bluuebunny/crossref_metadata_2025_split huggingface dataset:
Fe vii Emission Lines in the Wavelength Range 193–197 Å
Authors: Young Peter R. , Ryabtsev Alexander N. , Landi Enrico 
Published: February 2021

Abstract
The identifications of Fe vii emission lines in the wavelength range 193–197 Å are discussed in the light of new measurements of laboratory spectra and atomic data calculations. This region is of importance to studies of solar spectra from the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft, which has its peak sensitivity at these wavelengths. Ten lines are measured, arising from seven fine structure levels in the 3p
53d
3 configuration. Two lines have not previously been reported and lead to new experimental energies for the

levels. Updated experimental energies are obtained for the remaining levels. The new atomic model is used to compute theoretical values for the two density diagnostic ratios λ196.21/λ195.39 and λ196.21/λ196.06, and densities are derived from EIS spectra of coronal loop footpoints.
Optimized Statistical Approach for Comparing Multi-messenger Neutron Star Data
Authors: Raithel Carolyn A. , Özel Feryal , Psaltis Dimitrios 
Published: February 2021

Abstract
The neutron star equation of state is now being constrained from a diverse set of multi-messenger data, including gravitational waves from binary neutron star mergers, X-ray observations of the neutron star radius, and many types of laboratory nuclear experiments. These measurements are often mapped to a common domain for comparison with one another or are used to constrain the predictions of theoretical equations of state. We explore here the statistical biases that can arise when such multi-messenger data are compared or combined across different domains. We find that placing Bayesian priors individually in each domain of measurement can lead to biased constraints. We present a new prescription for defining Bayesian priors consistently across different experiments, which will allow for robust cross-domain comparisons. Using the first two binary neutron star mergers as an example, we show that a uniform prior in the tidal deformability can produce inflated evidence for large radii, while a uniform prior in the radius points toward smaller radii. Finally, using this new prescription, we provide a status update on multi-messenger constraints on the neutron star radius.
Updated BaSTI Stellar Evolution Models and Isochrones. II. α-enhanced Calculations
Authors: Pietrinferni Adriano , Hidalgo Sebastian , Cassisi Santi , Salaris Maurizio , Savino Alessandro , Mucciarelli Alessio , Verma Kuldeep , Aguirre Victor Silva , Aparicio Antonio , Ferguson Jason W. 
Published: February 2021

Abstract
This is the second paper of a series devoted to presenting an updated release of the BaSTI (a Bag of Stellar Tracks and Isochrones) stellar model and isochrone library. Following the publication of the updated solar-scaled library, here we present the library for an α-enhanced heavy element distribution. These new α-enhanced models account for all improvements and updates in the reference solar metal distribution and physics inputs, as in the new solar-scaled library. The models cover a mass range between 0.1 and 15 M
⊙, 18 metallicities between [Fe/H] = −3.20 and +0.06 with [α/Fe] = +0.4, and a He-to-metal enrichment ratio ΔY/ΔZ = 1.31. For each metallicity, He-enhanced stellar models are also provided. The isochrones cover (typically) an age range between 20 Myr and 14.5 Gyr, including consistently the pre-main-sequence phase. The asteroseismic properties of the theoretical models have also been calculated. Models and isochrones have been compared with results from independent calculations, with the previous BaSTI release, and also with selected observations, to test the accuracy/reliability of these new calculations. All stellar evolution tracks, asteroseismic properties, and isochrones are publicly available at http://basti-iac.oa-teramo.inaf.it.
A Comparison of Star-forming Clumps and Tidal Tails in Local Mergers and High-redshift Galaxies
Authors: Elmegreen Debra Meloy , Elmegreen Bruce G. , Whitmore Bradley C. , Chandar Rupali , Calzetti Daniela , Lee Janice C. , White Richard , Cook David , Ubeda Leonardo , Mok Angus , Linden Sean T. 
Published: February 2021

