Miracle-dz/UniFAR-FTUs huggingface dataset:
Design rules for dislocation filters

The efficacy of strained layer threading dislocation filter structures in single crystal epitaxial layers is evaluated using numerical modeling for (001) face-centred cubic materials, such as GaAs or Si1− x Ge x , and (0001) hexagonal materials such as GaN. We find that threading dislocation densities decay exponentially as a function of the strain relieved, irrespective of the fraction of threading dislocations that are mobile. Reactions between threading dislocations tend to produce a population that is a balanced mixture of mobile and sessile in (001) cubic materials. In contrast, mobile threading dislocations tend to be lost very rapidly in (0001) GaN, often with little or no reduction in the immobile dislocation density. The capture radius for threading dislocation interactions is estimated to be approximately 40 nm using cross section transmission electron microscopy of dislocation filtering structures in GaAs monolithically grown on Si. We find that the minimum threading dislocation density that can be obtained in any given structure is likely to be limited by kinetic effects to approximately 104–105 cm−2.
Superconductivity and the effects of pressure and structure in single-crystalline SrNi 2 P 2

Heat capacity, magnetic susceptibility, and resistivity of SrNi{sub 2}P{sub 2} single crystals are presented, illustrating the structural transition at 325 K, and bulk superconductivity at 1.4 K. The magnitude of {Tc}, fits to the heat capacity data, the small upper critical field H{sub c2} = 390 Oe, and {kappa} = 2.1 suggests a conventional fully gapped superconductor. With applied pressure we find that superconductivity persists into the so-called 'collapsed tetragonal' phase, although the transition temperature is monotonically suppressed with increasing pressure. This argues that reduced dimensionality can be a mechanism for increasing the transition temperatures of layered NiP, as well as layered FeAs and NiAs, superconductors.
Morphological and chemical characteristics of fruits and seeds of two cultivars of Opuntia ficus-indica (L.) Miller from northern Morocco

Fruits of two cultivars of Opuntia ficus-indica (the “Hajria” and “Dellahia” cultivars) growing in the Tetouan and Al-Hoceima provinces of northern Morocco were harvested at the same ripening stage. The chemical properties (total lipids, proteins, total sugars, moisture, and dry matter) of the peel and seeds were determined and the morphological characteristics (whole fruit weight, pulp weight, peel weight, and the number and weight of fertilized and aborted seeds) of the fruits and their seeds from both cultivars were compared. Surface-sterilized seeds were separated into six groups according to their length and germinated on Murashige and Skoog basal culture medium. Seed viability, by analyzing the correlation between (1) germination rate and seed length, and (2) germination rate and seed weight was determined. Results showed that the province or cultivar factor had significant effects on the morphological characteristics of fruits and seeds. Fruit and pulp weights were positively correlated with the seed number. In addition, a marked difference in the sugar content of the peel was observed (57.29% in the ‘‘Dellahia’’ cultivar compared to 36.66% in the “Hajria” cultivar). The seeds of the “Dellahia” cultivar contained 10.41% fat and 8.12% protein, whereas the seeds of “Hajria” contained 12.27% fat and 8.67% protein. Seed viability was assured from a length of 3.5 mm in both cultivars. The seed germination rate correlated positively with increased length and weight; however, this rate was significantly different between the two cultivars.
Chirality-dependent phonon-limited resistivity in multiple layers of graphene

We develop a theory for the temperature and density dependence of phonon-limited resistivity $\rho(T)$ in bilayer and multilayer graphene, and compare with the corresponding monolayer result. For the unscreened case, we find $\rho \approx C T$ with $C \propto v_{\rm F}^{-2}$ in the high-temperature limit, and $\rho \approx A T^4$ with $A \propto v_{\rm F}^{-2} k_{\rm F}^{-3}$ in the low-temperature Bloch-Gr\"uneisen limit, where $v_{\rm F}$ and $k_{\rm F}$ are Fermi velocity and Fermi wavevector, respectively. If screening effects are taken into account, $\rho \approx C T$ in the high-temperature limit with a renormalized $C$ which is a function of the screening length, and $\rho \approx A T^6$ in the low-temperature limit with $A \propto k_{\rm F}^{-5}$ but independent of $v_{\rm F}$. These relations hold in general with $v_{\rm F}$ and a chiral factor in $C$ determined by the specific chiral band structure for a given density.
INVESTIGATION OF SYSTEMATIC EFFECTS IN KEPLER DATA: SEASONAL VARIATIONS IN THE LIGHT CURVE OF HAT-P-7b

