bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGARUH KEPERCAYAAN DAN KEMUDAHAN TERHADAP KEPUTUSAN PEMBELIAN BELANJA SECARA ONLINE
Authors: Sandora Meri 
Published: November 2020

Penelitian ini dilakukan pada mahasiswa yang berbelanja secara online pada website-website berbasis aplikasi pada internet. Adapun Jenis data yang digunakan dalam penelitian ini adalah data primer dan data sekunder. Pengambilan sampel dilakukan dengan menggunakan metode snowball sampling. Sedangkan untuk mengetahui besarnya pengaruh variabel bebas (X) terhadap variabel terikat (Y) digunakan analisa Regresi Linear Berganda Berdasarkan hasil Uji Regresi Linear Berganda di peroleh persamaan: Y = 7,994 + 0,243X1 + 0,149X2 + ε. Kemudian secara simultan didapatkan bahwa kepercayaan dan kemudahan memiliki pengaruh terhadap keputusan pembelian berbelanja secara online. Sedangkan secara parsial baik itu variabel kepercayaan maupun variabel kemudahan memiliki pengaruh terhadap keputusan pembelian berbelanja secara online. Sedangkan kepercayaan dan kemudahan dapat mempengaruhi keputusan pembelian berbelanja secara online sebesar 18,4%, sementara sisanya dipengaruhi oleh variabel lain yang tidak diteliti dalam penelitian ini. Disisi lain konsumen belumlah percaya sepenuhnya melakukan transaksi berbelanja pada toko online yang ada di website. Namun sebagian besar (80%) mengatakan kemudahan mereka berbelanja pada toko online, seperti mudah dipelajari, mudah digunakan, mudah untuk dilakukan, dan mudah untuk memperoleh informasi produk
Pseudoleucite syenites at Loch Borralan, Scotland: Petrology and a genetic model
Authors: Reich Rebekka , Marks Michael A. W. , Wenzel Thomas , Markl Gregor 
Published: November 2020

ABSTRACT
The alkaline Loch Borralan intrusion (Assynt Region, NW Highlands of Scotland) consists of a composite arrangement of several ultramafic to felsic plutonic rock bodies which were emplaced around 430 Ma into the Moine Thrust Zone during the Caledonian Orogeny. Some of the Loch Borralan rocks are ultrapotassic and contain pseudoleucite, i.e., a pseudomorph of alkali feldspar and nepheline after leucite. In total, 25 samples have been investigated, representing garnet-bearing pseudoleucite syenites and accompanying rock types such as nepheline-garnet-bearing syenites, alkali feldspar syenites, an amphibole syenite, a biotite-clinopyroxene syenite, and calcite-bearing glimmerites.
Pseudoleucite is always associated with garnet, biotite, orthoclase, and minor clinopyroxene and titanite. Mineral chemical data indicate rather primitive magma compositions with no major differences between the various investigated main rock units. The abundant occurrence of up to 2 cm large, mostly euhedral pseudoleucite crystals and petrological phase considerations suggest that magmatic leucite physically separated from its host magma as a flotation cumulate. Based on our data and a comparison with previous field-based and experimental work, K-rich basanitic to tephriphonolitic melts that originated from a K-enriched mantle source may be parental to these rocks. The high liquidus temperatures at low pressures (e.g., ∼1100 °C at 1 bar PH2O) required to crystallize leucite could have resulted from the ascent of successive melt batches in a composite intrusion. Later melt batches would increase the temperature in earlier, already partially cooled batches, causing an increase in temperature and a decrease in pressure during ascent. The subsequent decomposition of leucite to pseudoleucite is interpreted to result from either dry breakdown or autometasomatism, i.e., involvement of late-magmatic fluids.
Chiyokoite, Ca3Si(CO3)[B(OH)4]O(OH)5·12H2O, a new ettringite-group mineral from the Fuka mine, Okayama Prefecture, Japan
Authors: Lykova Inna , Chukanov Nikita V. , Pekov Igor V. , Yapaskurt Vasiliy O. , Pautov Leonid A. , Karpenko Vladimir Yu. , Belakovskiy Dmitry I. , Varlamov Dmitry A. , Britvin Sergey N. , Scheidl Katharina S. 
Published: November 2020

