bluuebunny/crossref_metadata_2025_split huggingface dataset:
Enhanced Recovery After Total Knee Replacement
Authors: Metesky Jamie-Lee , Rosenblatt Meg A. 
Published: April 2023

Abstract
Currently there are more than 700,000 total knee replacements (TKRs) performed annually in the United States, and this number is increasing with an aging population. Total knee replacement is one of the most commonly performed procedures worldwide. Knee replacement is usually the last resort for degenerative arthritis of the knee. Recent efforts have focused on developing enhanced recovery after surgery (ERAS) protocols with hopes of improving patient outcomes while decreasing healthcare costs. The protocol focuses on intensive patient education, multimodal analgesia, including opioid and non-opioid analgesics, both neuraxial and peripheral nerve blocks, and early ambulation are integral components of these fast-track joint pathways. Regional nerve blocks have evolved to more distal and selective blocks to help in early ambulation and rehabilitation.
Regional Anesthesia for Ischemic Pain
Authors: Reddy Shanthi , Sumner Cameron , Kim James 
Published: April 2023

Abstract
Regardless of surgical indication, patients undergoing amputation commonly suffer immediate postoperative pain that is moderate to severe in nature. The goal of this chapter is to review the relevant literature in order to outline a framework for analgesia that optimizes the perioperative pain management of patients undergoing lower extremity amputation. The evidence for various analgesic modalities, including neuraxial, peripheral nerve blocks, and pharmacologic therapies, has been variable. It is well proven that neuraxial analgesia has opioid-sparing and analgesic benefits. Results have been historically mixed regarding perineural catheters in the immediate post-amputation setting. These conflicting results may have been due to suboptimal placement and/or shorter duration of perineural catheter maintenance. Perioperatively, the analgesic approach for management of post-amputation pain should be multidisciplinary and multimodal in nature, utilizing pharmacologic and interventional techniques. Some recent studies are now looking beyond the immediate postoperative period and investigating the impact of perioperative analgesic interventions on the incidence of chronic persistent pain after amputation.
Lower Extremity Weakness in a Patient With Epidural Analgesia
Authors: Helander Erik , Zasimovich Yury 
Published: April 2023

Abstract
Spinal epidural hematomas (SEHs) are rare but potentially devastating injuries and are the most common cause of neuraxial injury leading to litigation. Although the incidence of SEHs is low, it is likely underestimated. An emerging risk factor for SEHs is the use of anticoagulants, and knowledge of guidelines can help limit this risk. Prompt diagnosis is necessary to restrict neurological deterioration and improve chances for recovery, with magnetic resonance imaging (MRI) as the gold standard. Computerized tomography (CT) should be considered if MRI is not immediately available in order to avoid delaying diagnosis. Treatment of clinically significant SEHs typically involves decompressive laminectomy with evacuation of the hematoma. Outcomes are best in patients who undergo surgical decompression within 8 hours of the onset of symptoms, but full recovery is not guaranteed.
Nerve Injury After Plexus and Peripheral Nerve Blocks for Regional Anesthesia and Medicolegal Implications
Authors: Hardman H. David 
Published: April 2023

Abstract
Postoperative neurologic symptoms (PONS) or perioperative nerve injury (PNI) are frequently observed after peripheral nerve and plexus blocks (PNB). Many of these examples of PNI are falsely attributed to PNB, and clinicians fail to consider inherent risks associated with orthopedic surgery and patient-related conditions that predispose to subclinical peripheral neuropathy. Most PNIs spontaneously resolve within several months after surgery, although up to 0.2% may persist beyond 1 year. PNB is not an independent risk factor for developing PONS after surgery. Post-surgical inflammatory neuropathy may be responsible for many cases of PONS that have been incorrectly attributed to PNB. A separate anesthesia consent form, along with a comprehensive block note, can establish standard of care practice for regional anesthesia and PNBs and is encouraged for diagnostic and medicolegal reasons. Any serious motor nerve injury warrants a neurology consultation followed by ultrasound, magnetic resonance imaging, or electrodiagnostic studies. These studies usually localize the site and severity of injury but do not necessarily establish causation. The malpractice risk associated with PNB is low, accounting for 2% of anesthesia-related claims in the American Society of Anesthesiologists Closed Claims Project.
Amphotericin B, itraconazole, posaconazole, and isavuconazole MICs against clinical Mucorales isolates obtained by visual inspection and spectrophotometric reading according to the EUCAST 9.4 procedure
Authors: Escribano Pilar , Mesquida Aina , López-Montesinos Sara , Reigadas Elena , Muñoz Patricia , Guinea Jesús 
Published: April 2023