With years of Kepler data currently available, the measurement of variations in planetary transit depths over time can now be attempted. To do so, it is of primary importance to understand which systematic effects may affect the measurement of transits. We aim to measure the stability of Kepler measurements over years of observations. We present a study of the depth of about 500 transit events of the Hot Jupiter HAT-P-7b, using 14 quarters (Q0–Q13) of data from the Kepler satellite. We find a systematic variation in the depth of the primary transit, related to quarters of data and recurring yearly. These seasonal variations are about 1%. Within seasons, we find no evidence for trends. We speculate that the cause of the seasonal variations could be unknown field crowding or instrumental artifacts. Our results show that care must be taken when combining transits throughout different quarters of Kepler data. Measuring the relative planetary radius of HAT-P-7b without taking these systematic effects into account leads to unrealistically low error estimates. This effect could be present in all Kepler targets. If so, relative radius measurements of all Hot Jupiters to a precision much better than 1% are unrealistic.
THE PHYSICAL CONDITIONS OF A LENSED STAR-FORMING GALAXY AT z = 1.7

We report rest-frame optical Keck/NIRSPEC spectroscopy of the bright lensed galaxy RCSGA 032727-132609 at z = 1.7037. From precise measurements of the nebular lines, we infer a number of physical properties: redshift, extinction, star formation rate, ionization parameter, electron density, electron temperature, oxygen abundance, and N/O, Ne/O, and Ar/O abundance ratios. The limit on [O iii] 4363 Å tightly constrains the oxygen abundance via the “direct” or Te method, for the first time in an average-metallicity galaxy at z ∼ 2. We compare this result to several standard “bright-line” O abundance diagnostics, thereby testing these empirically-calibrated diagnostics in situ. Finally, we explore the positions of lensed and unlensed galaxies in standard diagnostic diagrams, and the diversity of ionization conditions and mass–metallicity ratios at z = 2.
Direct observation of the M1 transition between the ground state fine structure splitting of W VIII

We present direct observation of the M1 transition between the fine structure splitting in the 4f13 5s2 5p6 2F ground state of W VIII. The spectroscopic data of few-times ionized tungsten ions are important for the future ITER diagnostics, but there is a serious lack of data. The present study is part of an ongoing effort to solve this lack. Emission from the tungsten ions produced and trapped in a compact electron beam ion trap is observed with a Czerny-Turner visible spectrometer. Spectra in the EUV range are also observed at the same time to help the identification of the previously-unreported visible lines. The observed wavelength 574.47 pm 0.03 nm (air), which corresponds to the fine structure splitting of 17402.5 pm 0.9 cm-1, shows reasonable agreement with the previously reported value 17410 pm 5 cm-1 obtained indirectly through the analysis of EUV spectra [Ryabtsev et al., Atoms 3 (2015) 273].
Research Productivity among Scholarly Communication Librarians

Introduction. A growing number of academic libraries have specialized their support for scholarly communication by creating positions or expanding units with a focus on providing relevant services. This study was undertaken to explore the extent to which librarians with scholarly communication responsibilities produce research and scholarship, their motivations for doing so, the nature of that productivity, and the perceived impact of that activity on their professional responsibilities. Method. The authors administered a survey of librarians who identified as having their primary job responsibilities in scholarly communication. Results. Almost all study participants produced their own scholarly work. However, a high percentage indicated they received no relevant training in their library degree programs, and the majority experienced imposter syndrome pertaining to their own scholarship. Many respondents indicated the term “scholarly communication(s)” was in their professional titles, but open education services were also part of their portfolios. Although most respondents were motivated to produce research by institutional expectations for promotion and tenure, greater percentages were driven by personal or professional interests. In addition, participants indicated a strong correlation between producing their own scholarship and their ability to effectively carry out their professional responsibilities. Discussion. There may be an emerging convention for scholarly communication librarianship: one that includes open education services. Findings suggest a need for scholarly communication training to be more prominent in library degree programs. They also point to the utility of making research production a job requirement, regardless of institutional expectations for professional advancement. Conclusion. The authors argue for adjustments in library education curricula and the inclusion of research production in the portfolios of scholarly communication librarians. Future research directions are proposed.
Molecular investigations of comets C/2002 X5 (Kudo-Fujikawa), C/2002 V1 (NEAT), and C/2006 P1 (McNaught) at small heliocentric distances