Abstract
The Clusters, Clumps, Dust, and Gas in Extreme Star-forming Galaxies (CCDG) survey with the Hubble Space Telescope includes multiwavelength imaging of 13 galaxies less than 100 Mpc away, spanning a range of morphologies and sizes, from blue compact dwarfs to luminous infrared galaxies, all with star formation rates in excess of hundreds of solar masses per year. Images of seven merging galaxies in the CCDG survey were artificially redshifted to compare with galaxies at z = 0.5, 1, and 2. Most redshifted tails have surface brightnesses that would be visible at z = 0.5 or 1 but not at z = 2 due to cosmological dimming. Giant star clumps are apparent in these galaxies; the 51 measured have similar sizes, masses, and colors to clumps in observed high-z systems in the UDF, GEMS, GOODS, and CANDELS surveys. These results suggest that some clumpy high-z galaxies without observable tidal features could be the result of mergers. The local clumps also have the same star formation rate per unit area and stellar surface density as clumps observed at intermediate and high redshift, so they provide insight into the substructure of distant clumps. A total of 1596 star clusters brighter than M

V
= −9 were identified within the boundaries of the local clumps. The cluster magnitude distribution function is a power law with approximately the same slope (∼−1 for a plot of number versus log luminosity) for all the galaxies both inside and outside the clumps and independently of clump surface brightness.
Carbon Chain Chemistry in Hot-core Regions around Three Massive Young Stellar Objects Associated with 6.7 GHz Methanol Masers
Authors: Taniguchi Kotomi , Herbst Eric , Majumdar Liton , Caselli Paola , Tan Jonathan C. , Li Zhi-Yun , Shimoikura Tomomi , Dobashi Kazuhito , Nakamura Fumitaka , Saito Masao 
Published: February 2021

Abstract
We have carried out observations of CCH (N = 1 − 0), CH3CN (J = 5 − 4), and three 13C isotopologues of HC3N (J = 10 − 9) toward three massive young stellar objects (MYSOs), G12.89+0.49, G16.86−2.16, and G28.28−0.36, with the Nobeyama 45 m radio telescope. Combined with previous results on HC5N, the column density ratios of N(CCH)/N(HC5N), hereafter the CCH/HC5N ratios, in the MYSOs are derived to be ∼15. This value is lower than that in a low-mass warm carbon chain chemistry (WCCC) source by more than one order of magnitude. We compare the observed CCH/HC5N ratios with hot-core model calculations. The observed ratios in the MYSOs can be best reproduced by models when the gas temperature is ∼85 K, which is higher than in L1527, a low-mass WCCC source (∼35 K). These results suggest that carbon-chain molecules detected around the MYSOs exist at least partially in higher temperature regions than those in low-mass WCCC sources. There is no significant difference in column density among the three 13C isotopologues of HC3N in G12.89+0.49 and G16.86-2.16, while HCC13CN is more abundant than the others in G28.28–0.36. We discuss carbon-chain chemistry around the three MYSOs based on the CCH/HC5N ratio and the 13C isotopic fractionation of HC3N.
Maps of Magnetic Field Strength in the OMC-1 Using HAWC+ FIR Polarimetric Data
Authors: Guerra Jordan A. , Chuss David T. , Dowell C. Darren , Houde Martin , Michail Joseph M. , Siah Javad , Wollack Edward J. 
Published: February 2021

