bluuebunny/crossref_metadata_2025_split huggingface dataset:
Application of N-of-1 Experiments to Test the Efficacy of Inactivity Alert Features in Fitness Trackers to Increase Breaks from Sitting in Older Adults
Authors: Rosenberg Dori , Kadokura Elyse , Morris Margaret , Renz Anne , Vilardaga Roger 
Published: August 2017

SummaryBackground: Frequent breaks from sitting could improve health. Many commercially available fitness trackers deliver vibration alerts that could be used to cue sitting breaks. As a potentially pragmatic approach to promote frequent breaks from sitting, we tested the efficacy of inactivity alerts among obese older adults, a highly sedentary population.Methods: We conducted 10 sequential N-of-1 (single-case) experimental ABA trials. Participants (mean age = 68, mean BMI = 35) were monitored for a baseline phase (“A1”) followed by an intervention phase (“B”). The intervention was then removed and participants were monitored to test an experimental effect (reversal “A2” phase). Total time in the study was limited to 25 days. During the intervention phase (“B”), participants used fitness trackers to stand up or move every time they received an alert (every 15 or 20 minutes of inactivity). Participants wore activPAL devices to measure breaks from sitting each day. Randomization tests were used to determine whether the number of breaks was significantly higher during the “B” phase than the two “A” phases.Results: Breaks were higher by 7.2 breaks per day during the “B” phase compared to the mean of the “A” phases. Seven out of 10 participants had more sitting breaks during the intervention phase which subsequently decreased during the reversal “A2” phase (combined p-value < .05).Conclusion: Inactivity alert features within commercially available devices are efficacious for promoting modest improvements in breaks from sitting among older adults with obesity and could be a simple health-promoting strategy in this population.
IN-SYNC. V. Stellar Kinematics and Dynamics in the Orion A Molecular Cloud
Authors: Da Rio Nicola , Tan Jonathan C. , Covey Kevin R. , Cottaar Michiel , Foster Jonathan B. , Cullen Nicholas C. , Tobin John , Kim Jinyoung S. , Meyer Michael R. , Nidever David L. , Stassun Keivan G. , Chojnowski S. Drew , Flaherty Kevin M. , Majewski Steven R. , Skrutskie Michael F. , Zasowski Gail , Pan Kaike 
Published: August 2017

Abstract
The kinematics and dynamics of young stellar populations enable us to test theories of star formation. With this aim, we continue our analysis of the SDSS-III/APOGEE IN-SYNC survey, a high-resolution near-infrared spectroscopic survey of young clusters. We focus on the Orion A star-forming region, for which IN-SYNC obtained spectra of ∼2700 stars. In Paper IV we used these data to study the young stellar population. Here we study the kinematic properties through radial velocities (v

r
). The young stellar population remains kinematically associated with the molecular gas, following a

gradient along the filament. However, near the center of the region, the v

r
distribution is slightly blueshifted and asymmetric; we suggest that this population, which is older, is slightly in the foreground. We find evidence for kinematic subclustering, detecting statistically significant groupings of colocated stars with coherent motions. These are mostly in the lower-density regions of the cloud, while the ONC radial velocities are smoothly distributed, consistent with it being an older, more dynamically evolved cluster. The velocity dispersion

varies along the filament. The ONC appears virialized, or just slightly supervirial, consistent with an old dynamical age. Here there is also some evidence for ongoing expansion, from a v

r
-extinction correlation. In the southern filament,

is ∼2–3 times larger than virial in the L1641N region, where we infer a superposition along the line of sight of stellar subpopulations, detached from the gas. In contrast,

decreases toward L1641S, where the population is again in agreement with a virial state.
Formal Solutions for Polarized Radiative Transfer. II. High-order Methods
Authors: Janett Gioele , Steiner Oskar , Belluzzi Luca 
Published: August 2017

