bluuebunny/crossref_metadata_2025_split huggingface dataset:
New Products Based on Spelt for Restaurant Sector
Authors: Sakhno O. S. , Hryshchuk O. O. , Furmanova Y. P. , Pavliuchenko O. S. 
Published: June 2019

The spelt processed products that are presented on the Ukrainian food market have been analyzed in the paper. The comparative characteristics of chemical composition of spelt products – wholemeal flour, grits, flakes, bran – with same wheat and oat products have been investigated. Spelt flour and flakes are proposed for applying at the restaurant establishments. Authors havedeveloped technology of baked products for special dietician consumption – spelt crisp bread and spelt sweet bar as well. Spelt crisp bread contains linseed, sunflower seed, spices (cilantro, curcuma), herbs (fennel, parsley). Technology of this bread includes such operations as grinding of cleaned seeds, sifting of bran and flour, mixing of dry components, adding of kefir and water. Duration of first fermentation is 20 minutes, then rectangular shaping (5×13 cm) and drying at 80 oC during 4…5 hours, then cooling at ambient temperature near 30 min. Caloric value of spelt crisp bread is 260 kCal. Sensorial parameters of spelt crisp bread – rectangular shape, light brown colour, smooth top with inclusion of linseed and sunflower seed, pleasant taste and spicy aroma, crisp crust and thick texture. Sweet spelt bar is an example of beneficial sweets. It contains sunflower seed and pumpkin seed, nuts (walnut and almond), date, honey and sesame. Caloric value of spelt sweet bar is 220 kCal. Technology of this bread includes such operations as drying of spelt flakes at 120 oC during 2 min and further cooling, soaking of date in hot water during 3 min, removing of stone and grinding. Walnut is inspected due to the absence of walnut shell, almond is soaking for 3 hours, then parboiled and grinded. All ingredients are mixed during 5 min with honey. Then bar is rectangular shaping and served. Such bar has rectangular shape, ribbed top, crisp texture, light brown colour and intense walnut aroma.
Matias Aleksanteri Castrén ja Kalevalan ruotsinnos
Authors: Häkkinen Kaisa 
Published: June 2019

Kun Elias Lönnrotin kokoama runoeepos, ns. Vanha Kalevala, ilmestyi vuonna 1835, se käänsi suomen kielen ja suomalaisen kulttuurin arvostuksen huimaan nousuun. Kalevala innosti myös maisteriopintojaan viimeistelevää, alkuaan pappisuralle aikonutta Matias Aleksanteri Castrénia suuntaamaan huomionsa suomen ja sen sukukielten tutkimukseen.
Koska alkuperäistä Kalevalaa pystyivät lukemaan vain muutamat harvat oppineiston edustajat, Suomalaisen Kirjallisuuden Seura julisti kilpailun runomuotoisen ruotsin- tai saksankielisen käännöksen aikaansaamiseksi. Tällaisia ei kuitenkaan ilmaantunut. Helsingin yliopiston suomen kielen lehtori Carl Niclas Keckman luennoi Kalevalasta ja laati siitä sanatarkan ruotsinnoksen, mutta ei runomittaista versiota. Muutaman vuoden odotuksen jälkeen Kalevalasta jo aiemmin kiinnostunut Castrén ryhtyi kääntämään eeposta. Suomalaisen Kirjallisuuden Seuran stipendiaattina hän keräsi kesällä 1839 taustatietoa ja uutta kansanperinneaineistoa Vienan Karjalassa.
Aktiivinen kääntäminen kesti noin kaksi vuotta. Käännöstyön ohella Castrén julkaisi dosentinväitöskirjan ja joitakin pienempiä tieteellisiä tutkimuksia. Kevätlukukaudella 1841 Castrén luennoi Helsingin yliopistossa Kalevalasta ja viimeisteli käännöstään. Se ilmestyi kesäkuussa 1841 ja sai hyvän vastaanoton. Esimerkiksi historiallis-vertailevan kielentutkimuksen kärkiedustajiin kuulunut Jacob Grimm perehtyi Kalevalaan ja luennoi siitä Berliinin tiedeakatemiassa Castrénin ruotsinnoksen perusteella.
Castrénin ruotsinnos avasi uusia mahdollisuuksia Kalevalaa koskevalle tieteelliselle keskustelulle, koska eepos oli nyt aiempaa merkittävästi laajempien piirien luettavissa. Tärkeä rooli tässä keskustelussa oli itse Castrénilla ja hänen Kalevala-tulkinnoillaan. Kalevalan käännöksen myötä Castrén sai pysyvän kansainvälisen maineen arvostettuna kansanperinteen ja mytologian asiantuntijana. Kirjoitus perustuu Suomalais-Ugrilaisessa Seurassa 15.2.2019 pidettyyn esitelmään.
RETRACTED: CDX2/mir-145-5p/SENP1 Pathways Affect LNCaP Cells Invasion and Migration
Authors: He Jin-Hua , Han Ze-Ping , Zou Mao-Xian , He Meng-Ling , Li Yu-Guang , Zheng Lei 
Published: June 2019

