bluuebunny/crossref_metadata_2025_split huggingface dataset:
Exploring Possibilities for Transforming Established Subscription-based Scientific Journals into Open Access Journals
Authors: Kuballa Stefanie , Schulze Mareike , Böhm Claudia , Gefeller Olaf , Haaf Jan , Henning Peter , Mielke Corinna , Niggemann Florian , Schürg Andrea , Bergemann Dieter , Haux Reinhold 
Published: November 2016

SummaryBackground: Based on today‘s information and communication technologies the open access paradigm has become an important approach for adequately communicating new scientific knowledge.Objectives: Summarizing the present situa -tion for journal transformation. Presenting criteria for adequate transformation as well as a specific approach for it. Describing our exemplary implementation of such a journal transformation.Methods: Studying the respective literature as well as discussing this topic in various discussion groups and meetings (primarily of editors and publishers, but also of authors and readers), with long term experience as editors and /or publishers of scientific publications as prerequisite.Results: There is a clear will, particularly of political and funding organizations, towards open access publishing. In spite of this, there is still a large amount of scientific knowl edge, being communicated through subscription-based journals. For successfully transforming such journals into open access, sixteen criteria for a goal-oriented, stepwise, sustainable, and fair transformation are suggested. The Tandem Model as transformation approach is introduced. Our exemplary implementation is done in the Trans-O-MIM project. It is exploring strategies, models and evaluation metrics for journal transforma tion. As instance the journal Methods of Information in Medicine will apply the Tandem Model from 2017 onwards.Conclusions: Within Trans-O-MIM we will reach at least nine of the sixteen criteria for adequate transformation. It was positive to implement Trans-O-MIM as international research project. After first steps for transforming Methods have successfully been made, challenges will remain, among others, in identifying appropriate incentives for open access publishing in order to support its transformation.
MATHEMATICAL INVESTIGATION OF CLIMATE ADAPTIVE BUILDING SHELL
Authors: Zamovskis Maris , Vanaga Ruta , Blumberga Andra , Bazienė Kristina 
Published: November 2016

The European Parliament and Council Directive 2010/31/EU states that all member states of EU shall ensure that
all new buildings are nearly zero-energy after December 31 2020. For now, there are no efficient, cost effective and widely
used tools to achieve such performance. To achieve the goal set out in the legislation there is a need for an appropriate solution
in order to minimize energy consumption of a building or obtain energy on site from renewable resources. The first
method to achieve it is to minimize heat losses through the envelope of a building in winter and prevent overheating in summer.
Traditional construction types used in buildings have static thermal properties. There is an energy efficiency potential in
dynamic thermal properties of building constructions. Ideas for such constructions can be found in nature following the biomimicry
methodology that solves human problems inspired by processes in nature.
In this paper a feasibility is studied of one proposed CABS (Climate Adaptive Building Shell) using a numerical analysis.
The proposed CABS is a system where geothermal energy is used for façade heating thus minimizing heat losses through
building envelope and utilizing renewable energy. A geothermal heat from shallow depth of 3.2 m is utilized. The CABS
consists of a piping system built in the façade of a building ensuring a circulation of a heat-transfer medium which is transporting
the heat from the ground where the temperature is constant all year to the façade. Circulation of a fluid is ensured by
buoyancy forces alone. The resulting rise of façade temperature reduces peak primary energy demand thus improving building
performance. The mechanism of this CABS is inspired by the blood vessel system in animals. For the numerical analysis
ANSYS Fluent 16.2 is used.
THE MAGELLAN PFS PLANET SEARCH PROGRAM: RADIAL VELOCITY AND STELLAR ABUNDANCE ANALYSES OF THE 360 au, METAL-POOR BINARY “TWINS” HD 133131A & B*
Authors: Teske Johanna K. , Shectman Stephen A. , Vogt Steve S. , Díaz Matías , Butler R. Paul , Crane Jeffrey D. , Thompson Ian B. , Arriagada Pamela 
Published: November 2016