Abstract
When integrating the radiative transfer equation for polarized light, the necessity of high-order numerical methods is well known. In fact, well-performing high-order formal solvers enable higher accuracy and the use of coarser spatial grids. Aiming to provide a clear comparison between formal solvers, this work presents different high-order numerical schemes and applies the systematic analysis proposed by Janett et al., emphasizing their advantages and drawbacks in terms of order of accuracy, stability, and computational cost.
Very Low-energy Supernovae: Light Curves and Spectra of Shock Breakout
Authors: Lovegrove Elizabeth , Woosley S. E. , Zhang Weiqun 
Published: August 2017

Abstract
The brief transient emitted as a shock wave erupts through the surface of a pre-supernova star carrying information about the stellar radius and explosion energy. Here, the CASTRO code, which treats radiation transport using multigroup flux-limited diffusion, is used to simulate the light curves and spectra of shock breakout in very low-energy supernovae (VLE SNe), explosions in giant stars with final kinetic energy much less than 1051 erg. VLE SN light curves, computed here with the KEPLER code, are distinctively faint, red, and long-lived, making them challenging to find with transient surveys. The accompanying shock breakouts are brighter, though briefer, and potentially easier to detect. Previous analytic work provides general guidance, but numerical simulations are challenging, due to the range of conditions and lack of equilibration between color and effective temperatures. We consider previous analytic work and extend discussions of color temperature and opacity to the lower energy range explored by these events. Since this is the first application of the CASTRO code to shock breakout, test simulations of normal energy shock breakout of SN 1987A are carried out and compared with the literature. A set of breakout light curves and spectra are then calculated for VLE SNe with final kinetic energies in the range

erg for red supergiants with main-sequence masses of 15 and 25

. The importance of uncertainties in stellar atmosphere model, opacity, and ambient medium is discussed, as are observational prospects with current and forthcoming missions.
Gaia Reveals a Metal-rich, in situ Component of the Local Stellar Halo
Authors: Bonaca Ana , Conroy Charlie , Wetzel Andrew , Hopkins Philip F. , Kereš Dušan 
Published: August 2017

Abstract
We use the first Gaia data release, combined with the RAVE and APOGEE spectroscopic surveys, to investigate the origin of halo stars within

kpc from the Sun. We identify halo stars kinematically as moving at a relative speed of at least 220 km s−1 with respect to the local standard of rest. These stars are generally less metal-rich than the disk, but surprisingly, half of our halo sample is comprised of stars with

. The orbital directions of these metal-rich halo stars are preferentially aligned with the disk rotation, in sharp contrast with the intrinsically isotropic orbital distribution of the metal-poor halo stars. We find similar properties in the Latte cosmological zoom-in simulation of a Milky Way-like galaxy from the FIRE project. In Latte, metal-rich halo stars formed primarily inside of the solar circle, whereas lower-metallicity halo stars preferentially formed at larger distances (extending beyond the virial radius). This suggests that metal-rich halo stars in the solar neighborhood actually formed in situ within the Galactic disk, rather than having been accreted from satellite systems. These stars, currently on halo-like orbits, therefore have likely undergone substantial radial migration/heating.
Chromospheric Inversions of a Micro-flaring Region
Authors: Reid A. , Henriques V. , Mathioudakis M. , Doyle J. G. , Ray T. 
Published: August 2017

Abstract
We use spectropolarimetric observations of the Ca ii 8542 Å line, taken from the Swedish 1 m Solar Telescope, in an attempt to recover dynamic activity in a micro-flaring region near a sunspot via inversions. These inversions show localized mean temperature enhancements of ∼1000 K in the chromosphere and upper photosphere, along with co-spatial bi-directional Doppler shifting of 5–10 km s−1. This heating also extends along a nearby chromospheric fibril, which is co-spatial to 10–15 km s−1 downflows. Strong magnetic flux cancellation is also apparent in one of the footpoints, and is concentrated in the chromosphere. This event more closely resembles that of an Ellerman Bomb, though placed slightly higher in the atmosphere than what is typically observed.
High-resolution Near-infrared Observations of a Small Cluster Associated with a Bright-rimmed Cloud in W5
Authors: Imai Rieko , Sugitani Koji , Miao Jingqi , Fukuda Naoya , Watanabe Makoto , Kusune Takayoshi , Pickles Andrew J. 
Published: August 2017