Background/Aims: Recently, rapidly accumulating evidence has shown that microRNAs (miRNAs) are involved in human tumorigenesis, and the dysregulation of miRNAs has been observed in many cancers, including prostate cancer. miR-145-5p, an miRNA with reduced expression in prostate cancer cells, has been shown to have a tumor suppressive role in a variety of tumors. However, its underlying mechanism requires further elucidation.Methods: A lentiviral expression vector for miR-145-5p was constructed and used to establish a stable cell line (LNCaP) expressing miR-145-5p. The cells were cultured normally and divided into the control group (control), negative control group (negative control), and test group (miR-145-5p). Inhibition of proliferation was measured by a WST-8 assay. The early apoptosis rate of cells was detected by flow cytometry. Clone formation ability was detected by a clone formation inhibition test. Cell invasion and migration capacity was detected by a Transwell assay. The relative expression levels of proteins were detected by western blotting. We constructed a nude mouse model of prostate cancer to observe the effect of miR-145-5p on the growth of transplanted tumors. TargetScan bioinformatics software was used to predict target genes regulated by miR-14-5p. ChIPBase was used to predict transcription factors with binding sites in the upstream promoter region of miR-145-5p. Quantitative reverse transcription PCR was used to detect the relative expression level of genes. A bifluorescence-reporter gene vector was constructed to confirm the regulation of target genes by miR-145-5p. We used 5′ rapid amplification of cDNA ends to confirm the transcription start site of miR-145-5p.Chromatin immunoprecipitation technology was used to detect the effect of transcription factors binding to miR-145-5p.Results: The overexpression of miR-145-5p not only inhibited the proliferation, invasion, and migration of LNCaP cells but also promoted their early apoptosis. After overexpressing miR-145-5p, the expression of small ubiquitin-like modifier protein-specific protease 1 (SENP1), and caudal-related homeobox 2 (CDX2) protein was decreased in LNCaP cells. The transcription factor CDX2 bound to the miR-145-5p promoter region and inhibited its transcription. The transcription start site of miR-145-5p was located at a guanine residue 1,408 bp upstream of the stem-loop sequence. Upon overexpression, miR-145-5p could bind to the 3′-untranslated region of SENP1 to inhibit its translation.Conclusion: These results suggested that CDX2 inhibits the expression of miR-145-5p, thereby relieving the inhibitory effect of miR-145-5p on the translation of SENP1 and affecting the invasion and migration of prostate cancer cells.
ANALISIS FAKTOR-FAKTOR YANG MEMENGARUHI SKEPTISISME PROFESIONAL AUDITOR
Authors: H Novayanti Anggraini , Y Rahmawati Hanny 
Published: June 2019

The purpose of this study was to determine the extent to which the factors of competence, objectivity, integrity, experience, independence, and the risk of an effect on the auditor's professional skepticism. This type of research in this study is a qualitative research. The population in this study is the auditors who work in public accounting firm in the whole area of Central Jakarta. The sampling technique in this study were selected through purposive sampling technique. The number of samples in this study is 24 KAP with 150 respondents. Analysis of data using regression analysis. The result of this research is the competence of auditors have an influence on the auditor's professional skepticism . Objectivity auditor has an influence on the auditor's professional skepticism. Integrity auditor has an influence on the auditor's professional skepticism. Experience auditor has an influence on the auditor's professional skepticism. Auditor independence have an influence on the auditor's professional skepticism. Risk auditor has an influence on the auditor's professional skepticism. And competence audior , auditor objectivity, integrity auditor , auditor experience , auditor independence and auditor risk together have an influence on the auditor's professional skepticism .
PENGARUH PARTISIPASI ANGGARAN, PENEKANAN ANGGARAN, DAN KOMITMEN ORGANISASI TERHADAP SENJANGAN ANGGARAN PADA SUKU DINAS PEMERINTAHAN DI DKI JAKARTA
Authors: Putra I Gede Eka Dharma , Mintoyuwono Danang 
Published: June 2019

