bluuebunny/crossref_metadata_2025_split huggingface dataset:
VUCA-MEASURING CONCEPTUAL FOUNDATIONS IN THE CONTEXT OF PROFESSIONAL SELF-DEVELOPMENT
Authors: NIKONENKO I. O. 
Published: January 2020

Now, so important to consider the business as a financial and profitability structure, that is interested in competitiveness, efficient activity and economic development. The achievement of the defined indicators of successful business is possible of the presence of professional, experienced and conscientious employees, so is the important to form such a system of personnel management, which is in order to promote the competence of the employees. In addition to making business investments in training and developing competencies of the employees, an important prerequisite is the meaningful and purposeful willingness of the personality to foster the development of herself professional competence in the context of the actual volatile and unpredictable VUCA-world. To that, in the article describe the conceptual foundations of professional personal self-development in the context of the VUCA-world and presented of the basic VUCA-competencies as the competitive advantages of the modern business environment. According to the provisions of the VUCA-world, important competencies of the employees there are: prognostic vision in the context of prospect of business development; understanding of the actual needs and purpose of the business activity; creativity, as the ability to the put forward alternative solutions of the business problems, and agility, as the ability and the internally determined conviction to act in the interests of the business. The explained of importance of social and area organization as main conditions for the professional self-development, personal awareness and competitiveness of the employees. In the context of the activity approach, the revealed of the importance of the professional environment for the development of the leading competencies of the employe. So, in the article is express of the priority of the psycho-sociology need for the formation of such the model of the development of the competencies of the employee, that would be answer of the needs of actual unpredictable VUCA-world.
Pengaruh Aktivasi Regulasi Emosi Terhadap Prestasi Olahraga Atlet Disabilitas NPC Kota Surakarta
Authors: Kliwon Kliwon , Sarwanto Ari 
Published: January 2020

Background: Many studies have shown how important psychological roles are when enhancing an athlete's ability to deal with match situations. Psychological changes when comparing namely the increase in the ability of athletes to accept stress (pressure), keep concentrating, have a mental toughness (mental toughness) so as to overcome heavier opposition (Hastria Effendi, 2016: 23). Disability sports problems are closely related to psychological problems and symptoms of their athletes. Maximum achievement can be achieved by an athlete who is truly ready to compete with all his abilities. The readiness in question is the physical and psychological aspects of the athlete concerned.The research purpose was determined the effect of emotional regulation activation on the disability athletes’ performance in NPC of Surakarta City. Methods: The research type is quantitative research with analytic observational design through a cross-sectional approach. This research was conducted at NPC of Surakarta City. The research population was the Athletes of NPC of Surakarta City. The number of NPC athletes in the Surakarta city which became the researech population amounted to 160 athletes. The sampling technique was used random sampling. Collecting data techniques were used questionnaire, observation, and documentation. Result: The hypothesis testing was used Product Moment Correlation techniques. Conclusion: The research result was showed that there was a close influence between the emotions regulation on the performance of the NPC Surakarta athletes ( tcount > ttable ( (8.685> 1.571 ) )
Gangguan Pola Nafas Tidak Efektif Pada Pasien Congestive Heart Failure (CHF)
Authors: Wardani Wilantika Ida , Setyorini Yuyun , Rifai Akhmad 
Published: January 2020

Abstract Background: Congestive Heart Failure (CHF) is the heart failure in pumping blood so that the blood supply containing oxygen and nutrients to the entire body tissues is inhibited and causes shortness of breath. Problems that arise that the breath pattern is not effective and can be arranged intervention one of them assess the frequency of breath depth. Acquire a real picture and experience in patients with Congestive Heart Failure (CHF). Methods: The type of research used in the preparation of scientific papers is the type of descriptive research and case study design with the approach of nursing care. The number of patients who became the study respondents amounted to two people. Result: Based on observation result, it is concluded that with the same nursing diagnosis and done the same implementation there is difference of result and response between group of intervention with control group. Suggestion. Suggestions put forward in this study is the need to pay attention to the accuracy of the assessment to determine the priority problems that occur in patients and the principle of ONEC (Observation, Nursing Treatment, Education, Collaboration) on the intervention.
Parenting Psikoedukasi Dalam Mendukung Perkembangan Sosial Dan Emosional Anak Usia Pra Sekolah Di Kota Surakarta
Authors: Insiyah Insiyah , Sulistyowati Endang Caturini 
Published: January 2020