ABSTRACT
The new ettringite-group mineral chiyokoite, ideally Ca3Si(CO3)[B(OH)4]O(OH)5·12H2O, was found in a hydrothermally altered calc-silicate skarn at the Fuka mine, Okayama Prefecture, Japan. Associated minerals are calcite, henmilite, and tacharanite. Chiyokoite occurs as hexagonal prismatic crystals up to 30 μm long and up to 20 μm thick. The major forms are the hexagonal prism {100} and monohedra {0001} and {000}. The crystals are combined in clusters which form friable nests up to 1 cm across. The mineral is pink to colorless with white streak and vitreous luster. The cleavage is parallel to {100} and {0001}, good. The fracture is stepped. Dmeas is 1.85(1) g/cm3, Dcalc is 1.85 g/cm3. Chiyokoite is optically uniaxial (–), ω = 1.523(2) and ε = 1.492(3) (589 nm). The infrared spectrum is reported. The chemical composition (wt.%) is CaO 27.56, B2O3 3.47, Al2O3 3.05, Fe2O3 0.12, As2O3 4.77, MnO2 0.32, SiO2 6.55, SO3 0.76, H2O 46.3, CO2 7.30, total 100.2. The empirical formula calculated on the basis of 3 Ca apfu is H31.37Ca3(Si0.67Al0.37Mn4+0.02Fe3+0.01)Σ1.07(C1.01B0.61As3+0.29S0.06)Σ1.97O24.19. The simplified general formula is Ca3(Si,Al)(CO3,AsO3)[B(OH)4,AsO3](OH)6·12H2O. Chiyokoite is hexagonal, P63, a = 11.0119(5), c = 10.5252(6) Å, and V = 1105.3(1) Å3. The strongest reflections of the powder X-ray diffraction pattern [d,Å(I)(hkl)] are: 9.53(100)(100), 5.50(24)(110), 4.618(11)(102), 3.812(23)(112), 3.412(15)(211), 2.726(14)(302), 2.521(19)(123), and 2.172(13)(320,402,223). The crystal structure, refined from single-crystal X-ray diffraction data [R1(F) = 0.042], is based on [Ca3(Si,Al)(OH)6(H2O)12] columns parallel to the c axis with B(OH)4– and CO32– and admixed AsO33– anionic groups in channels between the columns. The mineral is named in honor of Professor Chiyoko Henmi (1949–2018).
Відносне зростання рядів Діріхле з різними абсцисами абсолютної збіжності
Authors: Mulyava O. M. , Sheremeta M. M. 
Published: November 2020

УДК 517.537.72
We study the growth of a Dirichlet series with zero abscissa of absolute convergence with respect to the entire Dirichlet series by using the generalized quantities of order and lower order where is the function inverse to and is a positive increasing function growing to
The Statistical Relationship between White-light Emission and Photospheric Magnetic Field Changes in Flares
Authors: Castellanos Durán J. Sebastián , Kleint Lucia 
Published: November 2020

