Energy Interaction Models Research Articles

Advanced cycling ageing-driven circular economy with E-mobility-based energy sharing and lithium battery cascade utilisation in a district community

Electrochemical storage technologies are essential for transformation towards electrification in both building and transportation sectors. The high cost, intensified carbon density and performance ageing of electrochemical batteries prevent its sustainable applications. Many studies have explored the battery circular economy based on reusing retired EV batteries with economic and environmental competitiveness. However, few studies combine battery circular economy with E-mobility-based interactive renewable energy sharing network for sustainability, together with comprehensive considerations on dynamic battery performance and degradation. In this study, a building-vehicle energy interaction model and a battery circular economy model were developed to simulate the process of reusing retired EV batteries. Considering the inconsistency in the carbon intensity of battery operation, manufacturing and recycling phases, a lifecycle battery carbon intensity criterion is proposed to quantify the lifetime carbon of batteries, and assess the decarbonisation capability of different renewable sources, battery reusing and V2B/B2V interaction, respectively. Results show that reusing retired batteries from EVs to buildings can improve the demand coverage ratio (DCR) from 0.480 to 0.504 and the renewable penetration ratio (RPR) from 0.502 to 0.531, respectively. Furthermore, the battery carbon intensity cannot be offset unless both renewables and reused batteries are integrated. The case study demonstrates the decrease of battery carbon intensity from 1284.57 kg CO2,e/kWh to −720.79 kg CO2,e/kWh with renewable and reused batteries. Research results can provide innovative battery circular economy frameworks for electrification transformation, decarbonisation and sustainable development.

Distribution grid electrical performance and emission analysis of combined cooling, heating and power (CCHP)-photovoltaic (PV)-based data center and residential customers

As the number of data centers is increasing worldwide, there are concerns about their growing electricity demand on power grids and its impact on the environment. These concerns can be mitigated at the urban scale by utilizing the waste heat generated by data centers and multi-energy hub integration. Using Combined Cooling, Heating, and Power (CCHP) and Photovoltaic (PV) systems within a data center, in combination with district energy network connections, can create energy interactions with residential customers in a multi-energy hub. However, connecting large energy consumers and distributed energy systems to the electrical distribution grid presents challenges due to the conventional design of the power grid with unidirectional electricity flow. There is a lack of understanding about the grid impact of data centers with multi-energy systems regarding electrical performance parameters, energy demand, and emissions. To address these open issues, we developed an hourly energy interaction model that includes a CCHP-PV-based data center and residential customers. In addition, the CCHP-PV-based data center was operated with a cost-optimized energy scheduling. We conducted six case studies to distinguish the specific effects of CCHP, PV, and district energy network connections. The model takes into account hourly outdoor temperatures, energy prices, and varying energy demands to capture the seasonal impact on electrical performance parameters and energy results. From an energy and environmental perspective, CCHP-PV systems can eliminate the data center's electricity demand from the grid, reduce residential energy demand, and decrease carbon dioxide equivalent emissions. This cleaner production and energy exchange further support the United Nations Sustainable Development goals. The experimental results showed a 43% reduction in power loss in the distribution grid and helped the data center's main electrical bus and residential bus against the voltage drop phenomenon. The CCHP-PV-based data center with district heating and cooling connection reduced the peak hour electricity demand on the grid by 39% and annual electricity consumption from the grid by 66%. Furthermore, Greenhouse Gas Protocols (GHG) Scope-2 emissions associated with the data center's grid electricity consumption and only residential electricity consumption were reduced by 77% and 36%, respectively.

Electron-beam energy reconstruction for neutrino oscillation measurements.