Background: Children in kindergarten are experiencing rapid growth and development. Supporting child development is not only the responsibility of the government but also the responsibility of parents, teachers and the surrounding community. Parents are expected to have a good understanding of the psychological child so that they can provide care and education that allows children to grow and develop according to their age. This study aims to determine the effect of parenting psychoeducation on the social and emotional development of pre-school children. Methods: This research used the method of "quasi experiment pre-post test with one group" with a total sample of 63 pre-school age children. Sampling was done using Non Randomized One Group Pretest Postest Design. Research data analysis was performed using SPSS version 23. Results: The results showed that preschool age children numbered 63 people consisting of 60.3% (38) people were male and the rest were female 39.7% (25). There was an increase in social development in preschool children whose parents received significantly higher parenting psychoeducation (p value 0,000) There was an increase in emotional development in pre-school children whose parents received significantly higher parenting psychoeducation (p value 0,000). Conclusion: The conclusion showed that there was a parenting psychoeducation effect on parents on social and emotional development of pre-school age children.
Keywords: Psychoeducation, Social and Emotional Development, Pre School Children
Hubungan Gangguan Tidur Ibu Nifas Dengan Kejadian Postpartum Blues Di Wilayah Kerja Puskesmas Karangmalang Sragen
Authors: Hasna Amalia Nabillah , Murwati Murwati , Susilowati Dewi 
Published: January 2020

Abstract Background : Postpartum mothers who fail to adjust to their new role can experience postpartum blues. Physical fatigue due to the activity of babysitting, breastfeeding, bathing the baby, cradling the baby at any time can cause maternal rest so that the mother's sleep/ rest can be disrupted. Rest/ sleep that is sufficient can reduce the occurrence of postpartum blues in postpartum mothers. Method: This study is an analytical study with a cross sectional approach. The population in this study were all postpartum mothers in the working area of Karangmalang Sragen health center. The sampling technique was purposive sampling and a sample of 31 postpartum mothers from day 3 to day 10 was obtained which had a history of spontaneous normal labor. Univariate analysis with frequency distribution and bivariate analysis with Rankspearman statistical test. The results of this study were the age of respondents at most,namely age 20-35 years 90.3%, multipara mothers 54.8%, respondents with secondary education 61.3%, mothers working at home 77.4%, severe sleep disorders 25.8%, experienced postpartum blues 32.3%. Result: The results of Rank-spearman statistical test can be concluded p value = 0,000 and r value of 0.812. onclusion: The conclusion is that there is a relationship between postpartum blues sleep disturbance in the working area of Karangmalang Sragen Health Center.
The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry
Authors: Nielsen Eric L. , De Rosa Robert J. , Wang Jason J. , Sahlmann Johannes , Kalas Paul , Duchêne Gaspard , Rameau Julien , Marley Mark S. , Saumon Didier , Macintosh Bruce , Millar-Blanchaer Maxwell A. , Nguyen Meiji M. , Ammons S. Mark , Bailey Vanessa P. , Barman Travis , Bulger Joanna , Chilcote Jeffrey , Cotten Tara , Doyon Rene , Esposito Thomas M. , Fitzgerald Michael P. , Follette Katherine B. , Gerard Benjamin L. , Goodsell Stephen J. , Graham James R. , Greenbaum Alexandra Z. , Hibon Pascale , Hung Li-Wei , Ingraham Patrick , Konopacky Quinn , Larkin James E. , Maire Jérôme , Marchis Franck , Marois Christian , Metchev Stanimir , Oppenheimer Rebecca , Palmer David , Patience Jennifer , Perrin Marshall , Poyneer Lisa , Pueyo Laurent , Rajan Abhijith , Rantakyrö Fredrik T. , Ruffio Jean-Baptiste , Savransky Dmitry , Schneider Adam C. , Sivaramakrishnan Anand , Song Inseok , Soummer Remi , Thomas Sandrine , Wallace J. Kent , Ward-Duong Kimberly , Wiktorowicz Sloane , Wolff Schuyler 
Published: January 2020