We present unique spectroscopic radio observations of comets C/2002 X5 (Kudo-Fujikawa), C/2002 VI (NEAT), and C/2006 P1 (McNaught), which came within r h ≈ 0.2 AU of the Sun in 2003 and 2007. The molecules OH, HCN, HNC, CS, and CH 3 OH were detected in each of these comets when they were exposed to strong heating from the Sun. HC 3 N and HCO + were detected in comets C/2002 X5 and C/2006 PI, respectively. We show that in these very productive comets close to the Sun screening of the photodissociation by the Sun UV radiation plays a non-negligible role. Acceleration of the gas expansion velocity and day-night asymmetry is also measured and modeled. The CS photodissociation lifetime was constrained to be about 2.5 x 10 ―5 s ―1 at r h = I AU. The relative abundances are compared to values determined from more distant observations of C/2002 X5 or other comets. A high HNC/HCN production-rate ratio, in the range 10-30% between 0.5 and 0.1 AU from the Sun, is measured. The trend for a significant enrichment in CS in cometary comae (CS/HCN ∝ r ―0.8 h ) is confirmed in all three comets. The CH 3 OH/HCN production rate ratio decreases at low r h . The HC 3 N/HCN production rate ratio in comet C/2002 X5 is four times higher than measured in any other comet.
The quiet Sun magnetic field observed with ZIMPOL on THEMIS - I. The probability density function

Context. The quiet Sun magnetic field probability density function (PDF) remains poorly known. Modeling this field also introduces a magnetic filling factor that is also poorly known. With these two quantities, PDF and filling factor, the statistical description of the quiet Sun magnetic field is complex and needs to be clarified. Aims. In the present paper, we propose a procedure that combines direct determinations and inversion results to derive the magnetic field vector and filling factor, and their PDFs. Methods. We used spectro-polarimetric observations taken with the ZIMPOL polarimeter mounted on the THEMIS telescope. The target was a quiet region at disk center. We analyzed the data by means of the UNNOFIT inversion code, with which we inferred the distribution of the mean magnetic field $\alpha B$, α being the magnetic filling factor. The distribution of α was derived by an independent method, directly from the spectro-polarimetric data. The magnetic field PDF $p(B)$ could then be inferred. By introducing a joint PDF for the filling factor and the magnetic field strength, we have clarified the definition of the PDF of the quiet Sun magnetic field when the latter is assumed not to be volume-filling. Results. The most frequent local average magnetic field strength is found to be 13 G. We find that the magnetic filling factor is related to the magnetic field strength by the simple law $\alpha = B_1/B$ with $B_1 = 15$ G. This result is compatible with the Hanle weak-field determinations, as well as with the stronger field determinations from the Zeeman effect (kGauss field filling 1–2% of space). From linear fits, we obtain the analytical dependence of the magnetic field PDF. Our analysis has also revealed that the magnetic field in the quiet Sun is isotropically distributed in direction. Conclusions. We conclude that the quiet Sun is a complex medium where magnetic fields having different field strengths and filling factors coexist. Further observations with a better polarimetric accuracy are, however, needed to confirm the results obtained in the present work.
Using Motor Tempi to Understand Rhythm and Grammatical Skills in Developmental Language Disorder and Typical Language Development

