Miracle-dz/UniFAR-FTUs huggingface dataset:
Self-assembling hybrid diamond–biological quantum devices

The realization of scalable arrangements of nitrogen vacancy (NV) centers in diamond remains a key challenge on the way towards efficient quantum information processing, quantum simulation and quantum sensing applications. Although technologies based on implanting NV-centers in bulk diamond crystals or hybrid device approaches have been developed, they are limited by the achievable spatial resolution and by the intricate technological complexities involved in achieving scalability. We propose and demonstrate a novel approach for creating an arrangement of NV-centers, based on the self-assembling capabilities of biological systems and their beneficial nanometer spatial resolution. Here, a self-assembled protein structure serves as a structural scaffold for surface functionalized nanodiamonds, in this way allowing for the controlled creation of NV-structures on the nanoscale and providing a new avenue towards bridging the bio–nano interface. One-, two- as well as three-dimensional structures are within the scope of biological structural assembling techniques. We realized experimentally the formation of regular structures by interconnecting nanodiamonds using biological protein scaffolds. Based on the achievable NV-center distances of 11 nm, we evaluate the expected dipolar coupling interaction with neighboring NV-centers as well as the expected decoherence time. Moreover, by exploiting these couplings, we provide a detailed theoretical analysis on the viability of multiqubit quantum operations, suggest the possibility of individual addressing based on the random distribution of the NV intrinsic symmetry axes and address the challenges posed by decoherence and imperfect couplings. We then demonstrate in the last part that our scheme allows for the high-fidelity creation of entanglement, cluster states and quantum simulation applications.
K-BAND SPECTROSCOPY OF (PRE-)CATACLYSMIC VARIABLES: ARE SOME DONOR STARS REALLY CARBON POOR?

We present a new sample of K-band spectral observations for cataclysmic variables (CVs): non-magnetic and magnetic as well as present-day and pre-CVs. The purpose of this diverse sample is to address the recent claim that the secondary stars in dwarf novae are carbon deficient, having become so through a far more evolved evolution than the current paradigm predicts. Our new observations, along with previous literature results, span a wide range of orbital period and CV type. In general, dwarf novae in which the secondary star is seen show weak to no CO absorption while polar and pre-CV donor stars appear to have normal CO absorption for their spectral type. However, this is not universal. The presence of normal looking CO absorption in the dwarf nova SS Aur and the hibernating CV QS Vir and a complete lack of CO absorption in the long-period polar V1309 Ori cloud the issue. A summary of the literature pointing to non-solar abundances including enhanced N v/C iv ratios is presented. It appears that some CVs have non-solar abundance material accreting onto the white dwarf suggesting an evolved secondary star while for others CO emission in the accretion disk may play a role. However, the exact mechanism or combination of factors causing the CO absorption anomaly in CVs is not yet clear.
Temperature dependence of the magnetic Casimir-Polder interaction

We analyze the magnetic dipole contribution to atom-surface dispersion forces. Unlike its electrical counterpart, it involves small transition frequencies that are comparable to thermal energy scales. A significant temperature dependence is found near surfaces with a nonzero dc conductivity, leading to a strong suppression of the dispersion force at $Tg0$. We use thermal response theory for the surface material and discuss both normal metals and superconductors. The asymptotes of the free energy of interaction and of the entropy are calculated analytically over a large range of distances. Near a superconductor, the onset of dissipation at the phase transition strongly changes the interaction, including a discontinuous entropy. We discuss the similarities with the Casimir interaction between two surfaces and suggest that precision measurements of the atom-surface interaction may shed light upon open questions around the temperature dependence of dispersion forces between lossy media.
THE DECREASE OF SPECIFIC ANGULAR MOMENTUM AND THE HOT TOROID FORMATION: THE MASSIVE CLUMP G10.6−0.4