Abstract
Continuum emission, also called white-light emission (WLE), and permanent changes of the magnetic field (ΔB
LOS) are often observed during solar flares. However, their relation and precise mechanisms are still unknown. We study statistically the relationship between ΔB
LOS and WLE during 75 solar flares of different strengths and locations on the solar disk. We analyze SDO/HMI data and determine for each pixel in each flare if it exhibited WLE and/or ΔB
LOS. We then investigate the occurrence, strength, and spatial size of the WLE, its dependence on flare energy, and its correlation to the occurrence of ΔB
LOS. We detected WLE in 44/75 flares and ΔB
LOS in 59/75 flares. We find that WLE and ΔB
LOS are related, and their locations often overlap between 0% and 60%. Not all locations coincide, thus potentially indicating differences in their origin. We find that the WL area is related to the flare class by a power law, and extend the findings of previous studies, that the WLE is related to the flare class by a power law, to also be valid for C-class flares. To compare unresolved (Sun-as-a-star) WL measurements with our data, we derive a method to calculate temperatures and areas of such data under the blackbody assumption. The calculated unresolved WLE areas improve, but still differ to the resolved flaring area by about a factor of 5–10 (previously 10–20), which could be explained by various physical or instrumental causes. This method could also be applied to stellar flares to determine their temperatures and areas independently.
Precision Orbital Dynamics from Interstellar Scintillation Arcs for PSR J0437–4715
Authors: Reardon Daniel J. , Coles William A. , Bailes Matthew , Bhat N. D. Ramesh , Dai Shi , Hobbs George B. , Kerr Matthew , Manchester Richard N. , Osłowski Stefan , Parthasarathy Aditya , Russell Christopher J. , Shannon Ryan M. , Spiewak Renée , Toomey Lawrence , Tuntsov Artem V. , van Straten Willem , Walker Mark A. , Wang Jingbo , Zhang Lei , Zhu Xing-Jiang 
Published: November 2020

Abstract
Intensity scintillations of radio pulsars are known to originate from interference between waves scattered by the electron density irregularities of interstellar plasma, often leading to parabolic arcs in the two-dimensional power spectrum of the recorded dynamic spectrum. The degree of arc curvature depends on the distance to the scattering plasma and its transverse velocity with respect to the line of sight. We report the observation of annual and orbital variations in the curvature of scintillation arcs over a period of 16 yr for the bright millisecond pulsar, PSR J0437−4715. These variations are the signature of the relative transverse motions of Earth, the pulsar, and the scattering medium, which we model to obtain precise measurements of parameters of the pulsar’s binary orbit and the scattering medium itself. We observe two clear scintillation arcs in most of our >5000 observations, and we show that they originate from scattering by thin screens located at distances D
1 = 89.8 ± 0.4 pc and D
2 = 124 ± 3 pc from Earth. The best-fit scattering model we derive for the brightest arc yields the pulsar’s orbital inclination angle, i = 137.°1 ± 0.°3, and longitude of ascending node, Ω = 206.°3 ± 0.°4. Using scintillation arcs for precise astrometry and orbital dynamics can be superior to modeling variations in the diffractive scintillation timescale, because the arc curvature is independent of variations in the level of turbulence of interstellar plasma. This technique can be used in combination with pulsar timing to determine the full three-dimensional orbital geometries of binary pulsars and provides parameters essential for testing theories of gravity and constraining neutron star masses.
Radio and X-Ray Observations of Short-lived Episodes of Electron Acceleration in a Solar Microflare
Authors: Sharma Rohit , Battaglia Marina , Luo Yingjie , Chen 陈 Bin 彬 , Yu 余 Sijie 思捷 
Published: November 2020

