The $Lambda$CDM model successfully explains the majority of cosmological observations. However, the $ Lambda$CDM model is challenged by Hubble tension, a remarkable difference of Hubble constant $H_0$ between measurements from local probe and the pre
diction from Planck cosmic microwave background observations under $ Lambda$CDM model. So one urgently needs new distance indicators to test the Hubble tension. Fast radio bursts (FRBs) are millisecond-duration pulses occurring at cosmological distances, which are attractive cosmological probes. However, there is a thorny problem that the dispersion measures (DMs) contributed by host galaxy and the inhomogeneities of intergalactic medium cannot be exactly determined from observations. Previous works assuming fixed values for them bring uncontrolled systematic error in analysis. A reasonable approach is to handle them as probability distributions extracted from cosmological simulations. Here we report a measurement of ${H_0} = 64.67^{+5.62}_{-4.66} {rm km s^{-1} Mpc^{-1}}$ using fourteen localized FRBs, with an uncertainty of 8.7% at 68.3 per cent confidence. Thanks to the high event rate of FRBs and localization capability of radio telescopes (i.e., Australian Square Kilometre Array Pathfinder and Very Large Array), future observations of a reasonably sized sample ($sim$100 localized FRBs) will provide a new way of measuring $ H_0$ with a high precision ($sim$2.6%) to test the Hubble tension.
The energy and waiting time distributions are important properties to understand the physical mechanism of repeating fast radio bursts (FRBs). Recently, Five-hundred-meter Aperture Spherical radio Telescope (FAST) detected the largest sample of FRB 1
21102, containing 1652 bursts. The energy distribution at high-energy range ($>10^{38}$ erg) can be fitted with a single power-law function with an index of $-1.86$. However, the distribution at low-energy range deviates from the power-law function. The energy distributions of high-energy bursts at different epochs are inconsistent. We find the power-law index of $-1.70$ for early bursts and $-2.60$ for later bursts. For bursts observed in a single day, a linear repetition pattern is found. We use the Weibull function to fit the waiting time distribution. The shape parameter $k = 0.72^{+0.01}_{-0.02}$ and the event rate $r = 734.47^{+29.04}_{-27.58}$ day$ ^{-1} $ are derived. If the waiting times with $delta_t < 28$ s are excluded, the burst behavior can be described by a Poisson process. The best-fitting values of $k$ are slightly different for low-energy and high-energy bursts. The event rates change significantly across the observing time, while the shape parameters $k$ vary slightly in different days.
Recently, kagome lattice metal AV$_3$Sb$_5$ (A = K, Rb, Cs) family has received wide attention due to its presence of superconductivity, charge density wave (CDW) and peculiar properties from topological nontrivial electronic structure. With time-res
olved pump-probe spectroscopy, we show that the excited quasiparticle relaxation dynamics can be explained by formation of energy gap below the phase transition being similar to a usual second-order CDW condensate, by contrast, the structure change is predominantly first order phase transition. Furthermore, no CDW amplitude mode is identified in the ordered phase. The results suggest that the CDW order is very different from the traditional CDW condensate. We also find that weak pump pulse can non-thermally melt the CDW order and drive the sample into its high temperature phase, revealing the fact that the difference in lattice potential between those phases is small.
Electrides are an emerging class of materials with highly-localized electrons in the interstices of a crystal that behave as anions. The presence of these unusual interstitial quasi-atom (ISQ) electrons leads to interesting physical and chemical prop
erties, and wide potential applications for this new class of materials. Crystal defects often have a crucial influence on the properties of materials. Introducing impurities has been proved to be an effective approach to improve the properties of a material and to expand its applications. However, the interactions between the anionic ISQs and the crystal defects in electrides are as yet unknown. Here, dense FCC-Li was employed as an archetype to explore the interplay between anionic ISQs and interstitial impurity atoms in this electride. This work reveals a strong coupling among the interstitial impurity atoms, the ISQs, and the matrix Li atoms near to the defects. This complex interplay and interaction mainly manifest as the unexpected tetrahedral interstitial occupation of impurity atoms and the enhancement of electron localization in the interstices. Moreover, the Be impurity occupying the octahedral interstice shows the highest negative charge state (Be8-) discovered thus far. These results demonstrate the rich chemistry and physics of this emerging material, and provide a new basis for enriching their variants for a wide range of applications.
In this letter, we study the resource allocation for a multiuser intelligent reflecting surface (IRS)-aided simultaneous wireless information and power transfer (SWIPT) system. Specifically, a multi-antenna base station (BS) transmits energy and info
rmation signals simultaneously to multiple energy harvesting receivers (EHRs) and information decoding receivers (IDRs) assisted by an IRS. Under this setup, we introduce a multi-objective optimization (MOOP) framework to investigate the fundamental trade-off between the data sum-rate maximization and the total harvested energy maximization, by jointly optimizing the energy/information beamforming vectors at the BS and the phase shifts at the IRS. This MOOP problem is first converted to a single-objective optimization problem (SOOP) via the $epsilon$-constraint method and then solved by majorization minimization (MM) and inner approximation (IA) techniques. Simulation results unveil a non-trivial trade-off between the considered competing objectives, as well as the superior performance of the proposed scheme as compared to various baseline schemes.