Abstract
We compared the antifungal susceptibility of 92 Mucorales isolates obtained by visual inspection and spectrophotometric readings following EUCAST (European Committee on Antimicrobial Susceptibility Testing) testing. Amphotericin B minimum inhibitory concentrations (MICs) were up to 1 mg/l against most isolates and variable among species, except for Cunninghamella bertholletiae. Posaconazole MICs against most isolates were up to 1 mg/l and high against Mucor circinelloides, some Rhizopus arrhizus, and Rhizopus microsporus. Isavuconazole MICs ranged between 1 and 8 mg/l but were invariably &gt;8 mg/l against M. circinelloides and C. bertholletiae. The agreement between MICs obtained by visual endpoint or spectrophotometric readings was moderate and higher when using the ≥90% fungal growth inhibition endpoint.
A numerical study of the impact of jet magnetic topology on radio galaxy evolution
Authors: Chen Yi-Hao , Heinz Sebastian , Hooper Eric 
Published: April 2023

ABSTRACT
The propagation of active galactic nucleus jets depends both on the environment into which they propagate and on their internal structure. To test the impact that different magnetic topologies have on the observable properties of radio galaxies on kpc scales, we conducted a series of magnetohydrodynamic simulations of jets injected with different magnetic field configurations propagating into a gaseous atmosphere modelled on the Perseus cluster. The simulations show that the structure of the field affects the collimation and propagation of the jets on cluster scales and thus the morphology of the radio lobes inflated by the jets, due to both magnetic collimation and the development of dynamical instabilities in jets with different magnetic topologies. In all cases, the simulations show a distinct reversal of the synchrotron spectral age gradient in the radio lobes about a dynamical time after the jets turn off due to large-scale circulation inside the radio lobe, driven primarily by buoyancy, which could provide a way to constrain the age of radio sources in cluster environments without the need for detailed spectral modelling and thus constrain the radio-mode feedback efficiency. We suggest a robust diagnostic to search for such age gradients in multifrequency radio data.
Dynamo modelling for cycle variability and occurrence of grand minima in Sun-like stars: rotation rate dependence
Authors: Vashishth Vindya , Karak Bidya Binay , Kitchatinov Leonid 
Published: April 2023

ABSTRACT
Like the solar cycle, stellar activity cycles are also irregular. Observations reveal that rapidly rotating (young) Sun-like stars exhibit a high level of activity with no Maunder-like grand minima and rarely display smooth regular activity cycles. On the other hand, slowly rotating old stars like the Sun have low activity levels and smooth cycles with occasional grand minima. We, for the first time, try to model these observational trends using flux transport dynamo models. Following previous works, we build kinematic dynamo models of one solar mass star with different rotation rates. Differential rotation and meridional circulation are specified with a mean-field hydrodynamic model. We include stochastic fluctuations in the Babcock–Leighton source of the poloidal field to capture the inherent fluctuations in the stellar convection. Based on extensive simulations, we find that rapidly rotating stars produce highly irregular cycles with strong magnetic fields and rarely produce Maunder-like grand minima, whereas the slowly rotating stars (with a rotation period of 10 d and longer) produce smooth cycles of weaker strength, long-term modulation in the amplitude, and occasional extended grand minima. The average duration and the frequency of grand minima increase with decreasing rotation rate. These results can be understood as the tendency of less supercritical dynamo in slower rotating stars to be more prone to produce extended grand minima.
The SZ flux-mass (Y–M) relation at low-halo masses: improvements with symbolic regression and strong constraints on baryonic feedback
Authors: Wadekar Digvijay , Thiele Leander , Hill J Colin , Pandey Shivam , Villaescusa-Navarro Francisco , Spergel David N , Cranmer Miles , Nagai Daisuke , Anglés-Alcázar Daniel , Ho Shirley , Hernquist Lars 
Published: April 2023