Abstract
We present new observations of the planet β Pictoris b from 2018 with the Gemini Planet Imager (GPI), the first GPI observations following conjunction. Based on these new measurements, we perform a joint orbit fit to the available relative astrometry from ground-based imaging, the Hipparcos Intermediate Astrometric Data (IAD), and the Gaia DR2 position, and demonstrate how to incorporate the IAD into direct imaging orbit fits. We find a mass consistent with predictions of hot-start evolutionary models and previous works following similar methods, though with larger uncertainties: 12.8+5.3
−3.2
M
Jup. Our eccentricity determination of

disfavors circular orbits. We consider orbit fits to several different imaging data sets, and find generally similar posteriors on the mass for each combination of imaging data. Our analysis underscores the importance of performing joint fits to the absolute and relative astrometry simultaneously, given the strong covariance between orbital elements. Time of conjunction is well-constrained within 2.8 days of 2017 September 13, with the star behind the planet’s Hill sphere between 2017 April 11 and 2018 February 16 (±18 days). Following the recent radial velocity detection of a second planet in the system, β Pic c, we perform additional two-planet fits combining relative astrometry, absolute astrometry, and stellar radial velocities. These joint fits find a significantly smaller mass (8.0 ± 2.6 M
Jup) for the imaged planet β Pic b, in a somewhat more circular orbit. We expect future ground-based observations to further constrain the visual orbit and mass of the planet in advance of the release of Gaia DR4.
Very Long Baseline Array Astrometry of Cassini: The Final Epochs and an Improved Orbit of Saturn
Authors: Jones Dayton L. , Folkner William M. , Jacobson Robert A. , Jacobs Christopher S. , Romney Jonathan , Dhawan Vivek 
Published: January 2020

Abstract
We report results from multi-epoch radio astrometry of the Cassini spacecraft with the Very Long Baseline Array (VLBA). These observations are part of a program to determine a series of accurate positions for the Saturn system barycenter in the inertial International Celestial Reference Frame (ICRF) and to use these position measurements to improve our knowledge of Saturn’s orbit in the planetary ephemeris. Our VLBA observations cover the full duration of the orbital phase of the Cassini mission, from Saturn orbit insertion in 2004 to the end of mission in 2017. This period covers more than one-third of Saturn’s orbital period, allowing us to obtain good orbit constraints for Saturn, particularly on the inclination and ascending node longitude. During the early years of Cassini’s orbital mission our VLBA data dominated the determination of orbit orientation, while later in the mission range measurements become more significant. The orientation of Saturn’s orbit is now known to approximately 0.25 milli-arcseconds (1.25 nrad), an order of magnitude improvement since the start of Cassini observations. Continuing improvements in the ICRF position accuracy for our phase reference sources, and possible improvements in the final orbit solutions for Cassini, may lead to a still better Saturn orbit over the coming years.
Type IIP Supernova Progenitors. II. Stellar Mass and Obscuration by the Dust in the Circumstellar Medium
Authors: Wagle Gururaj A. , Ray Alak 
Published: January 2020

Abstract
It has been well established from a variety of observations that red supergiants (RSGs) lose a lot of mass in stellar wind. Dust that has formed in this emitted gas over a few decades before core-collapse can lead to substantial extinction and obscure the intrinsic luminosity of the progenitor RSG. This may lead to a difficulty in determining the range of progenitor masses that lead to the different classes of supernovae. Even nearby, well-studied supernovae with pre-explosion observations, such as SN 2013ej, may suffer from this uncertainty in the progenitor mass. We explore here two different masses proposed for its progenitor. We compute their pre-supernova characteristics using Modules for Experiments in Stellar Astrophysics. We show that a non-rotating star with an initial mass of 26 M
⊙ would require a considerable amount of circumstellar medium (A