ABSTRACTWe present a new precision radial velocity (RV) data set that reveals multiple planets orbiting the stars in the ∼360 au, G2+G2 “twin” binary HD 133131AB. Our six years of high-resolution echelle observations from MIKE and five years from the Planet Finder Spectrograph (PFS) on the Magellan telescopes indicate the presence of two eccentric planets around HD 133131A with minimum masses of 1.43 ± 0.03 and 0.63 ± 0.15at 1.44 ± 0.005 and 4.79 ± 0.92 au, respectively. Additional PFS observations of HD 133131B spanning five years indicate the presence of one eccentric planet of minimum mass 2.50 ± 0.05at 6.40 ± 0.59 au, making it one of the longest-period planets detected with RV to date. These planets are the first to be reported primarily based on data taken with the PFS onMagellan, demonstrating the instrument’s precision and the advantage of long-baseline RV observations. We perform a differential analysis between the Sun and each star, and between the stars themselves, to derive stellar parameters and measure a suite of 21 abundances across a wide range of condensation temperatures. The host stars are old (likely ∼9.5 Gyr) and metal-poor ([Fe/H] ∼ −0.30), and we detect a ∼0.03 dex depletion in refractory elements in HD 133131A versus B (with standard errors ∼0.017). This detection and analysis adds to a small but growing sample of binary “twin” exoplanet host stars with precise abundances measured, and represents the most metal-poor and likely oldest in that sample. Overall, the planets around HD 133131A and B fall in an unexpected regime in planet mass–host star metallicity space and will serve as an important benchmark for the study of long-period giant planets.
MHD SIMULATIONS OF CORONAL SUPRA-ARCADE DOWNFLOWS INCLUDING ANISOTROPIC THERMAL CONDUCTION
Authors: Zurbriggen E. , Costa A. , Esquivel A. , Schneiter M. , Cécere M. 
Published: November 2016

ABSTRACT
Coronal supra-arcade downflows (SADs) are observed as dark trails descending toward hot turbulent-fan-shaped regions. Due to the large temperature values and gradients in these fan regions, the thermal conduction (TC) should be very efficient. While several models have been proposed to explain the triggering and the evolution of SADs, none of these scenarios address a systematic consideration of TC. Thus, we accomplish this task numerically simulating the evolution of SADs within this framework. That is, SADs are conceived as voided (subdense) cavities formed by nonlinear waves triggered by downflowing bursty localized reconnection events in a perturbed hot fan. We generate a properly turbulent fan, obtained by a stirring force that permits control of the energy and vorticity input in the medium where SADs develop. We include anisotropic TC and consider plasma properties consistent with observations. Our aim is to study whether it is possible to prevent SADs from vanishing by thermal diffusion. We find that this will be the case, depending on the turbulence parameters, in particular if the magnetic field lines are able to envelope the voided cavities, thermally isolating them from the hot environment. Velocity shear perturbations that are able to generate instabilities of the Kelvin–Helmholtz type help to produce magnetic islands, extending the lifetime of SADs.
PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395
Authors: Balog Zoltan , Siegler Nick , Rieke G. H. , Kiss L. L. , Muzerolle James , Gutermuth R. A. , Bell Cameron P. M. , Vinkó J. , Su K. Y. L. , Young E. T. , Gáspár András 
Published: November 2016

ABSTRACT
We present new deep UBVRI images and high-resolution multi-object optical spectroscopy of the young (∼6–10 Myr old), relatively nearby (800 pc) open cluster IC 2395. We identify nearly 300 cluster members and use the photometry to estimate their spectral types, which extend from early B to middle M. We also present an infrared imaging survey of the central region using the IRAC and MIPS instruments on board the Spitzer Space Telescope, covering the wavelength range from 3.6 to 24 μm. Our infrared observations allow us to detect dust in circumstellar disks originating over a typical range of radii from ∼0.1 to ∼10 au from the central star. We identify 18 Class II, 8 transitional disk, and 23 debris disk candidates, respectively, 6.5%, 2.9%, and 8.3% of the cluster members with appropriate data. We apply the same criteria for transitional disk identification to 19 other stellar clusters and associations spanning ages from ∼1 to ∼18 Myr. We find that the number of disks in the transitional phase as a fraction of the total with strong 24 μm excesses ([8] – [24] ≥ 1.5) increases from (8.4 ± 1.3)% at ∼3 Myr to (46 ± 5)% at ∼10 Myr. Alternative definitions of transitional disks will yield different percentages but should show the same trend.
SHIELD: NEUTRAL GAS KINEMATICS AND DYNAMICS
Authors: McNichols Andrew T. , Teich Yaron G. , Nims Elise , Cannon John M. , Adams Elizabeth A. K. , Bernstein-Cooper Elijah Z. , Giovanelli Riccardo , Haynes Martha P. , Józsa Gyula I. G. , McQuinn Kristen B. W. , Salzer John J. , Skillman Evan D. , Warren Steven R. , Dolphin Andrew , Elson E. C. , Haurberg Nathalie , Ott Jürgen , Saintonge Amelie , Cave Ian , Hagen Cedric , Huang Shan , Janowiecki Steven , Marshall Melissa V. , Thomann Clara M. , Sistine Angela Van 
Published: November 2016