Abstract
Far-infrared dust polarimetry enables the study of interstellar magnetic fields via tracing of the polarized emission from dust grains that are partially aligned with the direction of the field. The advent of high-quality polarimetric data has permitted the use of statistical methods to extract both the direction and magnitude of the magnetic field. In this work, the Davis–Chandrasekhar–Fermi technique is used to make maps of the plane-of-sky (POS) component of the magnetic field in the Orion Molecular Cloud (OMC-1) by combining polarization maps at 53, 89, 154 and 214 μm from HAWC+/SOFIA with maps of density and velocity dispersion. In addition, maps of the local dispersion of polarization angles are used in conjunction with Zeeman measurements to estimate a map of the strength of the line-of-sight (LOS) component of the field. Combining these maps, information about the three-dimensional magnetic field configuration (integrated along the LOS) is inferred over the OMC-1 region. POS magnetic field strengths of up to 2 mG are observed near the BN/KL object, while the OMC-1 bar shows strengths of up to a few hundred μG. These estimates of the magnetic field components are used to produce maps of the mass-to-magnetic-flux ratio (M/Φ)—a metric for probing the conditions for star formation in molecular clouds—and determine regions of sub- and supercriticality in OMC-1. Such maps can provide invaluable input and comparison to MHD simulations of star formation processes in filamentary structures of molecular clouds.
Large-scale Variation in Reionization History Caused by Baryon–Dark Matter Streaming Velocity
Authors: Park 박 Hyunbae 현 배 , Shapiro Paul R. , Ahn Kyungjin , Yoshida Naoki , Hirano Shingo 
Published: February 2021

Abstract
At cosmic recombination, there was supersonic relative motion between baryons and dark matter, which originated from baryonic acoustic oscillations in the early universe. This motion has been considered to have a negligible impact on the late stage of cosmic reionization because the relative velocity quickly decreases. However, recent studies have suggested that the recombination in gas clouds smaller than the local Jeans mass (≲108
M
☉) can affect the reionization history by boosting the number of ultraviolet photons required for ionizing the intergalactic medium. Motivated by this, we performed a series of radiation-hydrodynamic simulations to investigate whether the streaming motion can generate variation in the local reionization history by smoothing out clumpy small-scale structures and lowering the ionizing photon budget. We found that the streaming velocity can add a variation of Δz

e
∼ 0.05–0.5 in the end-of-reionization redshift, depending on the level of X-ray preheating and the time evolution of ionizing sources. The variation tends to be larger when the ionizing efficiency of galaxies decreases toward later times. Given the long spatial fluctuation scales of the streaming motion (≳100 Mpc), it can help to explain the Lyα opacity variation observed from quasars and leave large-scale imprints on the ionization field of the intergalactic medium during the reionization. The pre-reionization heating by X-ray sources is another critical factor that can suppress small-scale gas clumping and can diminish the variation in z

e
introduced by the streaming motion.
Wind Mass-loss Rates of Stripped Stars Inferred from Cygnus X-1
Authors: Neijssel Coenraad J. , Vinciguerra Serena , Vigna-Gómez Alejandro , Hirai Ryosuke , Miller-Jones James C. A. , Bahramian Arash , Maccarone Thomas J. , Mandel Ilya 
Published: February 2021

Abstract
Recent observations of the high-mass X-ray binary Cygnus X-1 have shown that both the companion star (41 solar masses) and the black hole (21 solar masses) are more massive than previously estimated. Furthermore, the black hole appears to be nearly maximally spinning. Here, we present a possible formation channel for the Cygnus X-1 system that matches the observed system properties. In this formation channel, we find that the orbital parameters of Cygnus X-1, combined with the observed metallicity of the companion, imply a significant reduction in mass loss through winds relative to commonly used prescriptions for stripped stars.
A Smoking Gun for Planetesimal Formation: Charge-driven Growth into a New Size Range
Authors: Teiser Jens , Kruss Maximilian , Jungmann Felix , Wurm Gerhard 
Published: February 2021

