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The AMS02 experiment has published the periodic spectra of proton, helium and helium isotopes across the majority of the 24 solar cycle. These precise data exhibit temporal structures that correlate with solar modulation. In this study, we utilize these data to probe three analytic solar modulation models, including the force-field approximation, the convection-diffusion model and the extended force-field approximation with a drift effect. We adopt a method that eliminates the influence of interstellar cosmic ray spectra, and use the Earth-observed spectra at time $t_1$ to predict those at time $t_2$. In order to explore the rigidity-dependence of solar modulation models, we substitute the conventional potential parameter $\phi$ with a modified parameter $\phi'=\frac{R}{ k_2(R)}\phi$ for our analysis. Combining with the $\chi^2$ minimization method, the best-fit modulation parameter $\phi'$ can be evaluated. First, we test the validity of a rigidity-independent $\phi'$ and find that both the force-field approximation (FFA) and the extended force-field approximation (EFFA) agree well with data near the solar minimum period. However, all models significantly deviate from the data during the solar maximum. Consequently, we assume a constant $\phi'(t_1)$ at solar minimum and calculate $\Delta\phi'=\phi'(t_2)-\phi'(t_1)$ for each rigidity bin at time $t_2$. It is found that $\Delta\phi'$ generally adheres to a linear-logarithm relationship with rigidity at any given time. By adopting a linear-logarithm formula of $\Delta\phi'$, we further discover that both the modified FFA and EFFA can reconcile the observations during solar maxima. This suggests that at solar maximum, the parameter $\phi'$, which correlates with the diffusion pattern in the heliospheric magnetic fields, exhibits a rigidity dependence., Comment: Accepted to be published in PRD

Encoding is the carrier of information. AI models possess basic capabilities in syntax, semantics, and reasoning, but these capabilities are sensitive to specific inputs. In this study, we introduce an encoding algorithm, TSIS (Simplified TSID), to the t-SMILES family as a fragment-based linear molecular representation. TSID has been demonstrated to significantly outperform classical SMILES, DeepSMILES, and SELFIES in previous work. A further comparative analysis in this study reveals that the tree structure used by TSID is more easily learned than anticipated, regardless of whether Transformer or LSTM models are used. Furthermore, TSIS demonstrates comparable performance to TSID and significantly outperforms SMILES, SELFIES, and SAFE. While SEFLIES and SAFE present significant challenges in semantic and syntactic analysis, respectively, due to their inherent complexity.

Effective representation of molecules is a crucial factor affecting the performance of artificial intelligence models. This study introduces a flexible, fragment-based, multiscale molecular representation framework called t-SMILES (tree-based SMILES) with three code algorithms: TSSA, TSDY and TSID. It describes molecules using SMILES-type strings obtained by performing a breadth-first search on a full binary tree formed from a fragmented molecular graph. Systematic evaluations using JTVAE, BRICS, MMPA, and Scaffold show the feasibility of constructing a multi-code molecular description system, where various descriptions complement each other, enhancing the overall performance. In addition, it can avoid overfitting and achieve higher novelty scores while maintaining reasonable similarity on labeled low-resource datasets, regardless of whether the model is original, data-augmented, or pre-trained then fine-tuned. Furthermore, it significantly outperforms classical SMILES, DeepSMILES, SELFIES and baseline models in goal-directed tasks. And it surpasses state-of-the-art fragment, graph and SMILES based approaches on ChEMBL, Zinc, and QM9.