The study aims to determine the influence of budgetary participation, budget emphasis and organisation commitment on budgetary slcak. Respondents were studied were departement chief, head of subsection, and section chief in departements at west jakarta, south jakarta, north jakarta, central jakarta, and east jakarta . Data collection techniques in this research using primary data by distributing questionnaires to 211 respondents. Technique data processing was performed using SPSS 21 and assisted by using microsoft office 2010. The variables studied consisted of budgetary participation, budget emphasis, organisation commitment and budgetary slack. The analysis used to test this research is multiple linear regression test. Partial results of the study showed absence of budgetary participation significant effect on budgetary slack, the absence of budget emphasis on budgetary slack, and absence of organisation commitment on budgetary slack. From the results of simultaneous studies showed a significant effect between the variables of budgetary participation, budget emphasis, organisation commitment on budgetary slack.
ANALISA PENGARUH PERTUMBUHAN KREDIT, JENIS KREDIT, TINGKAT BUNGA PINJAMAN BANK DAN INFLASI TERHADAP KREDIT BERMASALAH
Authors: Saputro Arfan Rachmadias , Sarumpaet Susi , Prasetyo Tri Joko 
Published: June 2019

Abstract: This research was conducted to analyze the effect of loan growth, loan type, interest and inflation on non-performing loan. Samples were focused on Indonesian commercial banks. Multiple regression linear analysis was used, whereas the samples were obtained using purposive sampling method. Total sample consists of 82 commercial banks with financial statements for the year of 2013 to 2017. Result shows that each variable; loan growth, loan type and interest have a positive effect on non-performing loan. On the other hand, inflation has a negative effect. Keywords: Loan Growth, Loan Type, Interest, Inflation, Non-Performing Loan.
ДО ПРОБЛЕМИ РОЗВИТКУ ЕМОЦІЙНОГО ІНТЕЛЕКТУ ОСОБИСТОСТІ
Authors: Стельмашук Жанна Григорівна 
Published: June 2019

У статті на основі здійсненого теоретичного аналізу розкрито сутність феномену емоційного інтелекту як особливого конструкта та здатності особистості.
Приділено увагу вітчизняним та зарубіжним концепціям у розумінні емоційного інтелекту, їх спільним та відмінним позиціям стосовно його структури та ґенези розвитку.
Доведено, що термін «емоційний інтелект» розглядається як здатність до розпізнання, розуміння емоцій і управління ними; служить для визначення сукупності здібностей, знань та вмінь, пов’язаних з регуляцією емоційної сфери особистості, необхідних для успішної соціалізації та комунікації.
Схарактеризовано дві форми репрезентації поняття «емоційний інтелект»: міжособистісний емоційний інтелект (спроможність людини розуміти інших людей, усвідомлювати мотиви їхньої діяльності, ставлення їх до роботи, вирішувати, як краще співпрацювати з цими людьми) та внутрішньоособистісний емоційний інтелект (властивість людини, спрямована на себе: спроможність формувати точну адекватну модель власного «я» та використовувати цю модель, щоб ефективно функціонувати у житті).
Обґрунтовано доцільність розглядати емоційний інтелект як інтегральну властивість особистості, що забезпечує здатність розуміти емоції та управляти ними через когнітивну обробку емоційної інформації.
Зроблено висновок, що емоційний інтелект як наскрізне уміння учня Нової української школи знайшло своє обґрунтування у наукових дослідженнях з психології, але є практично недослідженим у педагогічній теорії та практиці.
The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au
Authors: Nielsen Eric L. , De Rosa Robert J. , Macintosh Bruce , Wang Jason J. , Ruffio Jean-Baptiste , Chiang Eugene , Marley Mark S. , Saumon Didier , Savransky Dmitry , Mark Ammons S. , Bailey Vanessa P. , Barman Travis , Blain Célia , Bulger Joanna , Burrows Adam , Chilcote Jeffrey , Cotten Tara , Czekala Ian , Doyon Rene , Duchêne Gaspard , Esposito Thomas M. , Fabrycky Daniel , Fitzgerald Michael P. , Follette Katherine B. , Fortney Jonathan J. , Gerard Benjamin L. , Goodsell Stephen J. , Graham James R. , Greenbaum Alexandra Z. , Hibon Pascale , Hinkley Sasha , Hirsch Lea A. , Hom Justin , Hung Li-Wei , Ilene Dawson Rebekah , Ingraham Patrick , Kalas Paul , Konopacky Quinn , Larkin James E. , Lee Eve J. , Lin Jonathan W. , Maire Jérôme , Marchis Franck , Marois Christian , Metchev Stanimir , Millar-Blanchaer Maxwell A. , Morzinski Katie M. , Oppenheimer Rebecca , Palmer David , Patience Jennifer , Perrin Marshall , Poyneer Lisa , Pueyo Laurent , Rafikov Roman R. , Rajan Abhijith , Rameau Julien , Rantakyrö Fredrik T. , Ren Bin , Schneider Adam C. , Sivaramakrishnan Anand , Song Inseok , Soummer Remi , Tallis Melisa , Thomas Sandrine , Ward-Duong Kimberly , Wolff Schuyler 
Published: June 2019