This is the first paper of our series of high-resolution (1″) studies of the massive star-forming region G10.6−0.4. We present the emission line observations of the hot core type tracers (O13CS, OCS, SO2) with ∼0. ″5 resolution. By comparing the results to the high-resolution NH3 absorption line observation, we confirm for the first time the rotationally flattened hot toroid in the central <0.1 pc region, which has a rotational axis perpendicular to its geometrical major axis. In addition, we present the observations of NH3, 13CS, and CH3CN with ∼1″ resolution, and follow the dynamics of the molecular accretion flow from the 0.3 pc radius to the inner 0.03 pc radius. With reference to the rotational axis of the hot toroid, we measure the rotational velocity from the molecular emission in the region. The results are consistent with an envelope with a rapid decrease of the specific angular momentum from the outer to the inner region. These new results improve the current understanding of the molecular accretion flow in an ultracompact H ii region created by the embedded O-type cluster.
Dirac nodal lines and induced spin Hall effect in metallic rutile oxides

We have found Dirac nodal lines (DNLs) in the band structures of metallic rutile oxides ${\mathrm{IrO}}_{2}, {\mathrm{OsO}}_{2}$, and ${\mathrm{RuO}}_{2}$ and have revealed a large spin Hall conductivity contributed by these nodal lines, which explains a strong spin Hall effect (SHE) of ${\mathrm{IrO}}_{2}$ discovered recently. Two types of DNLs exist. The first type forms DNL networks that extend in the whole Brillouin zone and appears only in the absence of spin-orbit coupling (SOC), which induces surface states on the boundary. Because of SOC-induced band anticrossing, a large intrinsic SHE can be realized in these compounds. The second type appears at the Brillouin zone edges and is stable against SOC because of the protection of nonsymmorphic symmetry. Besides reporting these DNL materials, our work reveals the general relationship between DNLs and the SHE, indicating a way to apply Dirac nodal materials for spintronics.
Expression and in silico Analysis of CIDRα1 Recombinant Protein from Plasmodium Falciparum as a Malaria Subunit Vaccine Candidate

Malaria vaccination is an essential approach to combat malaria. One major protein studied for vaccine development is Plasmodium falciparum erythrocyte membrane protein-1 (PfEMP1). It contains several important domains for malaria pathogenesis. The binding of Cysteine-rich interdomain region α1 (CIDRα1) of PfEMP1 to endothelial protein C receptor (EPCR) is associated with cerebral malaria, while CIDRα1 binding to CD36 has been correlated with uncomplicated malaria. The vital function of CIDRα1 of PfEMP1 makes it a potential vaccine candidate to prevent clinical features of malaria. A long journey of vaccine development can be shortened by the advancement of bioinformatics and biotechnology techniques. This study aimed to express the recombinant CIDRα1 of PfEMP1 and investigate its potency as a malaria subunit vaccine candidate by in silico analysis. Constructed CIDRα1-PfEMP1 was expressed in E. coli BL21(DE3) after induction with Isopropyl ß-D-1-thiogalactopyranoside (IPTG) and purified using Ni-NTA column. In silico analysis on CIDRα1 of PfEMP1 sequence was conducted using ProtParam Tool for its physicochemical properties, Iterative Threading ASSEmbly Refinement (I-TASSER) server and JPred4 program to predict secondary structure, 3D modelling, and ligand-binding site, BepiPred 2.0 and Kolaskar-Tangaonkar to predict B-cell epitope, NetCTL server to determine T-cell epitope, and Vaxijen v2.0 server to predict its antigenicity. The chimeric CIDRα1 of PfEMP1 protein had a 27 kDa molecular weight and was classified as a stable protein. The secondary structure consisted of 6 helices connected with loops. It revealed similarity to CD36-binding protein, EPCR-binding domain, and protein involved in rosetting. The 3D structure modelling demonstrated conserved ligand-binding sites and accessible surface area, which are vital for receptor binding. It had B-cell and T-cell epitopes and was non-allergenic. The properties of the chimeric CIDRα of PfEMP1 indicated its potential as a malaria subunit vaccine candidate. HIGHLIGHTS The binding capacity of CIDRα1 of PfEMP1 to endothelial protein C receptor (EPCR) and CD36 makes it a potential vaccine candidate to prevent clinical malaria The chimeric CIDRα1 of PfEMP1 protein was a stable protein and showed similarity to CD36-binding protein, EPCR-binding domain, and protein involved in rosetting, which demonstrated conserved ligand-binding sites and accessible surface area, which are vital for receptor binding The chimeric CIDRα1 of PfEMP1 protein had B-cell and T-cell epitopes and was non-allergenic in in silico analysis, indicating its potential as a malaria vaccine candidate GRAPHICAL ABSTRACT
Dust and metal column densities in gamma-ray burst host galaxies

