bluuebunny/crossref_metadata_2025_split huggingface dataset:
ANALISIS STRATEGI BERSAING DAN STRATEGI BERTAHAN PADA INDUSTRI MIKRO DAN KECIL PANGANAN KERIPIK KEMASAN DI KECAMATAN COBLONG KOTA BANDUNG JAWA BARAT TAHUN 2020 DITENGAH SITUASI SULIT PENYEBARAN PANDEMI nCoV-19
Authors: Yanto Arief , Sukanta Tuntun 
Published: May 2020

Penelitian ini bertujuan untuk mengetahui dan menganalisis strategi bersaing dan strategi bertahan pada usaha mikro dan kecil panganan keripik kemasan di kecamatan coblong, Kota Bandung tahun 2020. Data yang digunakan merupakan data primer dan sekunder. Data primer diperoleh dari hasil survei lapangan dan wawancara, sedangkan data sekunder dari lembaga atau instansi terkait seperti Dinas Perindustrian dan Perdagangan, Badan Pusat Statistik serta Paguyuban ABDSI Korwil Jabar yang berada di sentra industri Panganan Keripik Kemasan. Alat analisis yang digunakan untuk strategi bersaing adalah dengan Teori Lima Kekuatan Persaingan dari Porter (1980). Sedangkan untuk analisis deskriptif digunakan untuk menganalisis strategi bertahan pada usaha mikro dan kecil produsen Panganan Keripik Kemasan. Berdasarkan pendekatan metode Lima Kekuatan Persaingan dari Porter (1980), produsen keripik mampu bersaing dengan harga, pengembangan produk, promosi, dan distribusi produk. Strategi Bertahan produsen Panganan Keripik Kemasan adalah dengan adanya model dari porter dari strategi bersaing, produsen mampu bertahan dari persaingan antar produsen keripik yang lebih besar karena strategi bertahan yang digunakan oleh produsen yaitu harga yang terjangkau bagi para konsumen.
24-Hour Proteinuria Weakly Correlated with Estimated Glomerular Filtration Rate in Lupus Nephritis Patients
Authors: Praptama Suhendra , Aini Yulia Hayatul , Ghozali Mohammad , Hamijoyo Laniyati 
Published: May 2020

Background: Lupus Nephritis (LN) is still the most frequent complication in Systemic Lupus Erythematous (SLE) patients which causing the major and significance morbidity and mortality. Proteinuria and Glomerular Filtration Rate (GFR) serves as objective and routine examinations to assessrenal function. 24-hour proteinuria still regarded as gold standard to quantify amount protein in urine. Estimated GFR (eGFR) is preferably used due its convenient. On the hand, estimated GFR (eGFR) is preferably used due its convenient. However, both of them should be measured in order to determine renal progression and prognosis. Only few studies have been conducted to find out the correlation between 24-hour proteinuria and eGFR in lupus nephritis patients as both of them serve as potential marker in progression of renal involvement. Thisstudy addressed to find out correlation between 24-hour proteinuria and eGFR in lupus nephritis patients.Method: Analytic-correlation study with cross-sectional approach at Dr. Hasan Sadikin Hospital, Bandung was done. Secondary data was used and paralleled with previous study entitled “Correlation of Random Urine Protein Creatinine (P-C) Ratio with 24-Hour Protein Urinein Lupus Nephritis Patients” carried out from October to December 2014.Correlation coefficient was analyzed by Spearmans’ correlation test.Results: Forty five samples were obtained based on inclusion criteria. Spearmans’ correlation test revealed non significant and very weak correlation between 24-hour proteinuria and eGFR (r=-0.095) with p>0.05.Conclusion: The 24-hour proteinuria and eGFR are weakly correlated. Despite the weak correlation, these examinationsshould be considered as important markers to monitor prognosis of renal involvement in lupus nephritis patients Keywords: Estimated glomerular filtration rate (eGFR),Lupus Nephritis (LN), Proteinuria, Systemic Lupus Erythematosus (SLE).
Pembangunan Aplikasi Pengukur Ketinggian Benda Berbasis Android dengan Menggunakan Metode Trigonometri
Authors: Mauluddin Amras , Supriadi Irwin 
Published: May 2020

