Miracle-dz/UniFAR-FTUs huggingface dataset:
On the location of the ring around the dwarf planet Haumea

The recently discovered ring around the dwarf planet (136108) Haumea is located near the 1:3 resonance between the orbital motion of the ring particles and the spin of Haumea. In the current work is studied the dynamics of individual particles in the region where is located the ring. Using the Poincar\'e Surface of Section technique, the islands of stability associated with the 1:3 resonance are identified and studied. Along all its existence this resonance showed to be doubled, producing pairs of periodic and quasi-periodic orbits. The fact of being doubled introduces a separatrix, which generates a chaotic layer that significantly reduces the size of the stable regions of the 1:3 resonance. The results also show that there is a minimum equivalent eccentricity ($e_{1:3}$) for the existence of such resonance. This value seems to be too high to keep a particle within the borders of the ring. On the other hand, the Poincar\'e Surface of Sections show the existence of much larger stable regions, but associated with a family of first kind periodic orbits. They exist with equivalent eccentricity values lower than $e_{1:3}$, and covering a large radial distance, which encompasses the region of the Haumea's ring. Therefore, this analysis suggests the Haumea's ring is in a stable region associated with a first kind periodic orbit instead of the 1:3 resonance.
PROPERTIES OF OPTICALLY SELECTED SUPERNOVA REMNANT CANDIDATES IN M33

Narrowband images covering strong emission lines are efficient for surveying supernova remnants (SNRs) in nearby galaxies. Using the narrowband images provided by the Local Group Galaxy Survey, we searched for SNRs in M33. Culling the objects with enhanced [S ii]/Hα and round morphology in the continuum-subtracted Hα and [S ii] images, we produced a list of 199 sources. Among them, 79 are previously unknown. Their progenitor and morphology types were classified. A majority of the sample (170 objects) are likely remnants of core-collapse supernovae (SNe), and 29 are remnants of Type Ia SNe. The cumulative size distribution of these objects is found to be similar to that of the M31 remnants derived in a similar way. We obtain a power-law slope, α = 2.38 ± 0.05. Thus, a majority of the sources are considered to be in the Sedov–Taylor phase, consistent with previous findings. The histogram of the emission-line ratio ([S ii]/Hα) of the remnants has two concentrations at [S ii]/Hα ∼ 0.55 and ∼0.8, as in M31. Interestingly, LX (and L20 cm) of the compact center-bright objects are correlated with their optical luminosity. The remnants with X-ray emission have brighter optical surface brightnesses and smaller diameters than those without X-ray emission.
Deterministic aperiodic composite lattice-structured silicon thin films for photon management

Exotic manipulation of the flow of photons in nanoengineered semiconductor materials with an aperiodic distribution of nanostructures plays a key role in efficiency-enhanced and industrially viable broadband photonic technologies. Through a generic deterministic nanotechnological route, in addition to periodic, transversely quasicrystallographic or disordered random photonic lattices, here we show scalable nanostructured semiconductor thin films on large area nanoimprinted substrates up to 4cm^2 with advanced functional features of aperiodic composite nanophotonic lattices having tailorable supercell tiles. The richer Fourier spectra of the presented artificially nanostructured materials with well-defined lattice point morphologies are designed functionally akin to two-dimensional incommensurate intergrowth aperiodic lattices-comprising periodic photonic crystals and in-plane quasicrystals as subgroups. The composite photonic lattice-structured crystalline silicon thin films with tapered nanoholes or nanocone-nanoholes are presented showing up to +30 % achievable short circuit current density in comparison to a periodic counterpart where as it is up to +190 % in comparison to a reference unstructured silicon thin film of 300 nanometers of thickness. In view of scalable bottom-up integrated device fabrication processes, the structural analysis is further extended to liquid phase crystallized double-side-textured deterministic aperiodic lattice-structured 10 micrometers thick large area crystalline silicon film.
Non-relativistic bound states in a moving thermal bath