Neutrinos exist in one of three types or 'flavours'-electron, muon and tau neutrinos-and oscillate from one flavour to another when propagating through space. This phenomena is one of the few that cannot be described using the standard model of particle physics (reviewed in ref. 1), and so its experimental study can provide new insight into the nature of our Universe (reviewed in ref. 2). Neutrinos oscillate as a function of their propagation distance (L) divided by their energy (E). Therefore, experiments extract oscillation parameters by measuring their energy distribution at different locations. As accelerator-based oscillation experiments cannot directly measure E, the interpretation of these experiments relies heavily on phenomenological models of neutrino-nucleus interactions to infer E. Here we exploit the similarity of electron-nucleus and neutrino-nucleus interactions, and use electron scattering data with known beam energies to test energy reconstruction methods and interaction models. We find that even in simple interactions where no pions are detected, only a small fraction of events reconstruct to the correct incident energy. More importantly, widely used interaction models reproduce the reconstructed energy distribution only qualitatively and the quality of the reproduction varies strongly with beam energy. This shows both the need and the pathway to improve current models to meet the requirements of next-generation, high-precision experiments such as Hyper-Kamiokande (Japan)3 and DUNE(USA)4.

Can new energy vehicles help to achieve carbon neutrality targets?

In the reforms pertaining to the energy structure in the automotive industry, new energy vehicles (NEVs) have long been the focus of government attention, as an effective means to reduce air pollution. Therefore, this paper employs the rolling-window Granger causality test, in order to discuss the environmental benefits of new energy vehicles, so as to explore the active role of the transportation sector in reducing air pollution. By studying the interactions between NEVs and particulate matter (PM2.5) from the time period spanning from 2013:M1 to 2020:M9, we have found that the positive influences from NEVs to PM2.5 ascertain that NEVs cannot be considered as an efficient measure to mitigate air pollution. Moreover, these results are not supported by the energy and environment interaction model, which essentially indicates that replacing traditional energy with renewable energy is an effective measure for controlling environmental pollution. In fact, PM2.5 tends to have a negative impact on NEVs, which underlines that the air quality index is a leading indicator, particularly when it comes to analyzing the development of the NEVs market. This essentially highlights that in China, NEVs still do not account for a high proportion of car sales, and therefore, its environmental protection effect is not obvious. At the same time, the factor of public awareness regarding environmental protection will thus occupy a considerable proportion in the transmission of NEVs sales. These revelations will help the government to formulate environmental governance policies, and expand the new energy vehicle market to achieve carbon neutrality targets in China.

Probing interacting dark energy and scattering of baryons with dark matter in light of the EDGES 21-cm signal

The EDGES experiment has observed an excess trough ($-500^{+200}_{-500}$ mK) in the brightness temperature $T_{21}$ of the 21cm absorption line of neutral Hydrogen atom (HI) from the era of cosmic dawn ($z \simeq 17.2$). We consider possible interaction of Dark Matter and Dark Energy fluid along with the cooling off of the baryon matter by its collision with Dark Matter to explain the observed excess trough of $T_{21}$. We make use of three different Dark Matter-Dark Energy (DM-DE) interaction models to taste the viability of those models in explaining the EDGES results. The evolution of Hubble parameter is modified by DM-DE interactions and this is also addressed in this work. This in turn influences the optical depth of HI 21cm as well as the baryon temperature and thus effects the $T_{21}$ brightness temperature. In addition we also find that the DM-DE interaction enables us to explore Dark Matter with varied mass regimes and their viabilities in terms of satisfying the EDGES result.

The KASCADE Cosmic-ray Data Centre KCDC: granting open access to astroparticle physics research data

The ‘KASCADE Cosmic ray Data Centre’ is a web portal (https://kcdc.ikp.kit.edu), where the data of the astroparticle physics experiment KASCADE-Grande are made available for the interested public. The KASCADE experiment was a large-area detector for the measurement of high-energy cosmic rays via the detection of extensive air showers. The multi-detector installations KASCADE and its extension KASCADE-Grande stopped the active data acquisition in 2013 after more than 20 years of data taking. In several updates since our first release in 2013 with KCDC we provide the public measured and reconstructed parameters of more than 433 million air showers. In addition, KCDC provides meta data information and documentation to enable a user outside the community of experts to perform their own data analysis. Simulation data from three different high energy interaction models have been made available as well as a compilation of measured and published spectra from various experiments. In addition, detailed educational examples shall encourage high-school students and early stage researchers to learn about astroparticle physics, cosmic radiation as well as the handling of Big Data and about the sustainable and public provision of scientific data.