ABSTRACT
We present kinematic analyses of the 12 galaxies in the “Survey of H i in Extremely Low-mass Dwarfs” (SHIELD). We use multi-configuration interferometric observations of the H i 21 cm emission line from the Karl G. Jansky Very Large Array (VLA)22
to produce image cubes at a variety of spatial and spectral resolutions. Both two- and three-dimensional fitting techniques are employed in an attempt to derive inclination-corrected rotation curves for each galaxy. In most cases, the comparable magnitudes of velocity dispersion and projected rotation result in degeneracies that prohibit unambiguous circular velocity solutions. We thus make spatially resolved position–velocity cuts, corrected for inclination using the stellar components, to estimate the circular rotation velocities. We find

30 km s−1 for the entire survey population. Baryonic masses are calculated using single-dish H i fluxes from Arecibo and stellar masses derived from HST and Spitzer imaging. Comparison is made with total dynamical masses estimated from the position–velocity analysis. The SHIELD galaxies are then placed on the baryonic Tully–Fisher relation. There exists an empirical threshold rotational velocity, V

< 15 km s−1, below which current observations cannot differentiate coherent rotation from pressure support. The SHIELD galaxies are representative of an important population of galaxies whose properties cannot be described by current models of rotationally dominated galaxy dynamics.
FORMING CHONDRULES IN IMPACT SPLASHES. II. VOLATILE RETENTION
Authors: Dullemond Cornelis Petrus , Harsono Daniel , Stammler Sebastian Markus , Johansen Anders 
Published: November 2016

ABSTRACT
Solving the mystery of the origin of chondrules is one of the most elusive goals in the field of meteoritics. Recently, the idea of planet(esimal) collisions releasing splashes of lava droplets, long considered out of favor, has been reconsidered as a possible origin of chondrules by several papers. One of the main problems with this idea is the lack of quantitative and simple models that can be used to test this scenario by directly comparing to the many known observables of chondrules. In Paper I of this series, we presented a simple thermal evolution model of a spherically symmetric expanding cloud of molten lava droplets that is assumed to emerge from a collision between two planetesimals. The production of lava could be either because the two planetesimals were already in a largely molten (or almost molten) state due to heating by 26Al, or due to impact jetting at higher impact velocities. In the present paper, number II of this series, we use this model to calculate whether or not volatile elements such as Na and K will remain abundant in these droplets or whether they will get depleted due to evaporation. The high density of the droplet cloud (e.g., small distance between adjacent droplets) causes the vapor to quickly reach saturation pressure and thus shuts down further evaporation. We show to what extent, and under which conditions, this keeps the abundances of these elements high, as is seen in chondrules. We find that for most parameters of our model (cloud mass, expansion velocity, initial temperature) the volatile elements Mg, Si, and Fe remain entirely in the chondrules. The Na and K abundances inside the droplets will initially stay mostly at their initial values due to the saturation of the vapor pressure, but at some point start to drop due to the cloud expansion. However, as soon as the temperature starts to decrease, most or all of the vapor recondenses again. At the end, the Na and K elements retain most of their initial abundances, albeit occasionally somewhat reduced, depending on the parameters of the expanding cloud model. These findings appear to be qualitatively consistent with the analysis of Semarkona Type II chondrules by Hewins et al. who found evidence for sodium evaporation followed by recondensation.
COSMOLOGICAL CONSTRAINTS FROM THE REDSHIFT DEPENDENCE OF THE ALCOCK–PACZYNSKI EFFECT: APPLICATION TO THE SDSS-III BOSS DR12 GALAXIES
Authors: Li Xiao-Dong , Park Changbom , Sabiu Cristiano G. , Park Hyunbae , Weinberg David H. , Schneider Donald P. , Kim Juhan , Hong Sungwook E. 
Published: November 2016