In this paper we present the results from the analysis of a sample of 28 gamma-ray burst (GRB) afterglow spectral energy distributions, spanning the X-ray through to near-infrared wavelengths. This is the largest sample of GRB afterglow spectral energy distributions thus far studied, providing a strong handle on the optical depth distribution of soft X-ray absorption and dust-extinction systems in GRB host galaxies. We detect an absorption system within the GRB host galaxy in 79 per cent of the sample, and an extinction system in 71 per cent of the sample, and find the Small Magellanic Cloud (SMC) extinction law to provide an acceptable fit to the host galaxy extinction profile for the majority of cases, consistent with previous findings. The range in the soft X-ray absorption to dust-extinction ratio, N-H,N-X/A(V), in GRB host galaxies spans almost two orders of magnitude, and the typical ratios are significantly larger than those of the Magellanic Clouds or Milky Way. Although dust destruction could be a cause, at least in part, for the large N-H,N-X/A(V) ratios, the good fit provided by the SMC extinction law for the majority of our sample suggests that there is an abundance of small dust grains in the GRB environment, which we would expect to have been destroyed if dust destruction were responsible for the large N-H,N-X/A(V) ratios. Instead, our analysis suggests that the distribution of N-H,N-X/A(V) in GRB host galaxies may be mostly intrinsic to these galaxies, and this is further substantiated by evidence for a strong negative correlation between N-H,N-X/A(V) and metallicity for a subsample of GRB hosts with known metallicity.
Melting at the absolute zero of temperature: Quantum phase transitions in condensed matter

We dedicate this article to our father, Prof. Dr. Guenter Vojta, on the occasion of his 80th birthday. While colleagues appreciate him as an excellent scientist with widespread interests and an amazingly broad knowledge, we see in him the father, teacher, friend, and much more. Thanks to him, we grew up immersed in the fascinating world of physics from an early age. His example and encouragement have crucially influenced our own lives.
Radio emission of magnetars driven by the quasi-linear diffusion.

ABSTRACT In the present paper we study the possibility of generation of electromagnetic waves inthe magnetospheres of radio magnetars by means of the quasi-linear diﬀusion (QLD). Considering the magnetosphere composed of the so-called beam and the plasma com-ponents respectively, we argue that the frozen-in condition will inevitably lead to thegeneration of the unstable cyclotron modes. These modes, via the QLD, will in turninﬂuence the particle distribution function, leading to certain values of the pitch an-gles, thus to an eﬃcient synchrotron mechanism, producing radio photons. We showthat for three known radio magnetars the QLD might be a realistic mechanism forproducing photons in the radio band.Key words: magnetars – radiation mechanisms: non-thermal – plasmas. 1 INTRODUCTIONPulsars since their discovery deserve a great attentionand many aspects of their nature still remain unclear.One of the peculiar class of the pulsars are characterizedby long period of rotation, which in turn leads to verystrong magnetic ﬁelds exceeding the so-called Schwingerlimit, B
Depletion of Fumarate Hydratase, an Essential TCA Cycle Enzyme, Drives Proliferation in a Two-Step Model