Abstract
Solar flares are sudden energy release events in the solar corona, resulting from magnetic reconnection, that accelerate particles and heat the ambient plasma. During a flare, there are often multiple temporally and spatially separated individual energy release episodes that can be difficult to resolve depending on the observing instrument. We present multiwavelength imaging and spectroscopy observations of multiple electron acceleration episodes during a GOES B1.7-class two-ribbon flare on 2012 February 25, observed simultaneously with the Karl G. Jansky Very Large Array at 1–2 GHz, the Reuven Ramatay High Energy Solar Spectroscopic Imager in X-rays, and the Solar Dynamics Observatory in extreme ultraviolet. During the initial phase of the flare, five radio bursts were observed. A nonthermal X-ray source was seen to be cotemporal but not cospatial with the first three radio bursts. Their radio spectra are interpreted as optically thick gyrosynchrotron emission. By fitting the radio spectra with a gyrosynchrotron model, we derive the magnetic field strength and nonthermal electron spectral parameters in each acceleration episode. Notably, the nonthermal parameters derived from X-rays differ considerably from the nonthermal parameters inferred from the radio. The observations are indicative of multiple cotemporal acceleration episodes during the impulsive phase of a solar microflare. The X-ray and radio burst sources likely originate from separate electron distributions in different magnetic loops.
First Discovery of a Fast Radio Burst at 350 MHz by the GBNCC Survey
Authors: Parent E. , Chawla P. , Kaspi V. M. , Agazie G. Y. , Blumer H. , DeCesar M. , Fiore W. , Fonseca E. , Hessels J. W. T. , Kaplan D. L. , Kondratiev V. I. , LaRose M. , Levin L. , Lewis E. F. , Lynch R. S. , McEwen A. E. , McLaughlin M. A. , Mingyar M. , Noori H. Al , Ransom S. M. , Roberts M. S. E. , Schmiedekamp A. , Schmiedekamp C. , Siemens X. , Spiewak R. , Stairs I. H. , Surnis M. , Swiggum J. , Leeuwen J. van 
Published: November 2020

Abstract
We report the first discovery of a fast radio burst (FRB), FRB 20200125A, by the Green Bank Northern Celestial Cap (GBNCC) Pulsar Survey conducted with the Green Bank Telescope at 350 MHz. FRB 20200125A was detected at a Galactic latitude of 58.°43 with a dispersion measure of 179 pc cm3, while electron density models predict a maximum Galactic contribution of 25 pc cm3 along this line of sight. Moreover, no apparent Galactic foreground sources of ionized gas that could account for the excess DM are visible in multiwavelength surveys of this region. This argues that the source is extragalactic. The maximum redshift for the host galaxy is z
max = 0.17, corresponding to a maximum comoving distance of approximately 750 Mpc. The measured peak flux density for FRB 20200125A is 0.37 Jy, and we measure a pulse width of 3.7 ms, consistent with the distribution of FRB widths observed at higher frequencies. Based on this detection and assuming a Euclidean flux density distribution of FRBs, we calculate an all-sky rate at 350 MHz of

FRBs sky−1 day−1 above a peak flux density of 0.42 Jy for an unscattered pulse having an intrinsic width of 5 ms, consistent with rates reported at higher frequencies, albeit with large uncertainties. Given the recent improvements in our single-pulse search pipeline, we also revisit the GBNCC survey sensitivity to various burst properties. Finally, we find no evidence of strong interstellar scattering in FRB 20200125A, adding to the growing evidence that some FRBs have circumburst environments where free–free absorption and scattering are not significant.
X-Ray through Very High Energy Intrabinary Shock Emission from Black Widows and Redbacks
Authors: van der Merwe C. J. T. , Wadiasingh Z. , Venter C. , Harding A. K. , Baring M. G. 
Published: November 2020

Abstract
Black widow and redback systems are compact binaries in which a millisecond pulsar heats and may even ablate its low-mass companion by its intense wind of relativistic particles and radiation. In such systems, an intrabinary shock can form as a site of particle acceleration and associated nonthermal emission. We model the X-ray and gamma-ray synchrotron and inverse Compton spectral components for select spider binaries, including diffusion, convection, and radiative energy losses in an axially symmetric, steady-state approach. Our new multizone code simultaneously yields energy-dependent light curves and orbital-phase-resolved spectra. Using parameter studies and matching the observed X-ray spectra and light curves, as well as Fermi Large Area Telescope spectra where available, with a synchrotron component, we can constrain certain model parameters. For PSR J1723–2837 these are notably the magnetic field and bulk flow speed of plasma moving along the shock tangent, the shock acceleration efficiency, and the multiplicity and spectrum of pairs accelerated by the pulsar. This affords a more robust prediction of the expected high-energy and very high energy gamma-ray flux. We find that nearby pulsars with hot or flaring companions may be promising targets for the future Cerenkov Telescope Array. Moreover, many spiders are likely to be of significant interest to future MeV-band missions such as AMEGO and e-ASTROGAM.
The Faint End of the Quasar Luminosity Function at z ∼ 5 from the Subaru Hyper Suprime-Cam Survey
Authors: Niida Mana , Nagao Tohru , Ikeda Hiroyuki , Akiyama Masayuki , Matsuoka Yoshiki , He Wanqiu , Matsuoka Kenta , Toba Yoshiki , Onoue Masafusa , Kobayashi Masakazu A. R. , Taniguchi Yoshiaki , Furusawa Hisanori , Harikane Yuichi , Imanishi Masatoshi , Kashikawa Nobunari , Kawaguchi Toshihiro , Komiyama Yutaka , Shirakata Hikari , Terashima Yuichi , Ueda Yoshihiro 
Published: November 2020