ABSTRACT
We apply the methodology developed in Li et al. to BOSS DR12 galaxies and derive cosmological constraints from the redshift dependence of the Alcock–Paczynski (AP) effect. The apparent anisotropy in the distribution of observed galaxies arise from two main sources, the redshift-space distortion (RSD) effect due to the galaxy peculiar velocities, and the geometric distortion when incorrect cosmological models are assumed for transforming redshift to comoving distance, known as the AP effect. Anisotropies produced by the RSD effect are, although large, maintaining a nearly uniform magnitude over a large range of redshift, while the degree of anisotropies from the AP effect varies with redshift by a much larger magnitude. We split the DR12 galaxies into six redshift bins, measure the two-point correlation function in each bin, and assess the redshift evolution of anisotropies. We obtain constraints of

, which are comparable with the current constraints from other cosmological probes such as SNe Ia, cosmic microwave background, and baryon acoustic oscillation (BAO). Combining these cosmological probes with our method yield tight constraints of

. Our method is complementary to the other large-scale structure (LSS) probes like BAO and topology. We expect this technique will play an important role in deriving cosmological constraints from LSS surveys.
CROSS-CORRELATION BETWEEN X-RAY AND OPTICAL/NEAR-INFRARED BACKGROUND INTENSITY FLUCTUATIONS
Authors: Mitchell-Wynne Ketron , Cooray Asantha , Xue Yongquan , Luo Bin , Brandt William , Koekemoer Anton 
Published: November 2016

ABSTRACT
Angular power spectra of optical and infrared background anisotropies at wavelengths between 0.5 and 5 μm are a useful probe of faint sources present during reionization, in addition to faint galaxies and diffuse signals at low redshift. The cross-correlation of these fluctuations with backgrounds at other wavelengths can be used to separate some of these signals. A previous study on the cross-correlation between X-ray and Spitzer fluctuations at 3.6 μm and 4.5 μm has been interpreted as evidence for direct collapse black holes present at z > 12. Here we return to this cross-correlation and study its wavelength dependence from 0.5 to 4.5 μm using Hubble and Spitzer data in combination with a subset of the 4 Ms Chandra observations in GOODS-S/ECDFS. Our study involves five Hubble bands at 0.6, 0.7, 0.85, 1.25, and 1.6 μm, and two Spitzer-IRAC bands at 3.6 μm and 4.5 μm. We confirm the previously seen cross-correlation between 3.6 μm (4.5 μm) and X-rays with 3.7σ (4.2σ) and 2.7σ (3.7σ) detections in the soft [0.5–2] keV and hard [2–8] keV X-ray bands, respectively, at angular scales above 20 arcsec. The cross-correlation of X-rays with Hubble is largely anticorrelated, ranging between the levels of 1.4σ–3.5σ for all the Hubble and X-ray bands. This lack of correlation in the shorter optical/NIR bands implies the sources responsible for the cosmic infrared background at 3.6 and 4.5 μm are at least partly dissimilar to those at 1.6 μm and shorter.
HELICAL KINK INSTABILITY IN A CONFINED SOLAR ERUPTION
Authors: Hassanin Alshaimaa , Kliem Bernhard 
Published: November 2016

ABSTRACT
A model for strongly writhing confined solar eruptions suggests an origin in the helical kink instability of a coronal flux rope that remains stable against the torus instability. This model is tested against the well observed filament eruption on 2002 May 27 in a parametric MHD simulation study that comprises all phases of the event. Good agreement with the essential observed properties is obtained. These include the confinement, terminal height, writhing, distortion, and dissolution of the filament, and the flare loops. The agreement is robust against variations in a representative range of parameter space. Careful comparisons with the observation data constrain the ratio of the external toroidal and poloidal field components to

and the initial flux rope twist to

. Different from ejective eruptions, two distinct phases of strong magnetic reconnection can occur. First, the erupting flux is cut by reconnection with overlying flux in the helical current sheet formed by the instability. If the resulting flux bundles are linked as a consequence of the erupting rope’s strong writhing, they subsequently reconnect in the vertical current sheet between them. This reforms the overlying flux and a far less twisted flux rope, offering a pathway to homologous eruptions.
THE EFFECT OF AN OFFSET POLAR CAP DIPOLAR MAGNETIC FIELD ON THE MODELING OF THE VELA PULSAR’S γ-RAY LIGHT CURVES
Authors: Barnard M. , Venter C. , Harding A. K. 
Published: November 2016