A new air-shower observable to constrain hadronic interaction models

The energy spectrum of muons at ground level in air showers is studied and a new observable is proposed to constrain hadronic interaction models used in air shower simulations. An asymmetric Gaussian function is proposed to describe the muon ground energy spectrum and its parameters are studied regarding primary particle, energy and hadronic interaction models. Based on two realistic measurements of the muon density at a given distance from the shower axis, a new observable (rμ) is defined. Considering realistic values of detector resolutions and number of measured events, it is also shown rμ can be successfully used to constrain low and high energy hadronic interaction models. The study is focused in the energy range between 1017.5 and 1018.0 eV because of the importance of this interval for particle physics and astrophysical models. The constraining power of the new observable is shown to be large within current experimental capabilities.

Does the diffusion dark matter-dark energy interaction model solve cosmological puzzles?

We study dynamics of cosmological models with diffusion effects modeling dark matter and dark energy interactions. We show the simple model with diffusion between the cosmological constant sector and dark matter, where the canonical scaling law of dark matter $({\ensuremath{\rho}}_{dm,0}{a}^{\ensuremath{-}3}(t))$ is modified by an additive $\ensuremath{\epsilon}(t)=\ensuremath{\gamma}t{a}^{\ensuremath{-}3}(t)$ to the form ${\ensuremath{\rho}}_{dm}={\ensuremath{\rho}}_{dm,0}{a}^{\ensuremath{-}3}(t)+\ensuremath{\epsilon}(t)$. We reduced this model to the autonomous dynamical system and investigate it using dynamical system methods. This system possesses a two-dimensional invariant submanifold on which the dark matter-dark energy (DM-DE) interaction can be analyzed on the phase plane. The state variables are density parameter for matter (dark and visible) and parameter $\ensuremath{\delta}$ characterizing the rate of growth of energy transfer between the dark sectors. A corresponding dynamical system belongs to a general class of jungle type of cosmologies represented by coupled cosmological models in a Lotka-Volterra framework. We demonstrate that the de Sitter solution is a global attractor for all trajectories in the phase space and there are two repellers: the Einstein-de Sitter universe and the de Sitter universe state dominating by the diffusion effects. We distinguish in the phase space trajectories, which become in good agreement with the data. They should intersect a rectangle with sides of ${\mathrm{\ensuremath{\Omega}}}_{m,0}\ensuremath{\in}[0.2724,0.3624]$, $\ensuremath{\delta}\ensuremath{\in}[0.0000,0.0364]$ at the 95% CL. Our model could solve some of the puzzles of the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model, such as the coincidence and fine-tuning problems. In the context of the coincidence problem, our model can explain the present ratio of ${\ensuremath{\rho}}_{m}$ to ${\ensuremath{\rho}}_{de}$, which is equal $0.457{6}_{\ensuremath{-}0.0831}^{+0.1109}$ at a $2\ensuremath{\sigma}$ confidence level.

Constraints on high energy interaction models from LHC and cosmic ray data

Predictions of popular cosmic ray interaction models for some basic character- istics of cosmic ray-induced extensive air showers are analyzed in view of experimental data on proton-proton collisions, obtained at the Large Hadron Collider. The differences between the results are traced down to different approaches for the treatment of hadronic interactions, implemented in those models. Potential measurements by LHC and cosmic ray experiments, which could be able to discriminate between the alternative approaches, are proposed. Modeling of high energy hadronic interactions is of considerable importance for experimental studies at the Large Hadron Collider (LHC) and, especially, in high energy cosmic ray (CR) field. In the latter case, one traditionally relies on the extensive air shower (EAS) techniques: the properties of primary CR particles are reconstructed from measured characteristics of nuclear-electro-magnetic cascades induced by CR interactions in the atmosphere. This naturally implies the importance of detailed Monte Carlo simulations of EAS development, particularly, of its backbone - the cascade of nuclear interactions of both the primary particles and of secondary hadrons produced. Thus, the success of the experimental studies depends on the validity of hadronic interaction models used in the analysis. One usually chooses between two main experimental procedures (1). In the first case, one deals with the information obtained with scintillation detectors positioned at ground. The energy of the pri- mary particle is reconstructed from the measured lateral density of charged particles (mostly electrons and positrons) while the particle type is inferred from the relative fraction of muons, compared to all charged particles at ground. Alternatively, one may study the longitudinal EAS development by mea- suring fluorescence light produced by excited air molecules at different heights in the atmosphere, for which purpose dedicated fluorescence telescopes are employed. The primary energy is then related to the total amount of fluorescence light emitted. In turn, the particle type may be determined from the measured position of the shower maximum Xmax - the depth in the atmosphere (in g/cm 2 )w here the number of ionizing particles reaches its maximal value. Not surprisingly, the observables used to determine the primary particle type - the lateral muon density ρμ and the EAS maximum position Xmax - appear to be very sensitive to details of high energy hadronic interactions. More precisely, Xmax depends strongly on the properties of the primary particle