Abstract
We carried out near-infrared (IR) observations to examine star formation toward the bright-rimmed cloud SFO 12, of which the main exciting star is O7V star in W5-W. We found a small young stellar object (YSO) cluster of six members embedded in the head of SFO 12 facing its exciting star, aligned along the UV radiation incident direction from the exciting star. We carried out high-resolution near-IR observations with the Subaru adaptive optics (AO) system and revealed that three of the cluster members appear to have circumstellar envelopes, one of which shows an arm-like structure in its envelope. Our near-IR and

-band photometry and Spitzer IRAC data suggest that formation of two members at the tip side occurred in advance of other members toward the central part, under our adopted assumptions. Our near-IR data and previous studies imply that more YSOs are distributed in the region just outside the cloud head on the side of the main exciting star, but there is little sign of star formation toward the opposite side. We infer that star formation has been sequentially occurring from the exciting star side to the central part. We examined archival data of far-infrared and CO (

) which reveals that, unlike in the optical image, SFO 12 has a head–tail structure that is along the UV incident direction. This suggests that SFO 12 is affected by strong UV from the main exciting star. We discuss the formation of this head–tail structure and star formation there by comparing with a radiation-driven implosion (RDI) model.
Electron Captures on
as a Trigger for Helium Shell Detonations
Authors: Bauer Evan B. , Schwab Josiah , Bildsten Lars 
Published: August 2017

Abstract
White dwarfs (WDs) that accrete helium at rates

, such as those in close binaries with sdB stars, can accumulate large (

) helium envelopes, which are likely to detonate. We perform binary stellar evolution calculations of sdB+WD binary systems with MESA, incorporating the important reaction chain

(NCO), including a recent measurement for the

rate. In large accreted helium shells, the NCO reaction chain leads to ignitions at the dense base of the freshly accreted envelope, in contrast to

ignitions, which occur away from the base of the shell. In addition, at these accretion rates, the shells accumulate on a timescale comparable to their thermal time, leading to an enhanced sensitivity of the outcome on the accretion rate history. Hence, time dependent accretion rates from binary stellar evolution are necessary to determine the helium layer mass at ignition. We model the observed sdB+WD system CD

and find that the inclusion of these effects predicts ignition of a

helium shell, nearly a factor of two larger than previous predictions. A shell with this mass will ignite dynamically, a necessary condition for a helium shell detonation.
On the Origin of the Bi-drifting Subpulse Phenomenon in Pulsars
Authors: Szary Andrzej , van Leeuwen Joeri 
Published: August 2017

Abstract
The unique and highly unusual drift feature reported for PSR J0815+0939, wherein one component’s subpulses drift in the direction opposite of the general trend, is a veritable challenge to pulsar theory. In this paper, we observationally quantify the drift direction throughout its profile, and find that the second component is the only one that exhibits “bi-drifting,” meaning that only the second component moves in the direction opposite of the others. We present a model that shows that the observed bi-drifting phenomenon follows from the insight that the discharging regions, i.e., sparks, do not rotate around the magnetic axis per se, but rather around the point of maximum potential at the polar cap. We show that a purely dipolar surface magnetic field cannot exhibit bi-drifting behavior. though certain non-dipolar configurations can. We can distinguish two types of solutions, with relatively low (

) and high (

) surface magnetic fields. Depending on the strength of the surface magnetic field, the radius of the curvature of magnetic field lines ranges from

to

. Pulsar J0815+0939 allows us to gain an understanding of the polar-cap conditions essential for plasma generation processes in the inner acceleration region, by linking the observed subpulse shift to the underlying spark motion.
Successive Two-sided Loop Jets Caused by Magnetic Reconnection between Two Adjacent Filamentary Threads
Authors: Tian Zhanjun , Liu Yu , Shen Yuandeng , Elmhamdi Abouazza , Su Jiangtao , Liu Ying D. , Kordi Ayman. S. 
Published: August 2017