One of the fundamental issues in cosmic ray physics is to explain the nature of cosmic ray acceleration and propagation mechanisms. Thanks to the precise cosmic ray data measured by recent space experiments, we are able to investigate the cosmic ray acceleration and propagation models more comprehensively and reliably. In this paper, we combine the secondary-to-primary ratios and the primary spectra measured by PAMELA, AMS02, ACE-CRIS and Voyager-1 to constrain the cosmic ray source and transport parameters. The study shows that the $Z>2$ data yield a medium-energy diffusion slope $\delta_{2}\sim\left(0.42, 0.48\right)$ and a high-energy slope $\delta_{3}\sim\left(0.22, 0.34\right)$. The $Z\leq2$ species obtain a looser constraint on $\delta_{2}\sim\left(0.38, 0.47\right)$, but a tighter constraint on $\delta_{3}\sim\left(0.21, 0.30\right)$. The overlaps infer that the heavy and light particles can give compatible results at medium to high energies. Besides, both the light and heavy nuclei indicate a consistent diffusion slope variation $\Delta\delta_{H}$ around $200\sim300$~GV. At low energies, significant disagreements exist between the heavy and light elements. The B/C ratio requires a much larger diffusion slope shift $\Delta\delta_{L}$ around 4 GV or a stronger \textit{Alfv$\acute{e}$n velocity} $v_{A}$ than the low-mass data. This indicates that the heavy and light particles may suffer different low-energy transport behaviors in Galaxy. However, better understanding on the consistency/inconsistency between the heavy and light cosmic rays relies on more precise cross-sections, better constraints on correlations in systematic errors of data, more accurate estimation on Galaxy halo size and more robust description for Solar modulation during the reversal period of HMF.

Quantum key distribution (QKD) can generate secure key bits between remote users with quantum mechanics. However, the gap between the theoretical model and practical realizations gives eavesdroppers opportunities to intercept secret key. The most insidious attacks, known as quantum hacking, are the ones with no significant discrepancy of the measurement results using side-channel loopholes of QKD systems. Depicting full-time-scale characteristics of the quantum signals, the quantum channel, and the QKD system can provide legitimate users extra capabilities to defeat malicious attacks. For the first time, we propose the method exploring temporal ghost imaging (TGI) scheme to perceive quantum hacking with temporal fingerprints and experimentally verify its validity. The scheme presents a common approach to promote QKD's practical security from a new perspective of signals and systems., Comment: 11 pages, 6 figures

Because of the limitations of the infrared imaging principle and the properties of infrared imaging systems, infrared images have some drawbacks, including a lack of details, indistinct edges, and a large amount of salt-andpepper noise. To improve the sparse characteristics of the image while maintaining the image edges and weakening staircase artifacts, this paper proposes a method that uses the Lp quasinorm instead of the L1 norm and for infrared image deblurring with an overlapping group sparse total variation method. The Lp quasinorm introduces another degree of freedom, better describes image sparsity characteristics, and improves image restoration. Furthermore, we adopt the accelerated alternating direction method of multipliers and fast Fourier transform theory in the proposed method to improve the efficiency and robustness of our algorithm. Experiments show that under different conditions for blur and salt-and-pepper noise, the proposed method leads to excellent performance in terms of objective evaluation and subjective visual results.

The secondary-to-primary ratios are unique tools to investigate cosmic ray propagation mechanisms. In this work, we use the latest data of deuteron-to-helium~4 ratio and helium~3-to-helium~4 ratio measured by PAMELA combined with other Z$\leq$2 primary fluxes measured by PAMELA and Voyager-1, to constrain the cosmic ray acceleration and propagation models. The analysis is performed by interfacing statistical tools with the GALPROP propagation package. To better fit both the modulated and unmodulated low energy cosmic ray data, we find that a time-, charge- and rigidity-dependent solar modulation model is better than the force-field approximation. Among all the studied cosmic ray propagation models, the diffusion-reacceleration-convection model is strongly supported by the derived Bayesian evidence. The robustness of the estimated diffusion slope $\delta$ is cross-checked by another low-mass secondary-to-primary ratio, i.e. the antiproton-to-proton ratio. It is shown that the diffusion-reacceleration-convection model can reconcile well with the high energy antiproton-to-proton ratio. This indicates that the estimated value of $\delta$ is reliable. The well constraint $\delta$ from the `best' model is found to be close to 1/3, inferring a Kolmogorov-type interstellar magnetic turbulence., Comment: Accepted by Physics Letters B