We study the propagation of non-relativistic bound states moving at constant velocity across a homogeneous thermal bath and we develop the effective field theory which is relevant in various dynamical regimes. We consider values of the velocity of the bound state ranging from moderate to highly relativistic and temperatures at all relevant scales smaller than the mass of the particles that form the bound state. In particular, we consider two distinct temperature regimes, corresponding to temperatures smaller or higher than the typical momentum transfer in the bound state. For temperatures smaller or of the order of the typical momentum transfer, we restrict our analysis to the simplest system, a hydrogen-like atom. We build the effective theory for this system first considering moderate values of the velocity and then the relativistic case. For large values of the velocity of the bound state, the separation of scales is such that the corresponding effective theory resembles the soft collinear effective theory (SCET). For temperatures larger than the typical momentum transfer we also consider muonic hydrogen propagating in a plasma which contains photons and massless electrons and positrons, so that the system resembles very much heavy quarkonium in a thermal medium of deconfined quarks and gluons. We study the behavior of the real and imaginary part of the static two-body potential, for various velocities of the bound state, in the hard thermal loop approximation. We find that Landau damping ceases to be the relevant mechanism for dissociation from a certain "critical" velocity on in favor of screening. Our results are relevant for understanding how the properties of heavy quarkonia states produced in the initial fusion of partons in the relativistic collision of heavy ions are affected by the presence of an equilibrated quark-gluon plasma.
Single-cell sequencing of human midbrain reveals glial activation and a Parkinson-speci ﬁ c neuronal state

ﬁ commentary on this article. Idiopathic Parkinson ’ s disease is characterized by a progressive loss of dopaminergic neurons, but the exact disease aetiology remains largely unknown. To date, Parkinson ’ s disease research has mainly focused on nigral dopaminergic neurons, although recent studies suggest disease-related changes also in non-neuronal cells and in midbrain regions beyond the substantia nigra. While there is some evidence for glial involvement in Parkinson ’ s disease, the molecular mechanisms remain poorly understood. The aim of this study was to characterize the contribution of all cell types of the midbrain to Parkinson ’ s disease pathology by single-nuclei RNA sequencing and to assess the cell type-speci ﬁ c risk for Parkinson ’ s disease using the latest genome-wide association study. We pro ﬁ led . 41 000 single-nuclei transcriptomes of post-mortem midbrain from six idiopathic Parkinson ’ s disease patientsand ﬁ veage-/sex-matchedcontrols.Tovalidateour ﬁ ndingsinaspatialcontext,weutilizedimmunolabelling of the same tissues. Moreover, we analysed Parkinson ’ s disease-associated risk enrichment in genes with cell type-speci ﬁ c expression patterns. We discovered a neuronal cell cluster characterized by CADPS2 overexpression and low TH levels, which was exclusively present in idiopathic Parkinson ’ s disease midbrains. Validation analyses in la-ser-microdissected neurons suggest that this cluster represents dysfunctional dopaminergic neurons. With regard to glial cells, we observed an increase in nigral microglia in Parkinson ’ s disease patients. Moreover, nigral idiopathic Parkinson ’ s disease microglia were more amoeboid, indicating an activated state. We also discovered a reduction in idiopathic Parkinson ’ s disease oligodendrocyte numbers with the remaining cells being characterized by a stress-in-duced upregulation of S100B . Parkinson ’ s disease riskvariants were associated withglia- and neuron-speci ﬁ c gene ex-pressionpatterns in idiopathic Parkinson ’ s disease cases. Furthermore, astrocytes and microglia presented idiopathic Parkinson ’ s disease-speci ﬁ c cell proliferation and dysregulation of genes related to unfolded protein response and cytokine signalling. While reactive patient astrocytes showed CD44 overexpression, idiopathic Parkinson ’ s disease microglia revealed a pro-in ﬂ ammatory trajectory characterized by elevated levels of IL1B , GPNMB and HSP90AA1 . Taken together, we generated the ﬁ rst single-nuclei RNA sequencing dataset from the idiopathic Parkinson ’ s disease midbrain, which highlights a disease-speci ﬁ c neuronal cell cluster as well as ‘ pan-glial ’ activation as a central mech-anisminthepathologyofthemovementdisorder.This ﬁ ndingwarrantsfurtherresearchintoin ﬂ ammatorysignalling and immunomodulatory treatments in Parkinson ’ s disease. analysis of done using snRNA-seq
THE DYNAMICAL EVOLUTION OF STELLAR BLACK HOLES IN GLOBULAR CLUSTERS