Simple Summary Fumarate hydratase (FH) is an evolutionary conserved TCA cycle enzyme and has a moonlight function in the DNA damage response (DDR). FH has a contradictory function, as it is pro-survival through its role in the TCA cycle, yet its loss can drive tumorigenesis. Here, we solve this contradiction and show that in both non-cancerous (HEK-293T) and cancerous cell lines (HepG2), the cell response to FH loss is separated into two distinct time frames. During the early stages of FH loss, cell proliferation and DNA damage repair are inhibited. However, over time, cells overcome the FH loss and form proliferative knockout stable clones. Furthermore, we discovered that the impaired DDR induces mutations enriched in central signaling pathways, such as JAK/STAT3, allowing the cells to circumvent FH and TCA cycle loss. Abstract Fumarate hydratase (FH) is an evolutionary conserved TCA cycle enzyme that reversibly catalyzes the hydration of fumarate to L-malate and has a moonlight function in the DNA damage response (DDR). Interestingly, FH has a contradictory cellular function, as it is pro-survival through its role in the TCA cycle, yet its loss can drive tumorigenesis. Here, we found that in both non-cancerous (HEK-293T) and cancerous cell lines (HepG2), the cell response to FH loss is separated into two distinct time frames based on cell proliferation and DNA damage repair. During the early stages of FH loss, cell proliferation rate and DNA damage repair are inhibited. However, over time the cells overcome the FH loss and form knockout clones, indistinguishable from WT cells with respect to their proliferation rate. Due to the FH loss effect on DNA damage repair, we assumed that the recovered cells bear adaptive mutations. Therefore, we applied whole-exome sequencing to identify such mutated genes systematically. Indeed, we identified recurring mutations in genes belonging to central oncogenic signaling pathways, such as JAK/STAT3, which we validated in impaired FH-KO clones. Intriguingly, we demonstrate that these adaptive mutations are responsible for FH-KO cell proliferation under TCA cycle malfunction.
Predictors of Massive Open Online Courses (MOOC) Learning Satisfaction: A Recipe for Success

Massive Open Online Courses (MOOCs) have recently gained great attention. However, the biggest challenge to the success of MOOCs is their low completion rate. During the lockdown of the COVID-19 pandemic, MOOCs were in high demand by many higher education institutions to replace their face-to-face lessons. MOOCs have great potential to grow and reinvent the way of learning in the 21st century. This study uses the Virtual Learning Environment (VLE) effectiveness model to understand how the five key factors (learner, instructor, course, technology system, and interactivity) influence student learning satisfaction from a holistic approach and determine the best predictor of student learning satisfaction in the MOOC learning environment. A set of online data based on a 5-point Likert scale was collected from 333 undergraduate students from the top five public universities in Malaysia whose students are actively using MOOCs in their learning. The Partial Least Squares Structural Equation Modelling (PLS-SEM) technique was used to analyse the data. The empirical results revealed that all factors significantly influence student learning satisfaction positively. Learner and interactivity factors were the strongest predictors in determining student learning satisfaction in MOOCs. These findings provide an empirically justified framework for developing successful online courses such as MOOCs in higher education.
Atomistic and continuum modeling of non-equilibrium melting of aluminum

MD simulations of the non-equilibrium melting of aluminum are performed both with and without accounting of the electronic subsystem. A continuum model of melting is purposed basing on the obtained MD results, in which the current phase state is described in terms of fields of concentration and size of melting sites. Growth equation for melting areas is derived from the heat fluxes analysis. Nucleation equation for melting sites is formulated basing on the thermofluctuational approach. The method of determination of the model coefficients with using the MD simulation results is purposed. The continuum model is applied to the problem of the non-equilibrium melting of aluminum within the energy absorption area of the high-current electron beam.
Dynamical evolution of black hole subsystems in idealized star clusters

In this paper, globular star clusters which contain a sub-system of stellar-mass black holes (BH) are investigated. This is done by considering two-component models, as these are the simplest approximation of more realistic multi-mass systems, where one component represents the BH population and the other represents all the other stars. These systems are found to undergo a long phase of evolution where the centre of the system is dominated by a dense BH sub-system. After mass segregation has driven most of the BH into a compact sub-system, the evolution of the BH sub-system is found to be influenced by the cluster in which it is contained. The BH sub-system evolves in such a way as to satisfy the energy demands of the whole cluster, just as the core of a one component system must satisfy the energy demands of the whole cluster. The BH sub-system is found to exist for a significant amount of time. It takes approximately 10t_{rh,i}, where t_{rh,i} is the initial half-mass relaxation time, from the formation of the compact BH sub-system up until the time when 90% of the sub-system total mass is lost (which is of order 10^{3} times the half-mass relaxation time of the BH sub-system at its time of formation). Based on theoretical arguments the rate of mass loss from the BH sub-system (\dot{M}_2) is predicted to be -(beta*zeta*M)/(alpha*t_{rh}), where M is the total mass, t_{rh} is the half-mass relaxation time, and alpha, beta, zeta are three dimensionless parameters (see Section 2 for details). An interesting consequence of this is that the rate of mass loss from the BH sub-system is approximately independent of the stellar mass ratio (m_2/m_1) and the total mass ratio (M_2/M_1) (in the range m_2/m_1 >~ 10 and M_2/M_1 ~ 10^{-2}, where m_1, m_2 are the masses of individual low-mass and high-mass particles respectively, and M_1, M_2 are the corresponding total masses).
A semi-analytical method to estimate the slip length of spreading cap-shaped droplets using Cox theory