Abstract Children with developmental language disorder (DLD) show relative weaknesses on rhythm tasks beyond their characteristic linguistic impairments. The current study compares preferred tempo and the width of an entrainment region for 5- to 7-year-old typically developing (TD) children and children with DLD and considers the associations with rhythm aptitude and expressive grammar skills in the two populations. Preferred tempo was measured with a spontaneous motor tempo task (tapping tempo at a comfortable speed), and the width (range) of an entrainment region was measured by the difference between the upper (slow) and lower (fast) limits of tapping a rhythm normalized by an individual’s spontaneous motor tempo. Data from N = 16 children with DLD and N = 114 TD children showed that whereas entrainment-region width did not differ across the two groups, slowest motor tempo, the determinant of the upper (slow) limit of the entrainment region, was at a faster tempo in children with DLD vs. TD. In other words, the DLD group could not pace their slow tapping as slowly as the TD group. Entrainment-region width was positively associated with rhythm aptitude and receptive grammar even after taking into account potential confounding factors, whereas expressive grammar did not show an association with any of the tapping measures. Preferred tempo was not associated with any study variables after including covariates in the analyses. These results motivate future neuroscientific studies of low-frequency neural oscillatory mechanisms as the potential neural correlates of entrainment-region width and their associations with musical rhythm and spoken language processing in children with typical and atypical language development.
Oxygen-vacancy-related relaxation and scaling behaviors of Bi 0.9 La 0.1 Fe 0.98 Mg 0.02 O 3 ferroelectric thin films

Oxygen-vacancies-related dielectric relaxation and scaling behaviors of ${\text{Bi}}_{0.9}{\text{La}}_{0.1}{\text{Fe}}_{0.98}{\text{Mg}}_{0.02}{\text{O}}_{3}$ (BLFM) thin film have been investigated by temperature-dependent impedance spectroscopy from $40\text{ }\ifmmode^\circ\else\textdegree\fi{}\text{C}$ up to $200\text{ }\ifmmode^\circ\else\textdegree\fi{}\text{C}$. We found that hopping electrons and single-charged oxygen vacancies $({V}_{\text{O}}^{\ifmmode\bullet\else\textbullet\fi{}})$ coexist in the BLFM thin film and make contribution to dielectric response of grain and grain boundary, respectively. The activation energy for ${V}_{\text{O}}^{\ifmmode\bullet\else\textbullet\fi{}}$ is shown to be 0.94 eV in the whole temperature range investigated whereas the distinct activation energies for electrons are 0.136 eV below $110\text{ }\ifmmode^\circ\else\textdegree\fi{}\text{C}$ and 0.239 eV above $110\text{ }\ifmmode^\circ\else\textdegree\fi{}\text{C}$ in association with hopping along the ${\text{Fe}}^{2+}\text{\ensuremath{-}}{V}_{\text{O}}^{\ifmmode\bullet\else\textbullet\fi{}}{\text{-Fe}}^{3+}$ chain and hopping between ${\text{Fe}}^{2+}{\text{-Fe}}^{3+}$, respectively, indicating different hopping processes for electrons. Moreover, it has been found that hopping electrons are in the form of long-range movement while localized and long-range movement of oxygen vacancies coexist in BLFM film. The Cole-Cole plots in modulus formalism show a polydispersive nature of relaxation for oxygen vacancies and a single relaxation time for hopping electrons. The scaling behavior of modulus spectra further suggests that the distribution of relaxation times for oxygen vacancies is temperature independent.
RESONANT REPULSION OF KEPLER PLANET PAIRS

Planetary systems discovered by the Kepler space telescope exhibit an intriguing feature. While the period ratios of adjacent low-mass planets appear largely random, there is a significant excess of pairs that lie just wide of resonances and a deficit on the near side. We demonstrate that this feature naturally arises when two near-resonant planets interact in the presence of weak dissipation that damps eccentricities. The two planets repel each other as orbital energy is lost to heat. This moves near-resonant pairs just beyond resonance, by a distance that reflects the integrated dissipation they experienced over their lifetimes. We find that the observed distances may be explained by tides if tidal dissipation is unexpectedly efficient (tidal quality factor ∼10). Once the effect of resonant repulsion is accounted for, the initial orbits of these low-mass planets show little preference for resonances. This could constrain their origin.
The central density of R136 in 30 Doradus