A cryo scanning transmission X-ray microscope, the cryo-STXM, has been designed and commissioned at the Canadian Light Source synchrotron. The instrument is designed to operate from 100 - 4000 eV (lambda = 12.4 - 0.31 nm). Users can insert a previously frozen sample, through a load lock, and rotate it plus minus 70 degrees in the beam to collect tomographic data sets. The sample can be maintained for extended periods at 92 K primarily to suppress radiation damage, and a pressure on the order of 10-9 Torr to suppress sample contamination. The achieved spatial resolution (30 nm) and spectral resolution (0.1 eV) are similar to other current soft X-ray STXMs, as demonstrated by measurements on known samples and test patterns. The data acquisition efficiency is significantly more favorable for both imaging and tomography. 2D images, 3D tomograms and 4D chemical maps of automotive hydrogen fuel cell thin sections are presented to demonstrate current performance and new capabilities, namely cryo-spectrotomography in the soft X-ray region., Comment: 56 pages

Phase manipulation is essential to quantum information processing, for which the orbital angular momentum (OAM) of photon is a promising high-dimensional resource. Dove prism (DP) is one of the most important element to realize the nondestructive phase manipulation of OAM photons. DP usually changes the polarization of light and thus increases the manipulation error for a spin-OAM hybrid state. DP in a Sagnac interferometer also introduces a mode-dependent global phase to the OAM mode. In this work, we implemented a high-dimensional controlled-phase manipulation module (PMM), which can compensate the mode-dependent global phase and thus preserve the phase in the spin-OAM hybrid superposition state. The PMM is stable for free running and is suitable to realize the high-dimensional controlled-phase gate for spin-OAM hybrid states. Considering the Sagnac-based structure, the PMM is also suitable for classical communication with spin-OAM hybrid light field., Comment: 5 pages, 6 figures

Molybdenum and nitrogen co-doped $TiO_2$ nanotube arrays (TNAs) were prepared by anodizing in association with hydrothermal treatment. As-prepared Mo and N co-doped TNAs were characterized by field emission scanning electron microscopy, X-ray diffraction, X-ray photoelectron spectroscopy and ultraviolet-visible light diffuse reflection spectroscopy. Besides, the photocatalytic activity of Mo and N co-doped TNAs for the degradation of methylene blue (denoted as MB) under visible light irradiation was evaluated. It was found that N in co-doped TNAs coexists in the forms of N-Ti-O and N-O-Ti, while Mo exists as $Mo^{6+}$ by substituting Ti in the lattice of $TiO_2$. In the meantime, Mo and N co-doping extends the absorption of TNAs into the whole visible light region and results in remarkably enhanced photocatalytic activity for the degradation of MB under visible light irradiation. This could be attributed to the synergetic effect between Mo-doping and N-doping. Namely, Mo and N passivated co-doping produces new states in TNAs, thereby narrowing the bandgap and decreasing the recombination rate of electrons and holes. As a result, the visible light absorption and photocatalytic activity of TNAs is greatly increased. Furthermore, Mo ions with multiple valences in all co-doped samples could act as trapping sites to effectively decrease the recombination rate of electrons and holes, which also contribute to improved photocatalytic activity of Mo and N co-doped TNAs. Keywords: TiO2 Nanotube Arrays, Mo, N, Co-Doping, Photocatalytic Activity., Comment: 7 pages, 6 figures. arXiv admin note: text overlap with arXiv:1312.1484

A series of W, N codoped TiO2 nanotube arrays with different dopant contents were fabricated by anodizing in association with hydrothermal treatment. The samples were characterized by scanning electron microscopy, X-ray diffraction, X-ray photoelectron spectroscopy, and ultraviolet-visible light diffuse reflection spectroscopy. Moreover, the photocatalytic activity of W and N codoped TiO2 nanotube arrays was evaluated by degradation of methylene blue under visible light irradiation., Comment: 8 pages, 5 figures