Anticipated breakthroughs in solid-state quantum computing will rely on achieving unprecedented control over the wave-like states of electrons in crystalline materials. For example, an international effort to build a quantum computer that is topologi
cally protected from decoherence is focusing on carefully engineering the wave-like states of electrons in hybrid devices that proximatize an elemental superconductor and a semiconductor nanostructure[1-6]. However, more than 90 years after Bloch derived the functional forms of electronic waves in crystals[7](now known as Bloch wavefunction) rapid scattering processes have so far prevented their direct experimental reconstruction, even in bulk materials. In high-order sideband generation (HSG)[8-15], electrons and holes generated in semiconductors by a near-infrared (NIR) laser are accelerated to high kinetic energy by a strong terahertz field, and recollide to emit NIR sidebands before they are scattered. Here we reconstruct the Bloch wavefunctions of two types of holes in gallium arsenide by experimentally measuring sideband polarizations and introducing an elegant theory that ties those polarizations to quantum interference between different recollision pathways. Because HSG can, in principle, be observed from any direct-gap semiconductor or insulator, we expect the method introduced in this Article can be used to reconstruct Bloch wavefunctions in a large class of bulk and nanostructured materials, accelerating the development of topologically-protected quantum computers as well as other important electronic and optical technologies.
Employing the the stellar evolution code (Modules for Experiments in Stellar Astrophysics), we calculate yields of heavy elements from massive stars via stellar wind and core-collapse supernovae (CCSN) ejecta to interstellar medium (ISM). In our mode
ls, the initial masses ($M_{rm ini}$) of massive stars are taken from 13 to 80 $M_odot$, their initial rotational velocities (V) are 0, 300 and 500 km s$^{-1}$, and their metallicities are [Fe/H] = -3, -2, -1, and 0. The yields of heavy elements coming from stellar winds are mainly affected by the stellar rotation which changes the chemical abundances of stellar surfaces via chemically homogeneous evolution, and enhances mass-loss rate. We estimate that the stellar wind can produce heavy element yields of about $10^{-2}$ (for low metallicity models) to several $M_odot$ (for low metallicity and rapid rotation models) mass. The yields of heavy element produced by CCSN ejecta also depend on the remnant mass of massive mass which is mainly determined by the mass of CO-core. Our models calculate that the yields of heavy elements produced by CCSN ejecta can get up to several $M_odot$. Compared with stellar wind, CCSN ejecta has a greater contribution to the heavy elements in ISM. We also compare the $^{56}$Ni yields by calculated in this work with observational estimate. Our models only explain the $^{56}$Ni masses produced by faint SNe or normal SNe with progenitor mass lower than about 25 $M_odot$, and greatly underestimate the $^{56}$Ni masses produced by stars with masses higher than about 30 $M_odot$.
Based on the realistic nuclear force of the high-precision CD-Bonn potential, we have performed comprehensive calculations for neutron-rich calcium isotopes using the Gamow shell model (GSM) which includes resonance and continuum. The realistic GSM c
alculations produce well binding energies, one- and two-neutron separation energies, predicting that $^{57}$Ca is the heaviest bound odd isotope and $^{70}$Ca is the dripline nucleus. Resonant states are predicted, which provides useful information for future experiments on particle emissions in neutron-rich calcium isotopes. Shell evolutions in the calcium chain around neutron numbers textit{N} = 32, 34 and 40 are understood by calculating effective single-particle energies, the excitation energies of the first $2^+$ states and two-neutron separation energies. The calculations support shell closures at $^{52}$Ca (textit{N} = 32) and $^{54}$Ca (textit{N} = 34) but show a weakening of shell closure at $^{60}$Ca (textit{N} = 40). The possible shell closure at $^{70}$Ca (textit{N} = 50) is predicted.
Recently, the discovery of Galactic FRB 200428 associated with a X-ray burst (XRB) of SGR 1935+2154 has built a bridge between FRBs and magnetar activities. In this paper, we assume that the XRB occurs in the magnetar magnetosphere. We show that the
observational properties of FRB 200428 and the associated XRB are consistent with the predictions of synchrotron maser emission at ultrarelativistic magnetized shocks, including radiation efficiency, similar energy occurrence frequency distributions, and simultaneous arrive times. It requires that the upstream medium is a mildly relativistic baryonic shell ejected by a previous flare. The energy injection by flares responsible for the radio bursts will produce a magnetar wind nebula, which has been used to explain the persistent radio source associated FRB 121102. We find that the radio continuum around SGR 1935+2154 can be well understood in the magnetar wind nebula model, by assuming the same energy injection rate $dot{E} propto t^{-1.37}$ as FRB 121102. The required baryonic mass is also estimated form the observations of FRB 121102 by GBT and FAST. By assuming the same radiation efficiency $eta sim 10^{-5}$, the total baryonic mass ejected from the central magnetar is about 0.005 solar mass. This value is much larger than the typical mass of a magnetar outer crust, but is comparable to the total mass of a magnetar crust.
The intrinsic antiferromagnetic (AFM) interlayer coupling in two-dimensional magnetic topological insulator MnBi$_2$Te$_4$ places a restriction on realizing stable quantum anomalous Hall effect (QAHE) [Y. Deng et al., Science 367, 895 (2020)]. Throug
h density functional theory calculations, we demonstrate the possibility of tuning the AFM coupling to the ferromagnetic coupling in MnBi$_2$Te$_4$ films by alloying about 50% V with Mn. As a result, QAHE can be achieved without alternation with the even or odd septuple layers. This provides a practical strategy to get robust QAHE in ultrathin MnBi$_2$Te$_4$ films, rendering them attractive for technological innovations.