Our current understanding of the stellar initial mass function and massive star evolution suggests that young globular clusters (GCs) may have formed hundreds to thousands of stellar-mass black holes (BHs), the remnants of stars with initial masses from ∼20–100 M☉. Birth kicks from supernova explosions may eject some BHs from their birth clusters, but most should be retained. Using a Monte Carlo method we investigate the long-term dynamical evolution of GCs containing large numbers of stellar BHs. We describe numerical results for 42 models, covering a broad range of realistic initial conditions, including up to 1.6 × 106 stars. In almost all models we find that significant numbers of BHs (up to ∼103) are retained all the way to the present. This is in contrast to previous theoretical expectations that most BHs should be ejected dynamically within a few gigayears The main reason for this difference is that core collapse driven by BHs (through the Spitzer “mass segregation instability”) is easily reverted through three-body processes, and involves only a small number of the most massive BHs, while lower-mass BHs remain well-mixed with ordinary stars far from the central cusp. Thus the rapid segregation of stellar BHs does not lead to a long-term physical separation of most BHs into a dynamically decoupled inner core, as often assumed previously. Combined with the recent detections of several BH X-ray binary candidates in Galactic GCs, our results suggest that stellar BHs could still be present in large numbers in many GCs today, and that they may play a significant role in shaping the long-term dynamical evolution and the present-day dynamical structure of many clusters.
THE DRIVER OF CORONAL MASS EJECTIONS IN THE LOW CORONA: A FLUX ROPE

Recent Solar Dynamic Observatory observations reveal that coronal mass ejections (CMEs) consist of a multi-temperature structure: a hot flux rope and a cool leading front (LF). The flux rope first appears as a twisted hot channel in the Atmospheric Imaging Assembly (AIA) 94 Å and 131 Å passbands. The twisted hot channel initially lies along the polarity inversion line and then rises and develops into a semi-circular flux-rope-like structure during the impulsive acceleration phase of CMEs. In the meantime, the rising hot channel compresses the surrounding magnetic field and plasma, which successively stack into the CME LF. In this paper, we study in detail two well-observed CMEs that occurred on 2011 March 7 and 2011 March 8, respectively. Each of them is associated with an M-class flare. Through a kinematic analysis we find that (1) the hot channel rises earlier than the first appearance of the CME LF and the onset of the associated flare and (2) the speed of the hot channel is always faster than that of the LF, at least in the field of view of AIA. Thus, the hot channel acts as a continuous driver of the CME formation and eruption in the early acceleration phase. Subsequently, the two CMEs in white-light images can be well reproduced by the graduated cylindrical shell flux rope model. These results suggest that the pre-existing flux rope plays a key role in CME initiation and formation.
Corrigendum: The Plebanski sectors of the EPRL vertex

We correct what amounts to a sign error in the proof of part (i) of theorem 3. The Plebanski sectors isolated by the linear simplicity constraints do not change—they are still the three sectors (deg), (II+) and (II−). What changes is the characterization of the continuum Plebanski two-form corresponding to the first two terms in the asymptotics of the EPRL vertex amplitude for Regge-like boundary data. These two terms do not correspond to the Plebanski sectors (II+) and (II−), but rather to the two possible signs of the product of the sign of the sector—+1 for (II+) and −1 for (II−)—and the sign of the orientation ϵIJKLBIJ∧BKL determined by BIJ. This is consistent with what one would expect, as this is exactly the sign which classically relates the BF action, in the Plebanski sectors (II+) and (II−), to the Einstein–Hilbert action, whose discretization is the Regge action appearing in the asymptotics.
Nonlinear Simulations of the Heat-Flux-driven Buoyancy Instability and Its Implications for Galaxy Clusters