Abstract
We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M
* > 1.5 M
⊙ more likely to host planets with masses between 2 and 13M
Jup and semimajor axes of 3–100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M
* > 1.5 M
⊙) of the form

, finding α = −2.4 ± 0.8 and β = −2.0 ± 0.5, and an integrated occurrence rate of

% between 5–13M
Jup and 10–100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with

% of stars hosting a brown dwarf companion between 13–80M
Jup and 10–100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.
Evolution of the Suprathermal Proton Population at Interplanetary Shocks
Authors: Lario D. , Berger L. , Decker R. B. , Wimmer-Schweingruber R. F. , Wilson L. B. , Giacalone J. , Roelof E. C. 
Published: June 2019

Abstract
We investigate the evolution of the suprathermal (ST) proton population as interplanetary shocks cross 1 au. The variability of the ST proton intensities and energy spectra upstream of the shocks is analyzed in terms of the shock parameters, upstream magnetic field configurations, and preexisting upstream populations. Propitious conditions for the observation of ST particles at distances far upstream from the shock occur in parallel shock configurations when particles can easily escape from the shock vicinity. In this situation, ST intensity enhancements show onsets characterized by velocity dispersion effects and energy spectra that develop into a “hump” profile peaking around ∼10 keV just before the arrival of the shock. The observation of field-aligned proton beams at low energies (5–10 keV) is possible under conditions that facilitate the scatter-free propagation of the particles streaming out of the shock. Upstream of perpendicular shocks, ST intensity enhancements are only observed in close proximity to the shock. Power-law proton spectra develop downstream of the shocks. The functional form for the downstream phase-space density proportional to v
−5 is observed only over a limited range of ST energies. The absence of ST populations observed far upstream of interplanetary shocks raises questions about whether ST protons contribute as a seed particle population in the processes of particle acceleration at shocks.
Discovery of a White Dwarf Companion to HD 159062
Authors: Hirsch Lea A. , Ciardi David R. , Howard Andrew W. , Marcy Geoffrey W. , Ruane Garreth , Gonzalez Erica , Blunt Sarah , Crepp Justin R. , Fulton Benjamin J. , Isaacson Howard , Kosiarek Molly , Mawet Dimitri , Sinukoff Evan , Weiss Lauren 
Published: June 2019

Abstract
We report on the discovery of a white dwarf companion to the nearby late G dwarf star, HD 159062. The companion is detected in 14 years of precise radial velocity (RV) data, and in high-resolution imaging observations. RVs of HD 159062 from 2003 to 2018 reveal an acceleration of −13.3 ± 0.12

, indicating that it hosts a companion with a long-period orbit. Subsequent imaging observations with the ShaneAO system on the Lick Observatory 3 m Shane telescope, the PHARO AO system on the Palomar Observatory 5 m telescope, and the NIRC2 AO system at the Keck II 10 m telescope reveal a faint companion 2.″7 from the primary star. We performed relative photometry, finding ΔJ = 10.09 ± 0.38 mag,

mag, and

mag for the companion from these observations. Analysis of the radial velocities, astrometry, and photometry reveals that the combined data set can only be reconciled for the scenario where HD 159062 B is a white dwarf. A full Bayesian analysis of the RV and imaging data to obtain the cooling age, mass, and orbital parameters of the white dwarf indicates that the companion is an old

white dwarf with an orbital period of

yr, and a cooling age of

Gyr.
Statistical Study of Whistler Waves in the Solar Wind at 1 au
Authors: Tong Yuguang , Vasko Ivan Y. , Artemyev Anton V. , Bale Stuart D. , Mozer Forrest S. 
Published: June 2019

