bluuebunny/crossref_metadata_2025_split huggingface dataset:
Military expenditures in the Umayyad era (40-132 H / 660-749 AD)
Authors: Hamid Assist. prof. Dr. Wafa Adnan 
Published: March 2021

The military expenses in the Islamic Arabic state has been considered an important indicator that reflects the significance of the military system. Our current study aims to these military expenses in the era of Umayyad to specify the level of change in this institution from that level of Al-Rashidi era by bringing forth the changes that have been happened , besides placing terms for those who enter into the volume . This was prevailing over in the previous ages , but it was simple . It has been witnessed organizing volumes . The Umayyad state followed the rules placed by the caliphate " Omar Bin Al-Khatab" just like Sources of gifts from tributes and abscess and the surplus one placed in house of money; one should not take gift from charity. The distribution of the gift has been the reason for having the tribes of Levant ( Yemeni and Qaisi tribes)appear loyalty for Umayyad princes in return they will be given financial rewards and to be appointed in the jobs .IF the gift keeps on in Muharam Month (Islamic month) salaries to the soldiers will be paid since he lateness was causing problems for Umayyad caliphates . The heritage of gift remains applicable until the end of the Umayyad era , after it was applicable in Al-Rashidi era; besides , the Umayyad has organized and developed livings and established a special office for that. The booties in the era of Umayyad have got divided based on shares with the preference of the knight to the non-knight since the former has exerted efforts that will be explained in this current study.
Research on the Reproduction of Traditional Handicrafts During the Epidemic Period from the Perspective of Anthropology -- Taking Dongchang Carving Gourd as an example
Authors: Jia Yingcui 
Published: March 2021

As an excellent representative of traditional
handicrafts in West Shandong, Dongchang carving
gourd brings together economy and culture. It is not
only one of the important sources of rural social and
economic income under the background of traditional
farming, but also carries the essence of local culture.
In 2020, the COVID-19 epidemic suddenly emerged,
which seriously affected the foreign sales and cultural
activities of Liaocheng's traditional handicraft and
Dongchang carved gourd. Based on this, this paper,
from the perspective of anthropology, focuses on
the transformation of the local social structure
and cognitive mode during the epidemic period,
and on the theoretical basis of Bourdieu's tourism
reproduction theory, expounds the exploration and
practice of its reproduction. Finally, combining with
the current situation of the development demands
of traditional handicraft during the epidemic period,
the significance of its reproduction is discussed, so
that it can be continuously innovated, inherited and
developed as a folk handicraft.
Hubungan Indeks Massa Tubuh Terhadap Siklus Menstruasi Pada Mahasiswa AKBID Pelamonia Makassar Tahun 2020
Authors: Ruqaiyah Ruqaiyah 
Published: March 2021

Menstruasi adalah siklus alamiah setiap wanita, namun terdapat banyak kasus pada wanita terutama remaja yang mengalami siklus menstruasi tidak teratur. Ketidakteraturan siklus menstruasi dapat mengindikasikan adanya kelainan fungsi reproduksi. Tujuan dilakukannya penelitian ini adalah untuk mengetahui hubungan indeks massa tubuh terhadap siklus menstruasi pada mahasiswa AKBID Pelamonia Makassar tahun 2020. Penelitian ini menggunakan metode penelitian Cross Sectional Study dengan jumlah populasi sebanyak 450 orang dan jumlah sampel 107 orang dengan menggunakan teknik Accidental Sampling. Dari hasil uji statistic dengan menggunakan uji Chi-Square (Exact Fishert Test) diperoleh nilai ρ(0,000) <α(0,05), sehingga Ha di terima dan Ho ditolak, penelitian ini menunjukkan bahwa ada hubungan antara indeks massa tubuh terhadap siklus menstruasi. Kesimpulan dari variabel yaitu ada hubungan antara indeks massa tubuh terhadap siklus menstruasi pada mahasiswa AKBID Pelamonia Makassar. Sehingga diharapkan bagi mahasiswa yang memiliki IMT tidak normal seperti berat badan berlebih maupun obesitas agar dapat menerapkan pola hidup sehat dengan cara berolahraga secara teratur, memperbanyak aktivitas fisik serta mengurangi asupan kalori yang berlebih. Sedangkan untuk mahasiswa yang memiliki berat badan kurang agar menambah asupan kalori agar mencapai berat badan yang ideal.
Hubungan Pengetahuan Kesehatan Reproduksi Terhadap Perilaku Remaja Di Desa Bontomatene Kabupaten Maros Tahun 2020
Authors: Agusalim Agusalim , Nazihah Nurul 
Published: March 2021

