudden death under the Hawking effect of the black hole, and for the other two types of Bell-like states, quantum entanglement can exist forever regardless of the Hawking temperature. Therefore, we should choose appropriate types of Bell-like states to handle relativistic quantum information tasks.

Shu-Min Wu

Si-Han Li

Do maximally entangled states always have an advantage over non-maximally entangled states in Schwarzschild black hole?