V
∼ 3) to obscure its high luminosity given the observed pre-explosion magnitudes detected by the Hubble Space Telescope (HST). Such a high value of visual extinction appears to be inconsistent with that derived for SN 2013ej as well as SN 2003gd in the same host galaxy, M74. In contrast, the evolutionary models of a lower mass (13 M
⊙) star are easily accommodated within the observed HST magnitudes. Some of the 26 M
⊙ simulations show luminosity variation in the last few years, which could be discriminated by high-cadence and multiband monitoring of supernova candidates in nearby galaxies. We demonstrate that our calculations are well resolved with adequate zoning and evolutionary time steps.
Evolution from Spherical AGB Wind to Multipolar Outflow in Pre-planetary Nebula IRAS 17150−3224
Authors: Huang Po-Sheng , Lee Chin-Fei , Sahai Raghvendra 
Published: January 2020

Abstract
We have mapped the pre-planetary nebula IRAS 17150−3224 in the 350 GHz continuum and CO J = 3–2 line at an angular resolution of ∼0.″09 using the Atacama Large Millimeter/submillimeter Array. A continuum source is detected at the center of the nebula, elongated along the equatorial plane, likely tracing a dusty torus around the central source. Continuum emission is also detected on both sides of the central continuum source in the equatorial plane, probably resulting from interactions of collimated fast winds (CFWs) with envelope material in the equator. CO emission is detected along the optical lobe. Although the optical lobe appears as bipolar, the CO map shows that it is actually a quadrupolar outflow consisting of two overlapping bipolar outflows. Two additional younger bipolar outflows are also detected in CO, one at the lower latitude and the other along the equatorial plane. In the CO position–velocity maps, blueshifted absorption stripes are detected in the outflow emissions, due to absorption by a series of shells produced by a series of asymptotic giant branch (AGB) wind ejections. By modeling the morphology and kinematics of the AGB wind and outflows, we find that the AGB wind could have ended ∼1300 yr ago, the quadrupolar outflow was ejected ∼350 yr ago, and the two additional bipolar outflows were ejected ∼280 and 200 yr ago, respectively. The outflows could be produced either by bullets coming from an explosion, or by a precessing CFW with a time-dependent ejection velocity.
Investigation of Surface Effects of Simple Flux Tubes Using Numerical Simulations
Authors: Waidele M. , Roth M. 
Published: January 2020

Abstract
We use the SPARC code for MHD simulations with monolithic flux tubes of varying subsurface topology. Our studies involve the interactions of waves caused by a single source with subsurface magnetic fields. Mode conversion causing acoustic power to trickle downwards along the flux tube has been described before and can be visualized in our simulations. We show that this downward propagation causes the flux tube to act as an isolated source, creating a characteristic surface wave field. Measuring this wave field at the surface reveals subsurface properties of the magnetic field topology. Using time–distance helioseismology, we demonstrate how to detect such a flux tube signal based on a group travel time delay of Δt = 282.6 s due to the wave packet spending time subsurface as a slow mode wave. Although the amplitude is small and generally superimposed by the full wave field, it can be detected if assumptions about Δt are made. We demonstrate this for a simulation with solar-like sources. This kind of study has the potential to reveal subsurface information of sunspots based on the analysis of a surface signal.
Stellar Migration in Galaxy Disks Using the Chirikov Diffusion Rate
Authors: Wozniak Hervé 
Published: January 2020

Abstract
We are reexamining the problem of stellar migration in disk galaxies from a diffusion perspective. We use for the first time the formulation of the diffusion rates introduced by Chirikov, applied to both energy, E, and angular momentum, L

z
, in self-consistent N-body experiments. We limit our study to the evolution of stellar disks well after the formation of the bar, in a regime of adiabatic evolution. We show that distribution functions of Chirikov diffusion rates have similar shapes, regardless of the simulations, but different slopes for energy and angular momentum. Distribution functions of derived diffusion timescales, T

D
, also have the same form for all simulations, but are different for T

D
(E) and T

D
(L

z
). Diffusion timescales are strongly dependent on L

z
.