The Cox-Voinov law on dynamic spreading relates the difference between the cubic values of the apparent contact angle (theta) and the equilibrium contact angle to the instantaneous contact line speed (U). Comparing spreading results with this law requires accurate data of theta and U during the entire process. We consider the case when gravitational forces are negligible and transform the general Cox law in a relationship for the temporal evolution of the spreading radius. For cap-shaped droplets, this enables a comparison of experimental or computational results with Cox theory without the need for instantaneous data of theta and U. The fitting of Cox theory against measured or computed base-radius-over-time curves allows estimating the effective slip length. This is useful for establishing relationships between slip length and parameters in numerical methods for moving contact lines. The procedure is illustrated by numerical simulations for partially wetting droplets employing the coupled level-set volume-of-fluid and phase field methods.
A hadronic minute-scale GeV flare from quasar 3C 279?

The flat spectrum radio quasar 3C 279 is a known $\gamma$-ray variable source that has recently exhibited minute-scale variability at energies $>100$ MeV. One-zone leptonic models for blazar emission are severely constrained by the short timescale variability that implies a very compact emission region at a distance of hundreds of Schwarzschild radii from the central black hole. Here, we investigate a hadronic scenario where GeV $\gamma$-rays are produced via proton synchrotron radiation. We also take into account the effects of the hadronically initiated electromagnetic cascades (EMC). For a $\gamma$-ray emitting region in rough equipartition between particles and kG magnetic fields, located within the broad-line region (BLR), the development of EMC redistributes the $\gamma$-ray luminosity to softer energy bands and eventually leads to broad-band spectra that differ from the observed ones. Suppression of EMC and energy equipartition are still possible, if the $\gamma$-ray emitting region is located beyond the BLR, is fast moving with Doppler factor ($>70$), and contains strong magnetic fields ($>100$ G). Yet, these conditions cannot be easily met in parsec-scale jets, thus disfavouring a proton synchrotron origin of the Fermi-LAT flare.
Optical design of the SuMIRe/PFS spectrograph

The SuMIRe Prime Focus Spectrograph (PFS), developed for the 8-m class SUBARU telescope, will consist of four identical spectrographs, each receiving 600 fibers from a 2394 fiber robotic positioner at the telescope prime focus. Each spectrograph includes three spectral channels to cover the wavelength range [0.38-1.26] um with a resolving power ranging between 2000 and 4000. A medium resolution mode is also implemented to reach a resolving power of 5000 at 0.8 um. Each spectrograph is made of 4 optical units: the entrance unit which produces three corrected collimated beams and three camera units (one per spectral channel: "blue, "red", and “NIR”). The beam is split by using two large dichroics; and in each arm, the light is dispersed by large VPH gratings (about 280x280mm). The proposed optical design was optimized to achieve the requested image quality while simplifying the manufacturing of the whole optical system. The camera design consists in an innovative Schmidt camera observing a large field-of-view (10 degrees) with a very fast beam (F/1.09). To achieve such a performance, the classical spherical mirror is replaced by a catadioptric mirror (i.e meniscus lens with a reflective surface on the rear side of the glass, like a Mangin mirror). This article focuses on the optical architecture of the PFS spectrograph and the perfornance achieved. We will first described the global optical design of the spectrograph. Then, we will focus on the Mangin-Schmidt camera design. The analysis of the optical performance and the results obtained are presented in the last section.