Abstract
Whistler waves are intermittently present in the solar wind, while their origin and effects are not entirely understood. We present a statistical analysis of magnetic field fluctuations in the whistler frequency range (above 16 Hz) based on about 801,500 magnetic field spectra measured over 3 yr aboard the Artemis spacecraft in the pristine solar wind. About 13,700 spectra (30 hr in total) with intense magnetic field fluctuations satisfy the interpretation in terms of quasi-parallel whistler waves. We provide estimates of the whistler wave occurrence probability, amplitudes, frequencies, and bandwidths. The occurrence probability of whistler waves is shown to strongly depend on the electron temperature anisotropy. The whistler wave amplitudes are in the range from about 0.01 to 0.1 nT and typically below 0.02 of the background magnetic field. The frequencies of the whistler waves are shown to be below an upper bound that is dependent on β

e
. The correlations established between the whistler wave properties and local macroscopic plasma parameters suggest that the observed whistler waves can be generated in local plasmas by the whistler heat flux instability. The whistler wave amplitudes are typically small, which questions the hypothesis that quasi-parallel whistler waves are capable to regulate the electron heat flux in the solar wind. We show that the observed whistler waves have sufficiently wide bandwidths and small amplitudes, so that effects of the whistler waves on electrons can be addressed in the frame of the quasi-linear theory.
Two-step Evolution of a Rising Flux Rope Resulting in a Confined Solar Flare
Authors: Yang Shuhong , Zhang Jun , Song Qiao , Bi Yi , Li Ting 
Published: June 2019

Abstract
Combining the Solar Dynamics Observatory and the New Vacuum Solar Telescope observations, we study a confined flare triggered by a rising flux rope within the trailing sunspots of active region 12733. The flux rope lying above the sheared polarity inversion line can be constructed through magnetic extrapolation but could not be detected in multiwavelength images at the pre-flare stage. The conspicuous shearing motions between the opposite-polarity fields in the photosphere are considered to be responsible for the flux rope formation. The maximum twist of the flux rope is as high as −1.76, and then the flux rope rises due to the kink instability. Only when the flare starts can the flux rope be observed in high-temperature wavelengths. The differential emission measure results confirm that this flux rope is a high-temperature structure. Associated with the rising flux rope, there appear many post-flare loops and a pair of flare ribbons. When the rising flux rope meets and reconnects with the large-scale overlying field lines, a set of large-scale twisted loops are formed, and two flare ribbons propagating in opposite directions appear on the outskirts of the former ribbons, indicating that the twist of the flux rope is transferred to a much larger system. These results imply that the external reconnection between the rising flux rope and the large-scale overlying loops plays an important role in the confined flare formation.
ALMA Polarimetry of AT2018cow
Authors: Huang Kuiyun , Shimoda Jiro , Urata Yuji , Toma Kenji , Yamaoka Kazutaka , Asada Keiichi , Nagai Hiroshi , Takahashi Satoko , Petitpas Glen , Tashiro Makoto 
Published: June 2019

Abstract
We present the first radio polarimetric observations of a fast-rising blue optical transient, AT2018cow. Two epochs of polarimetry with additional coincident photometry were performed with the Atacama Large Millimeter/submillimeter Array. The overall photometric results based on simultaneous observations in the 100 and 230 GHz bands are consistent with the nonthermal radiation model reported by Ho et al. and indicate that the spectral peaks (∼110 GHz at the first epoch and ∼67 GHz at the second epoch) represent the synchrotron self-absorption frequency. The non-detection of linear polarization with <0.15% in the 230 GHz band at the phase when the effect of synchrotron self-absorption was quite small in the band may be explained by internal Faraday depolarization with high circumburst density and strong magnetic field. This result supports the stellar explosion scenario rather than the tidal disruption model. The maximum energy of accelerating particles at the shocks of AT2018cow-like objects is also discussed.