Primary Cosmic Rays with Energies above 1015 eV – Rapporteur Review of Poster Presentations at the 23rd ECRS – Session PCR 2

Measurements of atmospheric Extensive Air Showers (EAS) are the only way of experimental studies of Primary Cosmic Rays (CR) with energies above 1015 eV. The final targets of these studies are search for astrophysical origin of these particles and properties of particle production in high energy particle interaction. Works presented at the PCR 2 session in the form of posters reflected the current progress in this area. In this review presented posters were grouped according to CR energy range, astrophysical significance, relation to high energy physics interaction properties and interaction models, and future experiments. 42 posters were submitted for this session. Some of the presented material in posters overlapped in parts with oral presentations.

Study of atmospheric muons using a cosmic ray telescope

The charge ratio of cosmic muons holds important information for both the atmospheric neutrino anomaly and hadronic interaction models. In this paper we measured the muon charge ratio () in the cosmic ray flux in the momenta range 0.76–1.60 GeV/c by using a cosmic ray telescope. The delayed coincidence method is used based on the reduced mean lifetime of negative muons due to nuclear capture in matter. The systematic time-dependent effects of the muon charge ratio are considered by grouping the decay data into different time intervals. We compared the experimental data with the predictions of CORSIKA simulations using a high energy interaction model (QGSJET-II) and two low energy interaction models (UrQMD and GHEISHA) in the energy range 1011–1016 eV for primary particles. In addition, by considering the muon flux in different zenithal and azimuthal angles, the muon angular distribution is obtained as I(θ) = I(0)cos nθ with average n = 1.91 ± 0.07. Dependence of the muon flux on the azimuth angle (the East–West effect) is also observed, due to the influence of the geomagnetic field in particular on low energy muons.

Influence of low energy hadronic interactions on air-shower simulations

Experiments measuring cosmic rays above an energy of 10^14 eV deduce the energy and mass of the primary cosmic ray particles from air-shower simulations. We investigate the importance of hadronic interactions at low and high energies on the distributions of muons and electrons in showers on ground. In air shower simulation programs, hadronic interactions below an energy threshold in the range from 80 GeV to 500 GeV are simulated by low energy interaction models, like Fluka or Gheisha, and above that energy by high energy interaction models, e.g. Sibyll or QGJSJet. We find that the impact on shower development obtained by switching the transition energy from 80 GeV to 500 GeV is comparable to the difference obtained by switching between Fluka and Gheisha.

Study of low energy hadronic interaction models based on BESS observed cosmic ray proton and antiproton spectra at medium high altitude

We study low energy hadronic interaction models based on BESS observed cosmic ray proton and antiproton spectra at medium high altitude. Among the three popular low energy interaction models, we find that FLUKA reproduces the results of BESS observations on the secondary proton spectrum reasonably well over the whole observed energy range, the model UrQMD works well at relatively higher energies, whereas the spectrum obtained with GHEISHA differs significantly from the measured spectrum. The simulated antiproton spectrum with FLUKA, however, exhibits significant deviation from the BESS observation whereas UrQMD and GHEISHA reproduce the BESS observations within experimental error.