Abstract
Collisions electrically charge grains, which promotes growth by coagulation. We present aggregation experiments with three large ensembles of basalt beads (150–180 μm), two of which are charged, while one remains almost neutral as a control system. In microgravity experiments, free collisions within these samples are induced with moderate collision velocities (0–0.2 m s−1). In the control system, coagulation stops at (sub-)mm size while the charged grains continue to grow. A maximum agglomerate size of 5 cm is reached, limited only by bead depletion in the free volume. For the first time, charge-driven growth well into the centimeter range is directly proven by experiments. In protoplanetary disks, this agglomerate size is well beyond the critical size needed for hydrodynamic particle concentration as, e.g., by the streaming instabilities.
Late-time Observations of Calcium-rich Transient SN 2019ehk Reveal a Pure Radioactive Decay Power Source
Authors: Jacobson-Galán Wynn V. , Margutti Raffaella , Kilpatrick Charles D. , Raymond John , Berger Edo , Blanchard Peter K. , Bobrick Alexey , Foley Ryan J. , Gomez Sebastian , Hosseinzadeh Griffin , Milisavljevic Danny , Perets Hagai , Terreran Giacomo , Zenati Yossef 
Published: February 2021

Abstract
We present multiband Hubble Space Telescope imaging of the calcium-rich supernova (SN) SN 2019ehk at 276-389 days after explosion. These observations represent the latest B-band to near-IR photometric measurements of a calcium-rich transient to date and allow for the first opportunity to analyze the late-time bolometric evolution of an object in this observational SN class. We find that the late-time bolometric light curve of SN 2019ehk can be described predominantly through the radioactive decay of 56Co for which we derive a mass of M(56Co) = (2.8 ± 0.1) × 10−2
M
⊙. Furthermore, the rate of decline in bolometric luminosity requires the leakage of γ-rays on timescale t

γ
= 53.9 ± 1.30 days, but we find no statistical evidence for incomplete positron trapping in the SN ejecta. While our observations cannot constrain the exact masses of other radioactive isotopes synthesized in SN 2019ehk, we estimate a mass ratio limit of M(57Co)/M(56Co) ≤ 0.030. This limit is consistent with the explosive nucleosynthesis produced in the merger of low-mass white dwarfs, which is one of the favored progenitor scenarios in early-time studies of SN 2019ehk.
Constraint on
G˙/G
from Orbital Timing
Authors: Gupta Rajendra P. 
Published: February 2021

Abstract
Constraints on the variation of the gravitational constant G have been obtained by many observers using different methods, the most reliable and stringent being those based on the orbital timing of bodies in the solar system and binary pulsars. We show that the constraints determined from orbital timing are on

G

˙

/

G
−
3

c

˙

/

c

rather than on

G

˙

/

G

when the speed of light c is also considered to be varying. Increasingly tighter constraint on

G

˙

/

G

from these observations are possibly due to

G

˙

/

G
−
3

c

˙

/

c
=
0

. This relationship between G and c was determined in a previous work by fitting the supernovae 1a data using the relativistically covariant cosmological model with varying

c
,
G

and cosmological constant Λ.
Transient Terrestrial Trojans: Comparative Short-term Dynamical Evolution of 2010 TK7 and 2020 XL5
Authors: de la Fuente Marcos Carlos , de la Fuente Marcos Raúl 
Published: February 2021

Abstract
The Trojan asteroids of Mars and Jupiter are long-term stable, those of Earth are expected to be just transient companions. The first Trojan of our planet, 2010 TK7, was discovered in 2010 and its resonant state was found to be transient. Here, we provide a preliminary assessment of the current dynamical status and short-term orbital evolution of 2020 XL5, a recently discovered near-Earth asteroid that might be the second known representative of this elusive population. Our calculations show that the current orbit determination of 2010 TK7 is consistent with that of a robust, present-day, yet transient, L4 Earth Trojan. In sharp contrast, the current orbit determination of 2020 XL5 is still too uncertain and its orbital evolution too chaotic to confirm a current Trojan engagement with Earth, although the nominal orbit shows such a behavior. More observations are required to provide a conclusive answer.
1918-1920 YILLARINDA KARABAĞ’DA ERMENİ İSYANLARI: AZERBAYCAN HÜKÜMETİ’NİN TOPRAK BÜTÜNLÜĞÜNÜ SAĞLAMAK İÇİN İSYANCILARA KARŞI MÜCADELESİ
Authors: SADIGOV Ramin 
Published: February 2021