Abstract
We present the quasar luminosity function at z ∼ 5 derived from the optical wide-field survey data obtained as a part of the Subaru strategic program (SSP) with the Hyper Suprime-Cam (HSC). From a ∼81.8 deg2 area in the Wide layer of the HSC-SSP survey, we selected 224 candidates of low-luminosity quasars at z ∼ 5 by adopting the Lyman-break method down to i = 24.1 mag. Based on our candidates and spectroscopically confirmed quasars from the Sloan Digital Sky Survey (SDSS), we derived the quasar luminosity function at z ∼ 5, covering a wide luminosity range of −28.76 < M
1450 < −22.32 mag. We found that the quasar luminosity function is fitted by a double power-law model with a break magnitude of

mag. The inferred number density of low-luminosity quasars is lower, and the derived faint-end slope,

, is flatter than those of previous studies at z ∼ 5. A compilation of the quasar luminosity function at 4 ≤ z ≤ 6 from the HSC-SSP suggests that there is little redshift evolution in the break magnitude and in the faint-end slope within this redshift range, although previous studies suggest that the faint-end slope becomes steeper at higher redshifts. The number density of low-luminosity quasars decreases more rapidly from z ∼ 5 to z ∼ 6 than from z ∼ 4 to z ∼ 5.
The X-Ray Fundamental Plane of the Platinum Sample, the Kilonovae, and the SNe Ib/c Associated with GRBs
Authors: Dainotti M. G. , Lenart A. Ł. , Sarracino G. , Nagataki S. , Capozziello S. , Fraija N. 
Published: November 2020

Abstract
A large fraction of gamma-ray burst (GRB) lightcurves (LCs) show X-ray plateaus. We analyze all GRBs with known redshifts presenting plateaus observed by The Neil Gehrels Swift Observatory from its launch until 2019 August. The fundamental plane relation between the rest-frame time and X-ray luminosity at the end of the plateau emission and the peak prompt luminosity holds for all the GRB classes when selection biases and cosmological evolutions are applied. We have discovered two important findings: (1) a new class of long GRBs with good data coverage: the platinum sample; and (2) the platinum, the SNe-LGRB, and the KN-SGRB samples, yield the smallest intrinsic scatter with σ
platinum,GRB−SNe = 0.22 ± 0.10 and σ
KN−SGRB = 0.24 ± 0.12. The SNe-LGRBs are composed of GRBs associated spectroscopically with the SNe Ib,c, the KN-SGRBs are composed by eight GRBs associated with kilonovae or where there could have been such an association. The highest correlation coefficients are yielded for the SN-LGRB-ABC sample, which includes GRBs spectroscopically associated with SNe Ib/c or with a clear optical bump in the LC resembling the SNe Ib/c, (