In low-collisionality plasmas heat flows almost exclusively along magnetic field lines and the condition for stability to convection is modified from the standard Schwarzschild criterion. We present local two- and three-dimensional simulations of a new heat-flux-driven buoyancy instability (the HBI) that occurs when the temperature in a plasma decreases in the direction of gravity. We find that the HBI drives a convective dynamo that amplifies an initially weak magnetic field by a factor of ~20. In simulations that begin with the magnetic field aligned with the temperature gradient, the HBI saturates by rearranging the magnetic field lines to be almost purely perpendicular to the initial temperature gradient. This magnetic field reorientation results in a net heat flux through the plasma that is less than 1% of the field-free (Spitzer) value. We show that the HBI is likely to be present in the cool cores of clusters of galaxies between ~0.1-100 kpc, where the temperature increases outward. The saturated state of the HBI suggests that inward thermal conduction from large radii in clusters is unlikely to solve the cooling flow problem. Finally, we also suggest that the HBI may contribute to suppressing conduction across cold fronts in galaxy clusters.
Rangeland Pasture Management Strategies during Drought among Pastoralists in Kajiado County, Kenya

- Pastoral communities have all along developed local mechanisms for managing forage resources to cope with recurrent severe droughts. Unfortunately, these practices have been suppressed and communities are struggling from losses succumbed by effects of drought on livestock feeds and water. In Kenya pastoral production system supplies the largest percentage of beef to the market as compared to the private sector. However, the study found out pastoralists have inadequate knowledge and sufficient training on pasture management contributing to low level of pasture conservation during periods of excess pasture. The frequently practiced methods were traditional herd tethering and migration. A small fraction of pastoralists adopted and practiced modern systems such as Paddocking, Zero grazing, hay making and use of other supplementary feeds. In addition, water harvesting technologies to reduce the possibility of rivalry and conflict between and within communities arising from limited water supply during drought should be promoted. There is an urgent call for all stakeholders in the pastoral areas of Kajiado East to establish sustainable strategies to accelerate capacity building in pasture resource management. Abstract- Pastoral communities have all along developed local mechanisms for managing forage resources to cope with recurrent severe droughts. Unfortunately, these practices have been suppressed and communities are struggling from losses succumbed by effects of drought on livestock feeds and water. In Kenya pastoral production system supplies the largest percentage of beef to the market as compared to the private sector. However, the study found out pastoralists have inadequate knowledge and sufficient training on pasture management contributing to low level of pasture conservation during periods of excess pasture. The frequently practiced methods were traditional herd tethering and migration. A small fraction of pastoralists adopted and practiced modern systems such as Paddocking, Zero grazing, hay making and use of other supplementary feeds. In addition, water harvesting technologies to reduce the possibility of rivalry and conflict between and within communities arising from limited water supply during drought should be promoted. There is an urgent call for all stakeholders in the pastoral areas of Kajiado East to establish sustainable strategies to accelerate capacity building in pasture resource management.
SPECTRAL VARIABILITY OF IRAS 18325-5926 AND CONSTRAINTS ON THE GEOMETRY OF THE SCATTERING MEDIUM

We analyze Suzaku and XMM-Newton data of the highly variable Seyfert 2, IRAS 18325-5926. The spectra of the source are well modeled as a primary component described as an absorbed power law and a secondary power-law component which is consistent with being scattered emission from an on-axis extended highly ionized medium. We show that while the primary component varies on a wide range of timescales from 104–108 s, the scattered emission is variable only on timescales longer than 105 s. This implies that the extent of the scattering medium is greater than 1016 cm. The ratio of the scattered to primary flux (∼0.03) implies a column density for the scattering medium to be ∼1023 cm−2. We argue that for such a medium to be highly ionized it must be located less than 1017 cm from the X-ray source. Thus, we localize the position and extent of scattering region to be ∼a few × 1016 cm, with an average particle density of ∼106 cm−3. We consider the physical interpretation of these results, and as an aside we confirm the presence of a broad iron line emission in both the XMM-Newton and Suzaku observations.
HD 210111: a new λ Bootis-type spectroscopic binary system