ABSTRACT
We performed geometric pulsar light curve modeling using static, retarded vacuum, and offset polar cap (PC) dipole B-fields (the latter is characterized by a parameter ϵ), in conjunction with standard two-pole caustic (TPC) and outer gap (OG) emission geometries. The offset-PC dipole B-field mimics deviations from the static dipole (which corresponds to

). In addition to constant-emissivity geometric models, we also considered a slot gap (SG) E-field associated with the offset-PC dipole B-field and found that its inclusion leads to qualitatively different light curves. Solving the particle transport equation shows that the particle energy only becomes large enough to yield significant curvature radiation at large altitudes above the stellar surface, given this relatively low E-field. Therefore, particles do not always attain the radiation-reaction limit. Our overall optimal light curve fit is for the retarded vacuum dipole field and OG model, at an inclination angle

and observer angle

. For this B-field, the TPC model is statistically disfavored compared to the OG model. For the static dipole field, neither model is significantly preferred. We found that smaller values of ϵ are favored for the offset-PC dipole field when assuming constant emissivity, and larger ϵ values favored for variable emissivity, but not significantly so. When multiplying the SG E-field by a factor of 100, we found improved light curve fits, with α and ζ being closer to best fits from independent studies, as well as curvature radiation reaction at lower altitudes.
DYNAMICAL MODEL FOR SPINDOWN OF SOLAR-TYPE STARS
Authors: Sood Aditi , Kim Eun-jin , Hollerbach Rainer 
Published: November 2016

ABSTRACT
After their formation, stars slow down their rotation rates by the removal of angular momentum from their surfaces, e.g., via stellar winds. Explaining how this rotation of solar-type stars evolves in time is currently an interesting but difficult problem in astrophysics. Despite the complexity of the processes involved, a traditional model, where the removal of angular momentum by magnetic fields is prescribed, has provided a useful framework to understand observational relations between stellar rotation, age, and magnetic field strength. Here, for the first time, a spindown model is proposed where loss of angular momentum by magnetic fields evolves dynamically, instead of being prescibed kinematically. To this end, we evolve the stellar rotation and magnetic field simultaneously over stellar evolution time by extending our previous work on a dynamo model which incorporates nonlinear feedback mechanisms on rotation and magnetic fields. We show that our extended model reproduces key observations and is capable of explaining the presence of the two branches of (fast and slow rotating) stars which have different relations between rotation rate Ω versus time (age), magnetic field strength

versus rotation rate, and frequency of magnetic field

versus rotation rate. For fast rotating stars we find that: (i) there is an exponential spindown

, with t measured in Gyr; (ii) magnetic activity saturates for higher rotation rate; (iii)

. For slow rotating stars we find: (i) a power-law spindown

; (ii) that magnetic activity scales roughly linearly with rotation rate; (iii)

. The results obtained from our investigations are in good agreement with observations. The Vaughan–Preston gap is consistently explained in our model by the shortest spindown timescale in this transition from fast to slow rotators. Our results highlight the importance of self-regulation of magnetic fields and rotation by direct and indirect interactions involving nonlinear feedback in stellar evolution.
ON THE NATURE OF THE SMALL-SCALE STRUCTURE IN THE COSMIC MICROWAVE BACKGROUND OBSERVED BY PLANCK AND WMAP
Authors: Verschuur G. L. , Schmelz J. T. 
Published: November 2016

ABSTRACT
Small-scale features observed by Wilkinson Microwave Anisotropy Probe (WMAP) and PLANCK in the frequency range of 22–90 GHz show a nearly flat spectrum, which meets with expectations that they originate in the early universe. However, free–free emission from electrons in small angular scale galactic sources that suffer beam dilution very closely mimic the observed spectrum in this frequency range. Fitting such a model to the PLANCK and WMAP data shows that the angular size required to fit the data is comparable to the angular width of associated H i filaments found in the Galactic Arecibo L-Band Feed Array-H isurvey data. Also, the temperature of the electrons is found to be in the range of 100–300 K. The phenomenon revealed by these data may contribute to a more precise characterization of the foreground masks required to interpret the cosmological aspect of PLANCK and WMAP data.