The central density rho_0 of a stellar cluster is an important physical parameter for determining its evolutionary and dynamical state. How much mass segregation there is, or whether the cluster has undergone core collapse both depends on rho_0. We reanalyze the results of a previous paper that gives the mass density profile of R136 and combine them with both a conservative upper limit for the core parameter and a more uncertain recent measurement. We thus place a lower limit on rho_0 under reasonable and defensible assumptions about the IMF, finding rho_0 >~ 1.5x10^4 Msun/pc^3 for the conservative assumption a < 0.4 pc for the cluster core parameter. If we use the lower, but more uncertain value a = 0.025 pc, the central density estimate becomes greater than 10^7 Msun/pc^3. A mechanism based on the destruction of a large number of circumstellar disks is posited to explain the hitherto unexplained increase in reddening presented in that same work.
Dynamical locking of the chiral and the deconfinement phase transition in QCD

We study the fixed-point structure of four-fermion interactions in two-flavor QCD with Nc colors close to the finite-temperature phase boundary. In particular, we analyze how the fixed-point structure of four-fermion interactions is related to the confining dynamics in the gauge sector. We show that there exists indeed a mechanism which dynamically locks the chiral phase transition to the deconfinement phase transition. This mechanism allows us to determine a window for the values of physical observables in which the two phase transitions lie close to each other.
Evidence for top-heavy stellar initial mass functions with increasing density and decreasing metallicity

ABSTRACT Residual-gas expulsion after cluster formation has recently been shown to leave animprint in the low-mass present-day stellar mass function (PDMF) which allowedthe estimation of birth conditions of some Galactic globular clusters (GCs) such asmass, radius and star formation eﬃciency. We show that in order to explain theircharacteristics (masses, radii, metallicity, PDMF) their stellar initial mass function(IMF) must have been top-heavy. It is found that the IMF is required to becomemore top-heavy the lower the cluster metallicity and the larger the pre-GC cloud-core density are. The deduced trends are in qualitative agreement with theoreticalexpectation. The results are consistent with estimates of the shape of the high-massend of the IMF in the Arches cluster, Westerlund 1, R136 and NGC 3603, as wellas with the IMF independently constrained for ultra-compact dwarf galaxies (UCDs). The latter suggests that GCs and UCDs might have formed along the same channel orthat UCDs formed via mergers of GCs. A fundamental plane is found which describesthe variation of the IMF with density and metallicity of the pre-GC cloud-cores. Theimplications for the evolution of galaxies and chemical enrichment over cosmologicaltimes are expected to be major.Keywords: stars: formation – stars: mass-function – stars: early-type – stars: late-type – globular clusters: general
The finite difference methods and its stability for glycolysis model in one dimension

The Glycolysis model has been solved numerically in one dimension by using two finite differences methods: explicit and Crank-Nicolson method and we were found that the explicit method is simpler while the Crank-Nicolson is more accurate. Also, we found that explicit method is conditionally stable while Crank-Nicolson method is unconditionally stable.
Prognostic factors for persistent pain after a distal radius fracture: a systematic review

Introduction The aim of this systematic review was to synthesize the evidence regarding prognostic factors for persistent pain, including Complex Regional Pain Syndrome (CRPS), after a distal radius fracture (DRF), a common condition after which persistent pain can develop. Methods Medline, Pubmed, Embase, Psychinfo, CINAHL, BNI, AMED and the Cochrane Register of Clinical Trials were searched from inception to May 2021 for prospective longitudinal prognostic factor studies investigating persistent pain in adults who had sustained a DRF. The Quality in Prognostic Studies (QUIPS) tool and Grading of Recommendations, Assessment, Development and Evaluation (GRADE) framework were used to assess the strength of evidence. Results A search yielded 440 studies of which 7 studies met full eligibility criteria. From five studies we found low evidence for high baseline pain or an ulnar styloid fracture as prognostic factors for persistent pain, and very low evidence for diabetes or older age. From two studies, investigating an outcome of CRPS, there was low evidence for high baseline pain, slow reaction time, dysynchiria, swelling and catastrophising as prognostic factors, and very low evidence for depression. Sex was found not to be a prognostic factor for CRPS or persistent pain. Conclusions The associations between prognostic factors and persistent pain following a DRF are unclear. The small number of factors investigated in more than one study, along with poor reporting and methodological limitations contributed to an assessment of low to very low strength of evidence. Further prospective studies, investigating psychosocial factors as candidate predictors of multidimensional pain outcomes are recommended.