XIX. yüzyılda Çarlık Rusya tarafından Karabağ’a iskân edildikten sonra bölgede yaşayan Azerbaycan halkına karşı sistematik bir şekilde baskı, tehdit ve vahşet uygulayan Ermeniler, Mayıs 1918’de kurulan Azerbaycan Cumhuriyeti Hükümeti’ne de tabi olmak istemediler. Nitekim 23 aylık varlığı süresince Cumhuriyet Hükümeti’ne karşı isyan ederek Karabağ’da önce kendi yönetimlerini kurmaya, sonra da bölgeyi Ermenistan’a birleştirmeye çalıştılar. Lakin Azerbaycan Hükümeti hem Ermenistan’dan hem de silahlı çete gruplardan destek alan Karabağ’da yaşayan Ermenilere fırsat vermedi ve tüm ülke sathında toprak bütünlüğünü sağlamayı başardı.
Yüz yıldan fazla bir süredir Karabağ’da hak talep eden Ermenilerin, 1918-1920 yıllarında Azerbaycan Hükümeti’ne karşı yaptığı isyanlar, bu çalışmanın konusunu oluşturmaktadır. Çalışmanın özgünlüğü de konunun, dönemin kaynaklarına dayanarak araştırılmış olmasıdır. Haliyle çalışmada, 1918-1920 yıllarında Karabağ’da Ermenilerin isyanları, büyük devletlerin Karabağ konusundaki yaklaşımları ve Azerbaycan Hükümeti’nin isyancılara karşı mücadelesi ayrıntılı bir şekilde irdelenmiştir.
Kontribusi Persewaan Tanaman Hias terhadap Pendapatan Produsen Tanaman Hias di Kota Malang dan Sekitarnya
Authors: Hanoum Farah Chalida 
Published: February 2021

This research aims to obtain an overview of rentals characteristic business ornamental plant of the scale of households and small scales and knowing the contribution rentals ornamental plant of the scale of households and small scales against income producers ornamental plants. The determination of the location of the research done deliberately (purposive) that is implemented in the city of Malang and Batu city with the consideration that location is an ornamental plant production center to continuously ornamental plants rental. Methods of data retrieval method using Census data, the analysis carried out qualitatively and quantitatively. The result of qualitative analysis : First , in the matter of pricing, where the scale of ornamental plants rental households, no price on the basis of plants, but based on the sized manufacturing, while on a small scale in addition to rental based on size is also based on the type of plants. Second, the targert market or tenant. Where on a small scale, ornamental plants rental market target is broader this is due to the partnership business, based on the result, the contribution of revenue each tenancy. The contribution rental income an ornamental against producers an ornamental received household scale of 33,26 percent. While on small scale of 22,90 percent.
Jaringan Syaraf Tiruan Untuk Memprediksi Penjualan Pakaian Menggunakan Algoritma Backpropagation
Authors: Mubarokh M. Fadhil , Nasir Muhammad , Komalasari Dinny 
Published: February 2021