We have used the dynamically constrained phase space coalescence model to investigate the centrality dependence of light (anti)nuclei and (anti)hypertriton production based on the $6.2\times 10^7$ hadronic final states generated by the PACIAE model in Au+Au collisions at $\sqrt{s_{\rm{NN}}}=200$ GeV in $|y| <1$ and $p_T<5$ acceptances. It turned out that the yields of light (anti)nuclei and (anti)hypertriton strongly depend on the centrality, i.e. their yields decrease rapidly with the increase of centrality bins; but their yield ratios are independent on centrality. These theoretical results are consistent with the STAR and PHENIX data. Furthermore, centrality distribution of $d$ ($\bar d$), $^3{He}$ ($^3{\bar{He}}$) and $_{\bar\Lambda}^3H$ ($\bar{_{\bar\Lambda}^3H}$) follows Gaussian distributions. This means that light (anti)nuclei and (anti)hypertriton are primarily produced in the central collisions., Comment: 6 pages, 4 figures. arXiv admin note: text overlap with arXiv:1209.4182

Studying the acceleration and propagation mechanisms of Galactic cosmic rays can provide information regarding astrophysical sources, the properties of our Galaxy, and possible exotic sources such as dark matter. To understand cosmic ray acceleration and propagation mechanisms, accurate measurements of different cosmic ray elements over a wide energy range are needed. The PAMELA experiment is a satellite-borne apparatus which allows different cosmic ray species to be identified over background. Measurements of the cosmic ray antiproton flux and the antiproton-to-proton flux ratio from 1.5 GeV to 180 GeV are presented in this thesis. Compared to previous experiments, PAMELA extends the energy range of antiproton measurements and provides significantly higher statistics. The derived antiproton flux and antiproton-to-proton flux ratio are consistent with previous measurements and generally considered to be produced as secondary products when cosmic ray protons and helium nuclei interact with the interstellar medium. To constrain cosmic ray acceleration and propagation models, the antiproton data measured by PAMELA were further used together with the proton spectrum reported by PAMELA, as well as the B/C data provided by other experiments. Statistical tools were interfaced with the cosmic ray propagation package GALPROP to perform the constraining analyses. Diffusion models with a linear diffusion coefficient and modified diffusion models with a low energy dependence of the diffusion coefficient were studied in the $\chi^{2}$ study. Uncertainties on the parameters and the goodness of fit of each model were given. Some models are further studied using the Bayesian inference. Posterior means and errors of the parameters base on our prior knowledge on them were obtained in the Bayesian framework. This method also allowed us to understand the correlation between parameters and compare models., Comment: Doctoral Thesis in Physics, Royal Institute of Technology (KTH), defense on 1st June 2012

Electronic devices that exploit electrical switching of physical properties of thin films of perovskite materials (especially colossal magnetoresistive materials) have been invented. Unlike some related prior devices, these devices function at room temperature and do not depend on externally applied magnetic fields. Devices of this type can be designed to function as sensors (exhibiting varying electrical resistance in response to varying temperature, magnetic field, electric field, and/or mechanical pressure) and as elements of electronic memories. The underlying principle is that the application of one or more short electrical pulse(s) can induce a reversible, irreversible, or partly reversible change in the electrical, thermal, mechanical, and magnetic properties of a thin perovskite film. The energy in the pulse must be large enough to induce the desired change but not so large as to destroy the film. Depending on the requirements of a specific application, the pulse(s) can have any of a large variety of waveforms (e.g., square, triangular, or sine) and be of positive, negative, or alternating polarity. In some applications, it could be necessary to use multiple pulses to induce successive incremental physical changes. In one class of applications, electrical pulses of suitable shapes, sizes, and polarities are applied to vary the detection sensitivities of sensors. Another class of applications arises in electronic circuits in which certain resistance values are required to be variable: Incorporating the affected resistors into devices of the present type makes it possible to control their resistances electrically over wide ranges, and the lifetimes of electrically variable resistors exceed those of conventional mechanically variable resistors. Another and potentially the most important class of applications is that of resistance-based nonvolatile-memory devices, such as a resistance random access memory (RRAM) described in the immediately following article, Electrically Variable Resistive Memory Devices (MFS-32511-1).