Saat ini kita mengenal dua cara untuk mengukur ketinggian benda. Cara pertama adalah menggunakan busur dan tape measure. Busur digunakan untuk menghitung besar sudut, kemudian tape measure digunakan untuk menghitung jarak antara titik sudut dan benda yang diukur. Sedangkan cara yang kedua adalah menggunakan alat yang disebut dengan thedolit. Hasil pengukuran dengan cara kedua ini lebih akurat dibandingkan dengan cara pertama. Hal ini dikarenakan thedolit memiliki tingkat ketelitian yang baik. Namun kedua cara pengukuran tersubut memiliki beberapa kelemahan, yakni cara pertama memerlukan ketelitian yang cermat saat menghitung sudut dan cara yang kedua memiliki kelemahan dalam hal biaya.
Untuk dapat menutupi kelemahan tersebut, maka dibuatlah sebuah Aplikasi pengukur ketinggian berbasis android. Penggunaan aplikasi ini cukup sederhana dan tidak memerlukan biaya. Sehingga diharapkan Aplikasi ini dapat menjadi solusi yang lebih efektif dan efisien.
Aplikasi pengukur ketinggian benda ini penulis namakan dengan Simple Measure. Perangkat ini dibangun dengan menggunakan bahasa pemograman JAVA. Metode pengukuran yang digunakan adalah trigonometri. Selain itu juga SensorFusion digunakan sebagai library untuk mendeteksi sudut kemiringan.
Sistem Informasi Geografi Daerah Potensi Kekeringan Menggunakan Fuzzy Inferensi Sistem
Authors: Chairuddin  , Nurafni Sevi 
Published: May 2020

Kekeringan merupakan salah satu bencana alam yang frekuensi kejadiannya tinggi (hampir setiap tahun). Daerah potensi kekeringan perlu diprediksi agar dapat mengurangi kerugian-kerugian yang tidak hanya pada sektor pertanian dan lingkungan hidup tetapi juga berdampak negatif pada sektor sosial dan ekonomi bahkan dapat mengganggu stabilitas politik.
Dalam pengolahan peta digital untuk sistem informasi geografis (SIG), seringkali ditemukan objek-objek penting yang tidak tepat dalam pengolahannya bahkan tidak dapat dilibatkan karena faktor ketidakpastian yang dimiliki oleh objek tersebut. Objek yang memiliki ketidakpastian berhubungan dengan data yang tidak dapat dinyatakan hanya dalam dua kondisi saja, yaitu kondisi ”ya” atau kondisi ”tidak”. Salah satu solusi yang ditawarkan dalam mengatasi keterlibatan objek yang memiliki ketidakpastian di dalam SIG adalah dengan menggunakan sistem inferensi fuzzy (SIF) metode Tsukamoto. Data yang memiliki ketidakpastian yang diangkat dalam penelitian ini adalah data non-spasial berupa faktor-faktor penentu daerah potensi kekeringan pada wilayah Nusa Tenggara Timur
Sistem infrensi fuzzy dapat dijadikan sebagai salah satu solusi dalam pembuatan peta digital yang melibatkan sejumlah data yang bersifat tidak pasti. Output yang diharapkan dari penelitian ini adalah peta yang memberikan informasi tentang daerah rawan demam berdarah berdasarkan warna yang ditentukan dengan nilai yang diperoleh dari proses inferensi fuzzy.
Machine Learning Diagnosis Kanker Payudara Menggunakan Algoritma Support Vector Machine
Authors: Chazar Chalifa , Erawan Bagus 
Published: May 2020