Abstract
We present observational analysis of two successive two-sided loop jets observed by the ground-based New Vacuum Solar Telescope and the space-borne Solar Dynamics Observatory. The two successive two-sided loop jets manifested similar evolution processes and both were associated with the interaction of two small-scale adjacent filamentary threads, magnetic emerging, and cancellation processes at the jet’s source region. High temporal and high spatial resolution observations reveal that the two adjacent ends of the two filamentary threads are rooted in opposite magnetic polarities within the source region. The two threads approached each other, and then an obvious brightening patch is observed at the interaction position. Subsequently, a pair of hot plasma ejections are observed heading in opposite directions along the paths of the two filamentary threads at a typical speed for two-sided loop jets of the order 150 km s−1. Close to the end of the second jet, we report the formation of a bright hot loop structure at the source region, which suggests the formation of new loops during the interaction. Based on the observational results, we propose that the observed two-sided loop jets are caused by magnetic reconnection between the two adjacent filamentary threads, largely different from the previous scenario that a two-sided loop jet is generated by magnetic reconnection between an emerging bipole and the overlying horizontal magnetic fields.
Star Formation Activity of Barred Spiral Galaxies
Authors: Kim Eunbin , Hwang Ho Seong , Chung Haeun , Lee Gwang-Ho , Park Changbom , Sodi Bernardo Cervantes , Kim Sungsoo S. 
Published: August 2017

Abstract
We study the star formation activity of nearby galaxies with bars using a sample of late-type galaxies at

and

from the Sloan Digital Sky Survey. We compare the physical properties of strongly and weakly barred galaxies with those of non-barred galaxies that have stellar mass and redshift distributions similar to barred galaxies. We find that the star formation activity of strongly barred galaxies probed by starburstiness,

,

, and mid-infrared [3.4]–[12] colors is, on average, lower than that of non-barred galaxies. However, weakly barred galaxies do not show such a difference between barred and non-barred galaxies. The amounts of atomic and molecular gas in strongly barred galaxies are smaller than those in non-barred galaxies, and the gas metallicity is higher in strongly barred galaxies than in non-barred galaxies. The gas properties of weakly barred galaxies again show no difference from those of non-barred galaxies. We stack the optical spectra of barred and non-barred galaxies in several mass bins and fit to the stacked spectra with a spectral fitting code, STARLIGHT. We find no significant difference in stellar populations between barred and non-barred galaxies for both strongly and weakly barred galaxies. Our results are consistent with the idea that the star formation activity of barred galaxies was enhanced in the past along with significant gas consumption, and is currently lower than or similar to that of non-barred galaxies. The past star formation enhancement depends on the strength of bars.
Pebble Accretion at the Origin of Water in Europa
Authors: Ronnet Thomas , Mousis Olivier , Vernazza Pierre 
Published: August 2017

Abstract
Despite the fact that the observed gradient in water content among the Galilean satellites is globally consistent with a formation in a circum-Jovian disk on both sides of the snowline, the mechanisms that led to a low water mass fraction in Europa (∼8%) are not yet understood. Here, we present new modeling results of solids transport in the circum-Jovian disk accounting for aerodynamic drag, turbulent diffusion, surface temperature evolution, and sublimation of water ice. We find that the water mass fraction of pebbles (e.g., solids with sizes of 10−2–1 m) as they drift inward is globally consistent with the current water content of the Galilean system. This opens the possibility that each satellite could have formed through pebble accretion within a delimited region whose boundaries were defined by the position of the snowline. This further implies that the migration of the forming satellites was tied to the evolution of the snowline so that Europa fully accreted from partially dehydrated material in the region just inside of the snowline.
Gentle Heating by Mixing in Cooling Flow Clusters
Authors: Hillel Shlomi , Soker Noam 
Published: August 2017