The small group of ? Bootis stars comprises late B- to early F-type stars, with moderate to extreme (up to a factor of 100) surface underabundances of most Fe-peak elements and solar abundances of lighter elements (C, N, O and S). The main mechanisms responsible for this phenomenon are atmospheric diffusion, meridional mixing and accretion of material from their surroundings. In particular, spectroscopic binary (SB) systems with ? Bootis-type components are very important to investigate the evolutionary status and accretion process in more detail. For HD 210111, d Scuti-type pulsation was also found, which gives the opportunity to use the tools of asteroseismology for further investigations. The latter could result in strict constraints for the amount of diffusion for this star. Together with models for the accretion and its source, this provides a unique opportunity to shed more light on these important processes. We present classification and high-resolution spectra for HD 210111. A detailed investigation of the most likely combinations of single star components was performed. For this, composite spectra with different stellar astrophysical parameters were calculated and compared to the observations to find the best-fitting combination. HD 210111 comprises two equal (within the estimated errors) stars with Teff= 7400 K, log g= 3.8 dex, [M/H] =-1.0 dex and v sin i= 30 km s-1. This result is in line with other strict observational facts published so far for this object. This is only the third detailed investigation of the ? Bootis-type SB system, but the first one with a known infrared excess.
BYU ScholarsArchive BYU ScholarsArchive A Comparison of Running Shoe Optimal Stiffness and Speed A Comparison of Running Shoe Optimal Stiffness and Speed

Purpose: Increasing the longitudinal bending stiffness of a running shoe decreases metabolic energy cost. Optimal stiffness occurs at the stiffness with the lowest metabolic cost. However, it is still unclear how optimal stiffness varies among individuals. The primary purpose of this study was to understand how optimal shoe stiffness is affected by running speed. A secondary purpose examined the anatomical and biomechanical characteristics associated with optimal stiffness variation. Methods: Six shoe stiffness conditions were manufactured by inserting carbon fiber plates between the midsole and outsole of a standard running shoe (shoe stiffness range: 9.26–23.83 N/mm). Twenty-one experienced male runners (mass = 67.1 ± 5.0 kg, height = 178.9cm ± 4.0 cm, age = 26.4 ± 8.4 years, American shoe size 10–11.5) completed testing at a slow 2.98 m/s and fast 4.47 m/s speed over two testing days, completing 5 min in each shoe condition. Metabolic cost was measured along with several biomechanical and anatomical variables. Data were also separated by foot strike to allow additional analysis. Results: At the fast speed, average optimal stiffness was 19.29 N/mm ( ± 5.62) with a metabolic benefit of 3.02% ( ± 2.62%). Slow speed average optimal stiffness was 17.04 N/mm ( ± 6.09) with a metabolic benefit of 1.93% ( ± 1.82%). Only rearfoot strikers demonstrated a significant increase in optimal stiffness ( p = .020) and the associated metabolic benefit ( p = .024) across speeds. There were no correlations between any of the measured anatomical or biomechanical variables and optimal stiffness. Conclusion: Optimal stiffness varied between subjects but was not correlated to any of our measured characteristics. Rearfoot striking runners may benefit from a high stiffness shoe at faster speeds to enable optimal performance.
Two new accreting, pulsating white dwarfs: SDSS J1457+51 and BW Sculptoris

We report the discovery of rapid periodic signals in the light curves of two cataclysmic variables with prominent white dwarf components in their spectra, SDSS J1457+51 and BW Sculptoris. These stars therefore appear to be new members of the GW Librae class of variable stars, in which the fast periodic (and non-commensurate with the orbital period) signals are believed to arise from non-radial pulsations in the underlying white dwarf. The power spectra of both stars show complex signals with primary periods near 10 and 20 min, respectively. These signals change in frequency by a few per cent on a time-scale of weeks or less, and probably contain an internal fine structure unresolved by our observations. We also detect double-humped waves signifying the underlying orbital periods, near 78 min for both stars. In addition, BW Sculptoris shows a transient but powerful signal with a period near 87 min, a quiescent superhump. The ∼11 per cent excess over the orbital period is difficult to understand, and may arise from an eccentric instability near the 2:1 resonance in the accretion disc.