Kanker payudara merupakan penyebab kematian nomor dua pada wanita. Penyakit ini sulit dideteksi pada fase awal. Akan tetapi, kebanyakan penderita baru mengetahui kondisinya setelah memasuki fase tertentu dalam kondisi yang parah dan sulit disembuhkan. Salah satu bentuk pemeriksaan untuk mendiagnosis penyakit kanker payudara adalah dengan melakukan biopsi. Biopsi adalah teknik pemeriksaan yang dilakukan dengan mengambil cairan di payudara menggunakan Fine Needle Aspiration (FNA), selanjutnya hasil biopsi FNA akan diperiksa lagi di laboratorium untuk mendapatkan hasil diagnosis. Untuk mendapatkan hasil yang akurat dari proses biopsi dibutuhkan waktu yang lama. Machine Learning (ML) dapat digunakan untuk mencari dan menemukan pola yang unik dari sekumpulan data. Algoritma Support Vector Machine (SVM) dipilih karena algoritma ini mampu mengklasifikasikan nilai ke dalam kelas-kelas tertentu. Algoritma SVM juga memiliki tingkat akurasi yang lebih tinggi dibandingkan dengan algoritma lainnya. Penelitian ini bertujuan untuk membangun aplikasi ML yang dapat mendiagnosis penyakit kanker payudara dengan menggunakan Algoritma SVM untuk mencari pola data dari sekumpulan data masa lalu untuk menghasilkan hasil diagnosis yang akurat. Hasil dari penelitian ini menunjukan bahwa Algoritma SVM pada ML dapat digunkan untuk mencari suatu pola data dari sekumpulan data masa lalu yang dapat menghasilkan prediksi untuk menentukan sel hidup kanker payudara bersifat ganas atau jinak.
The Most Metal-poor Stars in Omega Centauri (NGC 5139)*
Authors: Johnson Christian I. , Dupree Andrea K. , Mateo Mario , Bailey John I. , Olszewski Edward W. , Walker Matthew G. 
Published: May 2020

Abstract
The most massive and complex globular clusters in the Galaxy are thought to have originated as the nuclear cores of now tidally disrupted dwarf galaxies, but the connection between globular clusters and dwarf galaxies is tenuous with the M54/Sagittarius system representing the only unambiguous link. The globular cluster Omega Centauri (ω Cen) is more massive and chemically diverse than M 54, and is thought to have been the nuclear star cluster of either the Sequoia or Gaia-Enceladus galaxy. Local Group dwarf galaxies with masses equivalent to these systems often host significant populations of very metal-poor stars ([Fe/H] < −2.5), and one might expect to find such objects in ω Cen. Using high-resolution spectra from Magellan-M2FS, we detected 11 stars in a targeted sample of 395 that have [Fe/H] ranging from −2.30 to −2.52. These are the most metal-poor stars discovered in the cluster, and are five times more metal-poor than ω Cen’s dominant population. However, these stars are not so metal-poor as to be unambiguously linked to a dwarf galaxy origin. The cluster’s metal-poor tail appears to contain two populations near [Fe/H] ∼ −2.1 and −2.4, which are very centrally concentrated but do not exhibit any peculiar kinematic signatures. Several possible origins for these stars are discussed.
Two Transiting Hot Jupiters from the WASP Survey: WASP-150b and WASP-176b
Authors: Cooke Benjamin F. , Pollacco Don , Almleaky Y. , Barkaoui K. , Benkhaldoun Z. , Blake James A. , Bouchy François , Boumis Panos , Brown D. J. A. , Bruni Ivan , Burdanov A. , Cameron Andrew Collier , Chote Paul , Daassou A. , D’ago Giuseppe , Dalal Shweta , Damasso Mario , Delrez L. , Doyle A. P. , Ducrot E. , Gillon M. , Hébrard G. , Hellier C. , Henning Thomas , Jehin E. , Kiefer Flavien , King George W. , Liakos Alexios , Lopez Théo , Mancini Luigi , Mardling Rosemary , Maxted P. F. L. , McCormac James , Murray C. , Nielsen Louise D. , Osborn Hugh , Palle E. , Pepe Francesco , Pozuelos F. J. , Prieto-Arranz J. , Queloz D. , Schanche Nicole , Ségransan Damien , Smalley Barry , Southworth John , Thompson S. , Turner Oliver , Udry Stéphane , Velasco S. , West Richard , Wheatley Pete , Alikakos John 
Published: May 2020