ABSTRACT
Feedback from active galactic nuclei (AGNs) and supernovae can affect measurements of integrated Sunyaev–Zeldovich (SZ) flux of haloes (YSZ) from cosmic microwave background (CMB) surveys, and cause its relation with the halo mass (YSZ–M) to deviate from the self-similar power-law prediction of the virial theorem. We perform a comprehensive study of such deviations using CAMELS, a suite of hydrodynamic simulations with extensive variations in feedback prescriptions. We use a combination of two machine learning tools (random forest and symbolic regression) to search for analogues of the Y–M relation which are more robust to feedback processes for low masses ($M\lesssim 10^{14}\, \mathrm{ h}^{-1} \, \mathrm{ M}_\odot$); we find that simply replacing Y → Y(1 + M*/Mgas) in the relation makes it remarkably self-similar. This could serve as a robust multiwavelength mass proxy for low-mass clusters and galaxy groups. Our methodology can also be generally useful to improve the domain of validity of other astrophysical scaling relations. We also forecast that measurements of the Y–M relation could provide per cent level constraints on certain combinations of feedback parameters and/or rule out a major part of the parameter space of supernova and AGN feedback models used in current state-of-the-art hydrodynamic simulations. Our results can be useful for using upcoming SZ surveys (e.g. SO, CMB-S4) and galaxy surveys (e.g. DESI and Rubin) to constrain the nature of baryonic feedback. Finally, we find that the alternative relation, Y–M*, provides complementary information on feedback than Y–M.
The north–south asymmetry of the ALFALFA H i velocity width function
Authors: Brooks Richard A N , Oman Kyle A , Frenk Carlos S 
Published: April 2023

ABSTRACT
The number density of extragalactic 21-cm radio sources as a function of their spectral line widths – the H i width function (H i WF) – is a sensitive tracer of the dark matter halo mass function (HMF). The Lambda cold dark matter model predicts that the HMF should be identical everywhere provided it is sampled in sufficiently large volumes, implying that the same should be true of the H i WF. The Arecibo Legacy Fast ALFA (ALFALFA) 21-cm survey measured the H i WF in northern and southern Galactic fields and found a systematically higher number density in the north. At face value, this is in tension with theoretical predictions. We use the Sibelius-DARK N-body simulation and the semi-analytical galaxy formation model GALFORM to create a mock ALFALFA survey. We find that the offset in number density has two origins: the sensitivity of the survey is different in the two fields, which has not been correctly accounted for in previous measurements; and the 1/Veff algorithm used for completeness corrections does not fully account for biases arising from spatial clustering in the galaxy distribution. The latter is primarily driven by a foreground overdensity in the northern field within $30\, \mathrm{Mpc}$ , but more distant structure also plays a role. We provide updated measurements of the ALFALFA H i WF (and H i mass function) correcting for the variations in survey sensitivity. Only when systematic effects such as these are understood and corrected for can cosmological models be tested against the H i WF.
S-ACF: a selective estimator for the autocorrelation function of irregularly sampled time series
Authors: Kreutzer Lars T , Gillen Edward , Briegal Joshua T , Queloz Didier 
Published: April 2023