in a L

z
range roughly delimited by the set of stellar bar resonances (between the ultraharmonic resonance and the outer Lindblad resonance). Only particles with low L

z
have

, i.e., the simulation length. In terms of mass fraction, 35%–42% turn out to diffuse energy in a characteristic timescale shorter than 10 Gyr, i.e., simulations length, while 60%–64% undergo the diffusion of the angular momentum on the same timescale. Both the diffusion of L

z
and E are important to grasp the full characterization of the radial migration process, and we show that depending on the spatial region considered, one or the other diffusion dominates.
SOFIA/HAWC+ View of an Extremely Luminous Infrared Galaxy: WISE 1013+6112
Authors: Toba Yoshiki , Wang Wei-Hao , Nagao Tohru , Ueda Yoshihiro , Ueda Junko , Lim Chen-Fatt , Chang Yu-Yen , Saito Toshiki , Kawabe Ryohei 
Published: January 2020

Abstract
We present far-infrared (FIR) properties of an extremely luminous infrared galaxy (ELIRG) at z
spec = 3.703, WISE J101326.25+611220.1 (WISE 1013+6112). This ELIRG is selected as an IR-bright dust-obscured galaxy based on the photometry from the Sloan Digital Sky Survey and the Wide-field Infrared Survey Explorer (WISE). In order to derive its accurate IR luminosity, we perform follow-up observations at 89 and 154 μm using the High-resolution Airborne Wideband Camera-plus (HAWC+) on board the 2.7 m Stratospheric Observatory For Infrared Astronomy (SOFIA) telescope. We conduct spectral energy distribution (SED) fitting with CIGALE using 15 photometric data (0.4–1300 μm). We successfully pin down FIR SED of WISE 1013+6112 and its IR luminosity is estimated to be L
IR = (1.62 ± 0.08) × 1014
L
☉, making it one of the most luminous IR galaxies in the universe. We determine the dust temperature of WISE 1013+6112 is T
dust = 89 ± 3 K, which is significantly higher than that of other populations such as submillimeter galaxies and FIR-selected galaxies at similar IR luminosities. The resultant dust mass is M
dust = (2.2 ± 0.1) × 108
M
☉. This indicates that WISE 1013+6112 has a significant active galactic nucleus and star-forming activity behind a large amount of dust.
Expanding the Y Dwarf Census with Spitzer Follow-up of the Coldest CatWISE Solar Neighborhood Discoveries
Authors: Meisner Aaron M. , Caselden Dan , Kirkpatrick J. Davy , Marocco Federico , Gelino Christopher R. , Cushing Michael C. , Eisenhardt Peter R. M. , Wright Edward L. , Faherty Jacqueline K. , Koontz Renata , Marchese Elijah J. , Khalil Mohammed , Fowler John W. , Schlafly Edward F. 
Published: January 2020

Abstract
We present Spitzer 3.6 and 4.5 μm follow-up of 170 candidate extremely cool brown dwarfs newly discovered via the combination of Wide-field Infrared Survey Explorer (WISE) and NEOWISE imaging at 3–5 μm. CatWISE, a joint analysis of archival WISE and NEOWISE data, has improved upon the motion measurements of AllWISE by leveraging a >10× time baseline enhancement, from 0.5 yr (AllWISE) to 6.5 yr (CatWISE). As a result, CatWISE motion selection has yielded a large sample of previously unrecognized brown dwarf candidates, many of which have archival detections exclusively in the WISE 4.6 μm (W2) channel, suggesting that they could be both exceptionally cold and nearby. Where these objects go undetected in WISE W1 (3.4 μm), Spitzer can provide critically informative detections at 3.6 μm. Of our motion-confirmed discoveries, 17 have a best-fit Spitzer [3.6]–[4.5] color most consistent with spectral type Y. It is likely that CWISEP J144606.62–231717.8 (μ ≈ 1.″3 yr−1) is the reddest, and therefore potentially coldest, member of our sample with a very uncertain [3.6]–[4.5] color of 3.71 ± 0.44 mag. We also highlight our highest proper-motion discovery, WISEA J153429.75–104303.3, with μ ≈ 2.″7 yr−1. Given that the prior list of confirmed and presumed Y dwarfs consists of just 27 objects, the Spitzer follow-up presented in this work has substantially expanded the sample of identified Y dwarfs. Our new discoveries thus represent significant progress toward understanding the bottom of the substellar mass function, investigating the diversity of the Y dwarf population, and selecting optimal brown dwarf targets for James Webb Space Telescope spectroscopy.