Abstract
We report the discovery of two transiting exoplanets from the WASP survey, WASP-150b and WASP-176b. WASP-150b is an eccentric (e = 0.38) hot Jupiter on a 5.6 day orbit around a V = 12.03, F8 main-sequence host. The host star has a mass and radius of 1.4

and 1.7

respectively. WASP-150b has a mass and radius of 8.5

and 1.1 R
J, leading to a large planetary bulk density of 6.4 ρ
J. WASP-150b is found to be ∼3 Gyr old, well below its circularization timescale, supporting the eccentric nature of the planet. WASP-176b is a hot Jupiter planet on a 3.9 day orbit around a V = 12.01, F9 sub-giant host. The host star has a mass and radius of 1.3 M
⊙ and 1.9 R
⊙. WASP-176b has a mass and radius of 0.86 M
J and 1.5 R
J, respectively, leading to a planetary bulk density of 0.23 ρ
J.
OGLE-2018-BLG-0677Lb: A Super-Earth Near the Galactic Bulge
Authors: Herrera-Martín Antonio , Albrow M. D. , Udalski A. , Gould A. , Ryu Y.-H. , Yee J. C. , Chung S.-J. , Han C. , Hwang K.-H. , Jung Y. K. , Lee C.-U. , Shin I.-G. , Shvartzvald Y. , Zang W. , Cha S.-M. , Kim D.-J. , Kim H.-W. , Kim S.-L. , Lee D.-J. , Lee Y. , Park B.-G. , Pogge R. W. ,   (KMTNet Collaboration), Szymański M. K. , Mróz P. , Skowron J. , Poleski R. , Soszyński I. , Kozłowski S. , Pietrukowicz P. , Ulaczyk K. , Rybicki K. , Iwanek P. , Wrona M. ,   (OGLE Collaboration)
Published: May 2020

Abstract
We report the analysis of the microlensing event OGLE-2018-BLG-0677. A small feature in the light curve of the event leads to the discovery that the lens is a star–planet system. Although there are two degenerate solutions that could not be distinguished for this event, both lead to a similar planet-host mass ratio. We perform a Bayesian analysis based on a Galactic model to obtain the properties of the system and find that the planet corresponds to a super-Earth/sub-Neptune with a mass of

. The host star has a mass of

. The projected separation for the inner and outer solutions are

au and

au respectively. At

, this is by far the lowest Δχ
2 for any securely detected microlensing planet to date, a feature that is closely connected to the fact that it is detected primarily via a “dip” rather than a “bump.”
A Method for the Estimation of f- and p-mode Parameters and Rotational Splitting Coefficients from Un-averaged Solar Oscillation Power Spectra
Authors: Reiter J. , Rhodes E. J. , Kosovichev A. G. , Scherrer P. H. , Larson T. P. , II S. F. Pinkerton 
Published: May 2020

Abstract
We present a new methodology for the fitting of the peaks in solar oscillation power spectra that is equally well-suited for the estimation of low-, medium, and high-degree f- and p-mode parameters and frequency-splitting coefficients. The method can provide accurate input data over a wide portion of the dispersion plane for both structural and rotational inversions. This method, which we call the Multiple-Peak, Tesseral-Spectrum (MPTS) method, operates directly upon of all of the modes in a multiplet (n, l) of radial order n and degree l, and employs a fitting profile that consists of the sum of numerous individual overlapping profiles whose relative amplitudes are determined by the leakage matrix appropriate to the targeted mode. Hence, 2l + 1 sets of modal parameters are obtained simultaneously for each multiplet (n, l). By fitting an appropriate polynomial to the run of the fitted frequencies versus the azimuthal order, frequency-splitting coefficients are also obtained for the same multiplet. Using power spectra obtained from the 66 day long 2010 MDI Dynamics Run, we present sample structural and rotational inversions that employed frequencies and frequency-splitting coefficients from modes in the degree range of 0–1000 and the frequency range of 965–4600 μHz. The structural inversion confirms evidence for a pronounced departure of the sound speed in the outer solar convection zone from the radial sound-speed profile contained in Model S of Christensen-Dalsgaard and his collaborators that we obtained previously using a different fitting method.
Using Transverse Waves to Probe the Plasma Conditions at the Base of the Solar Wind
Authors: Weberg Micah J. , Morton Richard J. , McLaughlin James A. 
Published: May 2020