ABSTRACT
We present a generalized estimator for the autocorrelation function, S-ACF, which is an extended version of the standard estimator of the autocorrelation function (ACF). S-ACF is a versatile definition that can robustly and efficiently extract periodicity and signal shape information from a time series, independent of the time sampling and with minimal assumptions about the underlying process. Calculating the autocorrelation of irregularly sampled time series becomes possible by generalizing the lag of the standard estimator of the ACF to a real parameter and introducing the notion of selection and weight functions. We show that the S-ACF reduces to the standard ACF estimator for regularly sampled time series. Using a large number of synthetic time series, we demonstrate that the performance of the S-ACF is as good or better than commonly used Gaussian and rectangular kernel estimators, and is comparable to a combination of interpolation and the standard estimator. We apply the S-ACF to astrophysical data by extracting rotation periods for the spotted star KIC 5110407, and compare our results to Gaussian process (GP) regression and Lomb–Scargle (LS) periodograms. We find that the S-ACF periods typically agree better with those from GP regression than from LS periodograms, especially in cases where there is evolution in the signal shape. The S-ACF has a wide range of potential applications and should be useful in quantitative science disciplines where irregularly sampled time series occur. A python implementation of the S-ACF is available under the MIT license.
Statistical investigation of the widths of supra-arcade downflows observed during a solar flare
Authors: Tan Guangyu , Hou Yijun , Tian Hui 
Published: April 2023

ABSTRACT
Supra-arcade downflows (SADs) are dark voids descending towards the post-reconnection flare loops and exhibit obvious variation in properties like width. However, due to the lack of further statistical studies, the mechanism behind such variations hitherto remains elusive. Here, we statistically investigated widths of 81 SADs observed in one flare by the Solar Dynamics Observatory (SDO). For each of SADs, six moments were selected with equal time intervals to measure their widths at different stages of their evolution. It is found that most SADs show a roughly monotonous width decrease during their descents, while some SADs with small initial widths can have complex evolutions. 3D reconstruction results based on SDO and Solar Terrestrial Relations Observatory Ahead (STEREO-A) images and thermal properties analysis reveal that differences in magnetic and plasma environments may result in that SADs in the north are overall wider than those in the south. Additionally, correlation analysis between the width and other parameters of SADs was further conducted and revealed that (1) SADs with different initial widths show no significant differences in their temperature and density evolution characteristics; (2) SADs with small initial widths usually appear in lower heights, where more frequent collisions between SADs could lead to their intermittent acceleration, width increment, and curved trajectories. These results indicate that SADs with different initial widths are produced the same way, while different environments (magnetic field or plasma) could affect their subsequent width evolutions.
Impact of turbulence intensity and fragmentation velocity on dust particle size evolution and non-ideal magnetohydrodynamics effects
Authors: Kawasaki Yoshihiro , Machida Masahiro N 
Published: April 2023

ABSTRACT
We investigate the influence of dust particle size evolution on non-ideal magnetohydrodynamic (MHD) effects during the collapsing phase of star-forming cores, taking both the turbulence intensity in the collapsing cloud core and the fragmentation velocity of dust particles as parameters. When the turbulence intensity is small, the dust particles do not grow significantly, and the non-ideal MHD effects work efficiently in high-density regions. The dust particles rapidly grow in a strongly turbulent environment, while the efficiency of non-ideal MHD effects in such an environment depends on the fragmentation velocity of the dust particles. When the fragmentation velocity is small, turbulence promotes coagulation growth and collisional fragmentation of dust particles, producing small dust particles. In this case, the adsorption of charged particles on the dust particle surfaces becomes efficient and the abundance of charged particles decreases, making non-ideal MHD effects effective at high densities. On the other hand, when the fragmentation velocity is high, dust particles are less likely to fragment, even if the turbulence is strong. In this case, the production of small dust particles becomes inefficient and non-ideal MHD effects become less effective. We also investigate the effect of the dust composition on the star and disc formation processes. We constrain the turbulence intensity of a collapsing core and the fragmentation velocity of dust for circumstellar disc formation due to the dissipation of the magnetic field.
Shock waves in (1 + 1-dimensional) curved space-time
Authors: Verma Anshuman , Mallick Ritam 
Published: April 2023