Abstract
We analyze 3D hydrodynamical simulations of the interaction of jets and the bubbles they inflate with the intracluster medium (ICM) and show that the heating of the ICM by mixing hot bubble gas with the ICM operates over tens of millions of years and hence can smooth the sporadic activity of the jets. The inflation process of hot bubbles by propagating jets forms many vortices, and these vortices mix the hot bubble gas with the ICM. The mixing, and hence the heating of the ICM, starts immediately after the jets are launched, but continues for tens of millions of years. We suggest that the smoothing of the active galactic nucleus (AGN) sporadic activity by the long-lived vortices accounts for the recent finding of a gentle energy coupling between AGN heating and the ICM.
Estimating the Body Weight of Florida Panthers From Standard Morphometric Measurements
Authors: Bartareau Tad M. 
Published: August 2017

Abstract
Measuring a mammal's body weight has importance in understanding reproductive biology, ecology, and population health. It can be impractical for a researcher to measure the body weight of mammals when equipment needed to weigh individuals is inadequate or unavailable. My objective here was to develop a model to accurately estimate the body weight of Florida panthers Puma concolor coryi Bang based on the relationship between scale weight, sex, and standard morphometric measurement predictor variables obtainable in the field. I used an information-theoretic approach to evaluate simple and multiple linear regression models with 70% of the data, and validated the best model in the set using the remaining 30%. Individuals maintained a similar proportion of body weight to body length, chest girth2, and neck girth measurements, and the relationship was consistent between sexes. My best model explained 94% of the variation in body weight of Florida panthers, and the observed and estimated body weights in the validation data set were not different. The 95% confidence interval on the bias of the estimated body weight ranged from −1.1 to 0.9 kg in the validation data set. This body-weight estimation model will enable retrospective estimates of the body weight of Florida panthers in cases where standard morphometric measurements are available but the individuals were not weighed.
“Is There An App For That?” Orthopaedic Patient Preferences For A Smartphone Application
Authors: Dattilo Jonathan R. , Gittings Daniel J. , Sloan Matthew , Hardaker William M. , Deasey Matthew J. , Sheth Neil P. 
Published: August 2017

Summary
Background: Patients are seeking out medical information on the Internet and utilizing smartphone health applications (“apps”). Smartphone use has exponentially increased among orthopaedic surgeons and patients. Despite this increase, patients are rarely directed to specific apps by physicians. No study exists querying patient preferences for a patient-centered, orthopaedic smartphone application.
Objectives: The purpose of this study is to 1) determine Internet use patterns amongst orthopaedic patients; 2) ascertain access to and use of smartphones; and 3) elucidate what features orthopaedic patients find most important in a smartphone application.
Methods: We surveyed patients in an orthopaedic practice in an urban academic center to assess demographics, access to and patterns of Internet and Smartphone use, and preferences for features in a smartphone app.
Results: A total of 310 surveys were completed. Eighty percent of patients reported Internet access, and 62% used the Internet for health information. Seventy-seven percent owned smartphones, 45% used them for health information, and 28% owned health apps. Only 11% were referred to an app by a physician. The highest ranked features were appointment reminders, ability to view test results, communication with physicians, and discharge instructions. General orthopaedic information and pictures or videos explaining surgery were the 2 lowest ranked features. Seventy-one percent of patients felt an app with some of the described features would improve their healthcare experiences, and 40% would pay for the app.
Conclusions: The smartphone is an under-utilized tool to enhance patient-physician communication, increase satisfaction, and improve quality of care. Patients were enthusiastic about app features that are often included in patient health portals, but ranked orthopaedic educational features lowest. Further study is required to elucidate how best to use orthopaedic apps as physician-directed educational opportunities to promote patient satisfaction and quality of care.
Citation: Dattilo JR, Gittings DJ, Sloan M, Hardaker WM, Deasey MJ, Sheth NP. “Is There An App For That?“ Orthopaedic Patient Preferences For A Smartphone Application. Appl Clin Inform 2017; 8: 832–844 https://doi.org/10.4338/ACI-2017-04-RA-0058