Energy spectra of elemental groups of cosmic rays: Update on the KASCADE unfolding analysis

The KASCADE experiment measures extensive air showers induced by cosmic rays in the energy range around the so-called knee. The data of KASCADE have been used in a composition analysis showing the knee at 3–5 PeV to be caused by a steepening in the light-element spectra [T. Antoni et al., (KASCADE Coll.), Astropart. Phys. 24 (2005) 1–25]. Since the applied unfolding analysis depends crucially on simulations of air showers, different high-energy hadronic interaction models (QGSJet and SIBYLL) were used. The results have shown a strong dependence of the relative abundance of the individual mass groups on the underlying model. In this update of the analysis we apply the unfolding method with a different low energy interaction model (FLUKA instead of GHEISHA) in the simulations. While the resulting individual mass group spectra do not change significantly, the overall description of the measured data improves by using the FLUKA model. In addition data in a larger range of zenith angle are analysed. The new results are completely consistent, i.e. there is no hint to any severe problem in applying the unfolding analysis method to KASCADE data.

Comparison of high energy interaction models used for atmospheric shower simulations above 1 TeV

We present here a comparison of interaction models commonly used for simulating cosmic ray shower development in the atmosphere at energies greater than 1 TeV. The implementations of these models in CORSIKA and the FLUKA transport and interaction code are relevant for extensive air shower experiments, neutrino telescopes, and gamma-ray surfacebased detectors. We compare the pion, kaon, charmed meson and baryon energy fractions and the multiplicities at the first interaction stage of monoenergetic protons on nitrogen nuclei in the range 1 TeV-100 PeV. We also show comparisons in terms of Z-moments, a spectrumweighted multiplicity often used in the cosmic ray community. The transverse and longitudinal momentum distributions of the secondary muons produced in proton-nitrogen collisions are also shown.

Validation of the FLUKA Monte Carlo code for predicting induced radioactivity at high-energy accelerators

Samples of different materials, consisting of major elements with masses up to the one of copper, were exposed to the stray radiation field created by a 120 GeV hadron beam in a copper target. The induced specific activities of radionuclides, as measured with gamma spectrometry, then served as benchmark of the FLUKA Monte Carlo code. A careful analysis of the experimental data as well as of the reactions leading to the various isotopes in the simulation demonstrated that FLUKA is capable of predicting individual isotopes with an uncertainty of less than 20–30% in most cases. Due to the universal nature of the high energy interaction models the results also serve as indirect validation of FLUKA predictions for target materials, reactions and isotopes not covered by this study.

Ultra high energy interaction models for Monte Carlo calculations: what model is the best fit

We briefly outline two methods for extension of hadronic interaction models to extremely high energy. Then we compare the main characteristics of representative computer codes that implement the different models and give examples of air shower parameters predicted by those codes.

How should we modify the high energy interaction models?

An analysis has been made of the present situation with respect to the high energy hadron-nucleus and nucleusnucleus interaction models as applied to cosmic rays. As is already known, there are inconsistencies in the interpretation of experimental data on the primary mass composition, which appear when different EAS components are used for the analyses, even for the same experiment. In the absence of obvious experimental defects, there is a clear need for an improvement to the existing models; we argue that the most promising way is to enlist two effects which should be present in nucleus-nucleus collisions but have not been allowed for before. These are: a few percent energy transfer into the EAS electromagnetic component due to electron-positron pair production or electromagnetic radiation of the quark-gluon plasma and a small slow-down of the cascading process in its initial stages associated with the extended lifetime of excited nuclear fragments. The latter process displaces the shower maximum deeper into the atmosphere.

A study on the utilization of tritide titanium targets for monoenergetic neutron production

Proton beam interaction with a tritide titanium target in an electrostatic accelerator was studied by measuring the produced neutron rate as a function of bombarding time. The results are analyzed in the frame of target temperature increase, extension of existing low energy interaction model and SRIM simulation. Special emphasis is put on the evaluation of the release of radiotoxic tritium from the solid target.

Study of the cosmic ray primary spectrum at 10 15 < E0 < 10 16 eV with the EAS-TOP array

The break observed in the electron shower size power law spectrum of Extensive Air Showers (EAS) at corresponding primary energy E 0 ∼ (3–5)10 15 eV (“knee”) is studied different EAS components (electromagnetic and muonic) and at different atmospheric depths. A consistent description is obtained. The interpretation of data in terms of primary composition, and following the most accepted high energy interaction models, leads to an increasing average primary mass in this energy range. The study of such behaviour is expected to provide a crucial information for the understanding of the physical parameters that characterize the break for the different primaries.