ABSTRACT
Shock jump conditions are widely used to solve various astrophysical problems. From the hydrodynamic equation, we derive the jump condition and the Taub adiabat equation in curve space-time for both time-like and space-like shocks. We find that the change in entropy for the weak shocks for curved space-time is small, similar to that for flat space-time. We also find that for general relativistic space-like shocks, the Chapman–Jouguet point does not necessarily correspond to the sonic point for downstream matter, unlike the special relativistic case. To analyse the shock wave solution for the curved space-time, one needs the information of metric potentials describing the space-time, which is assumed to be a neutron star for the present work. Assuming a shock wave is generated at the star’s centre, and as it propagates outward, it combusts nuclear matter to quark matter. We find that the general relativistic treatment of shock conditions is necessary to study shocks in neutron stars so that the results are consistent. We also find that with such general relativistic treatment, the combustion process in neutron stars is always a detonation.
The shared evaporation history of three sub-Neptunes spanning the radius–period valley of a hyades star
Authors: Fernández Fernández Jorge , Wheatley Peter J , King George W 
Published: April 2023

ABSTRACT
We model the evaporation histories of the three planets around K2-136, a K-dwarf in the Hyades open cluster with an age of 700 Myr. The star hosts three transiting planets, with radii of 1.0, 3.0, and 1.5 Earth radii, where the middle planet lies above the radius–period valley and the inner and outer planets are below. We use an XMM–Newton observation to measure the XUV radiation environment of the planets, finding that the X-ray activity of K2-136 is lower than predicted by models but typical of similar Hyades members. We estimate the internal structure of each planet, and model their evaporation histories using a range of structure and atmospheric escape formulations. While the precise X-ray irradiation history of the system may be uncertain, we exploit the fact that the three planets must have shared the same history. We find that the Earth-sized K2-136b is most likely rocky, with any primordial gaseous envelope being lost within a few Myr. The sub-Neptune, K2-136c, has an envelope contributing 1–1.7 per cent of its mass that is stable against evaporation thanks to the high mass of its rocky core, whilst the super-Earth, K2-136d, must have a mass at the upper end of the allowed range in order to retain any of its envelope. Our results are consistent with all three planets beginning as sub-Neptunes that have since been sculpted by atmospheric evaporation to their current states, stripping the envelope from planet b and removing most from planet d whilst preserving planet c above the radius-period valley.
AGNs in the CALIFA survey: X-ray detection of nuclear sources
Authors: Osorio-Clavijo N , Gonzalez-Martín O , Sánchez S F , Guainazzi M , Cruz-González I 
Published: April 2023

ABSTRACT
A complete demographic of active galactic nuclei (AGNs) is essential to understand the evolution of the Universe. Optical surveys estimate the population of AGNs in the local Universe to be of ∼ 4 per cent. However, these results could be biased towards bright sources, not affected by the host galaxy attenuation. An alternative method for detecting these objects is through the X-ray emission. In this work, we aim to complement the AGN population of the optical CALIFA survey (941 sources), by using X-ray data from Chandra, which provides the best spatial resolution to date, essential to isolate the nuclear emission from the host galaxy. We study a total of 138 sources with available data. We find 34 new bona fide AGNs and 23 AGN candidates, which could increase the AGN population to 7–10 per cent among the CALIFA survey. X-rays are particularly useful for low-luminosity AGNs since they are excluded by the criterion of large equivalent width of the $\rm {H\alpha }$ emission line when applied to optical selections. Indeed, placing such a restrictive criteria might cause a loss of up to 70 per cent of AGN sources. X-ray detected sources are preferentially located in the right side of the [${\mathrm{O}}\, {\small {\rm III}}$ ]/Hβ versus [${\mathrm{N}}\, {\small {\rm II}}$ ]/Hα diagram, suggesting that this diagram might be the most reliable at classifying AGN sources. Our results support the idea that multiwavelength studies are the best way to obtain a complete AGN population.