Abstract
It has long been suggested that magnetohydrodynamic (MHD) waves may supply a significant proportion of the energy required to heat the corona and accelerate the solar wind. Depending on the properties of the local plasma, MHD wave modes may exhibit themselves as a variety of incompressible, transverse waves. The local magnetic field and particle density influence the properties of these waves (e.g., amplitude), thus direct measurements of transverse waves provide a mechanism to indirectly probe the local plasma conditions. We present the first statistical approach to magnetoseismology of a localized region of the solar corona, analyzing transverse waves above the south polar coronal hole on 2011 May 23. Automated methods are utilized to examine 4 hr of EUV imaging data to study how the waves evolve as a function of height (i.e., altitude) through the low corona. Between heights of 15 and 35 Mm, we find that the measured wave periods are approximately constant, and that observed displacement and velocity amplitudes increase at rates that are consistent with undamped waves. This enables us to derive a relative density profile for the coronal hole environment in question, without the use of spectroscopic data. Furthermore, our results indicate that between 5 and 15 Mm above the limb, the relative density is larger than that expected from 1D hydrostatic models, and signals a more extended transition region with a gradual change in density. This has implications for self-consistent models of wave propagation from the photosphere to the corona and beyond.
The Nature of Ultra-diffuse Galaxies in Distant Massive Galaxy Clusters: A370 in the Hubble Frontier Fields
Authors: Lee Jeong Hwan , Kang Jisu , Lee Myung Gyoon , Jang In Sung 
Published: May 2020

Abstract
We report the discovery of ultra-diffuse galaxies (UDGs) in Abell 370 (A370; z = 0.375). We find 46 UDGs in A370 from the images of the Hubble Frontier Fields. Most UDGs are low-luminosity red sequence galaxies, while a few of them are blue UDGs. We estimate the abundance of UDGs in A370, N(UDG) = 644 ± 104. Combining these results with those of Abell S1063 (z = 0.348) and Abell 2744 (z = 0.308), we derive a mean radial number density profile of UDGs in the three clusters. The number density profiles of UDGs and bright galaxies show a discrepancy in the central region of the clusters: the profile of UDGs shows a flattening as clustercentric distance decreases, while that of bright galaxies shows a continuous increase. This implies that UDGs are prone to disruption in the central region of the clusters. The relation between the abundance of UDGs and virial masses of their host systems is described by a power law with an index of nearly one:

for M
200 > 1013
M
⊙. We estimate approximately dynamical masses of UDGs using the fundamental manifold method and find that most UDGs have dwarf-like masses (M
200 < 1011
M
⊙). This implies that most UDGs have a dwarf-like origin and a small number of them could be failed L* galaxies. These results suggest that multiple origins may contribute to the formation and evolution of UDGs in massive galaxy clusters.
Three-dimensional Kinematic Reconstruction of the Optically Emitting, High-velocity, Oxygen-rich Ejecta of Supernova Remnant N132D
Authors: Law Charles J. , Milisavljevic Dan , Patnaude Daniel J. , Plucinsky Paul P. , Gladders Michael D. , Schmidt Judy , Sravan Niharika , Banovetz John , Sano Hidetoshi , McGraw Jordan M. , Takahashi George , Orlando Salvatore 
Published: May 2020