Penilitian ini memprediksi penjualan pakaian yang terdiri dari penjualan Gamis dan penjualan Jilbab yang terdapat pada Toko Sumber Busana Palembang dengan menggunakan metode Jaringan Syaraf Tiruan. Jaringan Syaraf Tiruan merupakan salah satu representasi buatan dari otak manusia yang selalu mencoba untuk mensimulasikan proses pembelajaran otak manusia. Untuk saat ini persaingan penjualan pakain semakin ketat diiringi dengan meningkatnya tingkat ekonomi masyarakat. Market share atau prediksi penjualan, merupakan suatu bentuk acuan tiap perusahaan untuk mendapatkan hasil yang optimalPenerapannya menggunakan algoritma Backpropagation dimana suatu data yang diinputkan Jumlah Terjual, Pemasukkan, Pengeluaran, dan saldo sebagai data target. Kemudian dibentuk suatu Jaringan Syaraf Tiruan dengan menentukan jumlah unit dalam setiap lapisan. Setelah Jaringan terbentuk dilakukan training dari data yang sudah dikelompokkan tersebut. Percobaan itu dilakukan dengan arsitektur jaringan yang terdiri dari unit masukan , unit tersembunyi, unit keluaran, dan arsitektur jaringan 3-3-1. Pengujian dalam penelitian ini dilakukan dengan perangkat lunak Matlab
Analisis Perilaku Malware Dengan Metode Surface Analysis Dan Runtime Analysis
Authors: Siddiq Ahmad , Yudiastuti Helda , Panjaitan Febriyanti 
Published: February 2021

Saat ini penggunaan komputer sudah menjadi hal yang biasa baik oleh pegawai, mahasiswa dan anak-anak sekolah. Umumnya sistem operasi yang digunakan adalah Windows, oleh karena kemudahan, namun hal ini juga memberikan peluang bagi orang-orang yang memiliki niat buruk untuk mengambil keuntungan secara ilegal dengan berbagai macam cara, salah satunya dengan membuat sebuah Malware yang disusupkan dalam sebuah program atau dengan cara-cara lainnya. Berdasarkan hal tersebut penulis ingin meneliti perilaku apa saja yang dilakukan oleh Malware ketika menyerang sebuah system operasi khususnya Windows menggunakan metode Surface Analysis dan Runtime Analysis untuk. Dengan menggunkan metode ini, informasi yang didapat berupa jenis file asli yang di periksa, ukuran file sebenarnya dan melihat apakah ada file lain di dalam file yang di periksa. Dari pemeriksaan menggunakan metode ini juga didapatkan hash function atau MD5 yang merupakan identitas unik dari file yang di periksa serta dapat memeriksa secara keseluruhan seperti proses yang berjalan di komputer, dan peristiwa janggal lainnya yang biasa terjadi saat komputer terinfeksi Malware. Sehingga nantinya dapat diklasifikasikan kedalam Malware jenis apa
Reviews and syntheses: The biogeochemical cycle of silicon in the modern ocean
Authors: Tréguer Paul J. , Sutton Jill N. , Brzezinski Mark , Charette Matthew A. , Devries Timothy , Dutkiewicz Stephanie , Ehlert Claudia , Hawkings Jon , Leynaert Aude , Liu Su Mei , Llopis Monferrer Natalia , López-Acosta María , Maldonado Manuel , Rahman Shaily , Ran Lihua , Rouxel Olivier 
Published: February 2021

Abstract. The element silicon (Si) is required for the growth of silicified organisms in marine environments, such as diatoms. These organisms consume vast amounts of Si together with N, P, and C, connecting the biogeochemical cycles of these elements. Thus, understanding the Si cycle in the ocean is critical for understanding wider issues such as carbon sequestration by the ocean's biological pump. In this review, we show that recent advances in process studies indicate that total Si inputs and outputs, to and from the world ocean, are 57 % and 37 % higher, respectively, than previous estimates. We also update the total ocean silicic acid inventory value, which is about 24 % higher than previously estimated. These changes are significant, modifying factors such as the geochemical residence time of Si, which is now about 8000 years, 2 times faster than previously assumed. In addition, we present an updated value of the global annual pelagic biogenic silica production (255 Tmol Si yr−1) based on new data from 49 field studies and 18 model outputs, and we provide a first estimate of the global annual benthic biogenic silica production due to sponges (6 Tmol Si yr−1). Given these important modifications, we hypothesize that the modern ocean Si cycle is at approximately steady state with inputs =14.8(±2.6) Tmol Si yr−1 and outputs =15.6(±2.4) Tmol Si yr−1. Potential impacts of global change on the marine Si cycle are discussed.