), the SN-LGRBs (

), and the KN-SGRBs (

) when the redshift evolution is considered. These category planes are reliable candidates to use as cosmological tools. Furthermore, the distance from the gold fundamental plane is a crucial discriminant among classes. In fact, we find that the distributions of the distances of the SNe-LGRB, SNe-LGRB-ABC, KN-SGRB, and SGRB samples from the gold fundamental plane are statistically different from the distribution of the gold GRBs’ distances from the gold fundamental plane with and without considering evolution cases.
Investigating the Effect of Galaxy Interactions on the Enhancement of Active Galactic Nuclei at 0.5 < z < 3.0
Authors: Shah Ekta A. , Kartaltepe Jeyhan S. , Magagnoli Christina T. , Cox Isabella G. , Wetherell Caleb T. , Vanderhoof Brittany N. , Calabro Antonello , Chartab Nima , Conselice Christopher J. , Croton Darren J. , Donley Jennifer , Groot Laura de , de la Vega Alexander , Hathi Nimish P. , Ilbert Olivier , Inami Hanae , Kocevski Dale D. , Koekemoer Anton M. , Lemaux Brian C. , Mantha Kameswara Bharadwaj , Marchesi Stefano , Martig Marie , Masters Daniel C. , McGrath Elizabeth J. , McIntosh Daniel H. , Moreno Jorge , Nayyeri Hooshang , Pampliega Belen Alcalde , Salvato Mara , Snyder Gregory F. , Straughn Amber N. , Treister Ezequiel , Weston Madalyn E. 
Published: November 2020

Abstract
Galaxy interactions and mergers are thought to play an important role in the evolution of galaxies. Studies in the nearby universe show a higher fraction of active galactic nuclei (AGNs) in interacting and merging galaxies than in their isolated counterparts, indicating that such interactions are important contributors to black hole growth. To investigate the evolution of this role at higher redshifts, we have compiled the largest known sample of major spectroscopic galaxy pairs (2381 with ΔV < 5000 km s−1) at 0.5 < z < 3.0 from observations in the COSMOS and CANDELS surveys. We identify X-ray and IR AGNs among this kinematic pair sample, a visually identified sample of mergers and interactions, and a mass-, redshift-, and environment-matched control sample for each in order to calculate AGN fractions and the level of AGN enhancement as a function of relative velocity, redshift, and X-ray luminosity. While we see a slight increase in AGN fraction with decreasing projected separation, overall, we find no significant enhancement relative to the control sample at any separation. In the closest projected separation bin (< 25 kpc, ΔV < 1000 km s−1), we find enhancements of a factor of

and

for X-ray and IR-selected AGNs, respectively. While we conclude that galaxy interactions do not significantly enhance AGN activity on average over 0.5 < z < 3.0 at these separations, given the errors and the small sample size at the closest projected separations, our results would be consistent with the presence of low-level AGN enhancement.
Pre-main-sequence Stars in Taurus: Comparison of Magnetic and Nonmagnetic Model Fits to the Low-mass Stars
Authors: Mullan D. J. , MacDonald J. 
Published: November 2020

Abstract
Stellar associations should be co-eval, but some associations exhibit apparently discrepant ages: M stars appear younger than FG stars. Among M stars in the Upper Sco association (age ≈ 11 Myr), magnetic effects have been shown to slow down evolution of the lowest mass stars, thereby alleviating the age discrepancy. A recent study of pre-main-sequence (PMS) stars in the much younger Taurus star-forming region (SFR) suggest that an age discrepancy may also exist there. Our goal is to compare two approaches to magnetic/nonmagnetic modeling of the Taurus stars. In one approach, Simon et al. concluded that an age discrepancy exists, but it can be resolved by magnetic models if one imposes an “equipartition condition” on the photospheric field of each star. In this paper, we examine an independent sample of seven Taurus PMS stars reported by Rizzuto et al. Our approach to modeling magneto-convection imposes no condition on the photospheric field strength. We find that nonmagnetic isochrones can successfully fit the stars in the Rizzuto et al. sample with ages 1.6–2.4 Myr, without the need to invoke magnetic effects. An upper limit on the vertical field strength on the surfaces of the Rizzuto stars is found to be ∼300 G for the low-mass secondaries of FF Tau and HP Tau/G2 and ∼100 G for the other, more massive stars. The Taurus SFR is so large (extending over many square degrees in the sky) that magnetic conditions may plausibly differ from star to star.