Abstract
We present a three-dimensional kinematic reconstruction of the optically emitting, oxygen-rich ejecta of supernova remnant N132D in the Large Magellanic Cloud (LMC). Data were obtained with the 6.5 m Magellan telescope in combination with the IMACS+GISMO instrument and survey [O iii] λλ4959, 5007 line emission in a ∼3′ × 3′ region centered on N132D. The spatial and spectral resolutions of our data enable detailed examination of the optical ejecta structure. The majority of N132D’s optically bright oxygen ejecta are arranged in a torus-like geometry tilted approximately 28° with respect to the plane of the sky. The torus has a radius of 4.4 pc (D
LMC/50 kpc), exhibits a blueshifted radial velocity asymmetry of −3000 to +2300 km s−1, and has a conspicuous break in its circumference. Assuming homologous expansion from the geometric center of O-rich filaments, the average expansion velocity of 1745 km s−1 translates to an age since explosion of 2450 ± 195 yr. A faint, spatially separated “runaway knot” (RK) with total space velocity of 3650 km s−1 is nearly perpendicular to the torus plane and coincident with X-ray emission that is substantially enhanced in Si relative to the LMC and N132D’s bulk ejecta. These kinematic and chemical signatures suggest that the RK may have had its origin deep within the progenitor star. Overall, the main-shell morphology and high-velocity, Si-enriched components of N132D have remarkable similarity with those of Cassiopeia A, which was the result of a Type IIb supernova explosion. Our results underscore the need for further observations and simulations that can robustly reconcile whether the observed morphology is dominated by explosion dynamics or shaped by interaction with the environment.
Inferring Vector Magnetic Fields from Stokes Profiles of GST/NIRIS Using a Convolutional Neural Network
Authors: Liu Hao , Xu Yan , Wang Jiasheng , Jing Ju , Liu Chang , Wang Jason T. L. , Wang Haimin 
Published: May 2020

Abstract
We propose a new machine-learning approach to Stokes inversion based on a convolutional neural network (CNN) and the Milne–Eddington (ME) method. The Stokes measurements used in this study were taken by the Near InfraRed Imaging Spectropolarimeter (NIRIS) on the 1.6 m Goode Solar Telescope (GST) at the Big Bear Solar Observatory. By learning the latent patterns in the training data prepared by the physics-based ME tool, the proposed CNN method is able to infer vector magnetic fields from the Stokes profiles of GST/NIRIS. Experimental results show that our CNN method produces smoother and cleaner magnetic maps than the widely used ME method. Furthermore, the CNN method is four to six times faster than the ME method and able to produce vector magnetic fields in nearly real time, which is essential to space weather forecasting. Specifically, it takes ∼50 s for the CNN method to process an image of 720 × 720 pixels comprising Stokes profiles of GST/NIRIS. Finally, the CNN-inferred results are highly correlated to the ME-calculated results and closer to the ME’s results with the Pearson product-moment correlation coefficient (PPMCC) being closer to 1, on average, than those from other machine-learning algorithms, such as multiple support vector regression and multilayer perceptrons (MLP). In particular, the CNN method outperforms the current best machine-learning method (MLP) by 2.6%, on average, in PPMCC according to our experimental study. Thus, the proposed physics-assisted deep learning–based CNN tool can be considered as an alternative, efficient method for Stokes inversion for high-resolution polarimetric observations obtained by GST/NIRIS.
Extended Calculations of Energy Levels and Transition Rates for Singly Ionized Lanthanide Elements. I. Pr–Gd
Authors: Radžiūtė Laima , Gaigalas Gediminas , Kato Daiji , Rynkun Pavel , Tanaka Masaomi 
Published: May 2020

Abstract
Lanthanide elements play important roles as an opacity source in the ejected material from neutron star mergers. Accurate and complete atomic data are necessary to evaluate the opacities and to analyze the observed data. In this paper, we perform extended, ab initio atomic calculations from Pr ii (Z = 59) to Gd ii (Z = 64). By using multiconfiguration Dirac–Hartree–Fock and relativistic configuration-interaction methods, implemented in the general-purpose relativistic atomic structure package (GRASP2K), we calculate the energy levels and transition data of electric dipole transitions. These computations are based on strategies (with small variations) of Nd ii published by Gaigalas et al. Accuracy of data is evaluated by comparing computed energy levels with the National Institute of Standards and Technology (NIST) database or other works. For the energy levels, we obtain the average relative accuracy of 8%, 12%, 6%, 8%, and 7% for Pr ii, Pm ii, Sm ii, Eu ii, and Gd ii ions, respectively, as compared with the NIST data. Accuracy of energy transfer to the wavelength is 3%, 14%, and 11% for Pr ii, Eu ii, and Gd ii. Our computed E1 type transition probabilities are in good agreement with experimental values presented by other authors especially for strong transitions.