Berdasarkan data yang didapatkan dari hasil penyebaran quisioner yang dilakukan di di Desa Bontomatene Kabupaten Maros RT 04 dan 05 didapatkan jumlah sampel sebanyak 42 responden pada bulan juni-agustus dengan jumlah populasi yaitu 42 orang. Tujuan dilakukannya penelitian ini adalah untuk mengetahui hubungan pengetahuan kesehatan reproduksi terhadap perilaku seks remaja di desa bontomatene kabupaten maros tahun 2020. Penelitian ini menggunakan metode penelitian analitik dengan melakukan pendekatan Cross Sectional Study untuk mengetahui dengan jumlah sampel yang diteliti dengan tujuan untuk mengetahui hubungan pengetahuan kesehatan reproduksi terhadap perilaku seks remaja di desa bontomatene kabupaten maros tahun 2020dengan jumlah populasi sebanyak 473 orang dan sampel sebanyak 4 2orang dengan menggunakan teknik Random Sampling. Dari hasil uji statistik dengan menggunakan uji Chi-Square (pearson chi-square) diperoleh nilai p = 0,041 < α = 0,05 maka Ho ditolak dan Ha diterima artinya ada hubungan antara pengetahuan kesehatan reproduksi terhadap perilaku seks remaja di Desa Bontomatene Maros tahun 2020. Kemudian diharapkan remaja mampu meningkatkan pengetahuan dengan banyak sharing akan pentingnya seks remaja di kalangan remaja dan mampu menjaga pergaulan agar tidak terjerumus kedalam pergaulan bebas.
Hubungan Dukungan Petugas Kesehatan Terhadap Pemberian Imunisasi Pada Anak Di Poliklinik Kesehatan Monginsidi Makassar Tahun 2020
Authors: Noviyanti Nur Indah , Noviana Ismi 
Published: March 2021

Berdasarkan data imunisasi Poliklinik kesehatan Monginsidi Makassar pada tahun 2018 jumlah anak yang di imunisasi sebanyak 108 anak, pada tahun 2019 sebanyak 182 anak, dan pada tahun 2020 sebanyak 130 anak, Tujuan dilakukannya penelitian ini yaitu, untuk mengetahui hubungan dukungan petugas kesehatan terhadap pemberian imunisasi pada anak di Poli Monginsi di Makaasar. Penelitian ini menggunakan metode analitik dengan pendekatan Cross Sectional Study untuk mengetahui hubungan dukungan petugas kesehatan terhadap pentingnya pemberian imunisasi di Poli Monginsidi Makassar, dengan jumlah Populasi adalah seluruh ibu yang memiliki anak umur 10-16 bulan yang berjumlah 60 orang di Poliklinik Kesehatan Monginsidi Makassar, yang melakukan kunjungan dari bulan Januari sampai dengan Juli 2020, jumlah sampel dalam penelitian ini sebanyak 60 orang dengan menggunakan tehnik total sampling. Dari hasil uji statistik dengan menggunakan uji Chi-Square di peroleh nilai P (0,000) < α (0,050). Maka Ha diterima dan Ho ditolak, artinya terdapat hubungan dukungan petugas kesehatan terhadap pemberian imunisasi di Poli klinik Kesehatan Monginsidi Makassar. Dengan demikian dapat ditarik kesimpulan bahwa dukungan petugas kesehatan sangat berpengaruh terhadap pemberian imunisasi
Digital technologies for risk category definition of subject of protection at Federal State Fire Supervision
Authors: Зобков Денис Валерьевич , Лагозин Андрей Юрьевич , Ушаков Дмитрий Викторович , Сурина Галина Петровна 
Published: March 2021

При подготовке изменений в Положение о федеральном государственном пожарном надзоре на основе концепции риск-ориентированного подхода в целях автоматизации процесса определения категории риска для объекта защиты разработано программное приложение - онлайн-калькулятор. Онлайн-калькулятор реализует новую модель отнесения объектов защиты к категориям риска, в которой учитываются не только категория риска для групп объектов, однородных по виду экономической деятельности и классам функциональной пожарной опасности, но и индивидуальные характеристики конкретного объекта защиты. Онлайн-калькулятор позволяет легко и быстро определить категорию риска объекта защиты или принять решение об ее изменении.
In the process of preparing changes to the Regulation on Federal State Fire Supervision on the basis of the concept of a risk-oriented approach, there has been developed an online calculator software application in order to automate the process of determining the risk category for the object of protection. The online calculator implements a new model for risk rating of objects of protection, which takes into account not only the risk category for groups of objects that are similar either in type of economic activity or functional fire hazard classes, but also the individual characteristics of a particular object of protection. The online calculator easily and quickly allows to determine the risk category of the object of protection or to take decision about its changing.
A Spatially Resolved Survey of Distant Quasar Host Galaxies. II. Photoionization and Kinematics of the ISM
Authors: Vayner Andrey , Wright Shelley A. , Murray Norman , Armus Lee , Boehle Anna , Cosens Maren , Larkin James E. , Mieda Etsuko , Walth Gregory 
Published: March 2021

Abstract
We present detailed observations of photoionization conditions and galaxy kinematics in 11 z = 1.39–2.59 radio-loud quasar host galaxies. Data were taken with the OSIRIS integral field spectrograph and the adaptive optics system at the W. M. Keck Observatory that targeted nebular emission lines (Hβ, [O iii], Hα, [N ii]) redshifted into the near-infrared (1–2.4 μm). We detect extended ionized emission on scales ranging from 1 to 30 kpc photoionized by stars, shocks, and active galactic nuclei (AGN). Spatially resolved emission-line ratios indicate that our systems reside off the star formation and AGN-mixing sequence on the Baldwin, Phillips, & Terlevich diagram at low redshift. The dominant cause of the difference between line ratios of low-redshift galaxies and our sample is due to lower gas-phase metallicities, which are 2–5× less compared to galaxies with AGN in the nearby universe. Using gas velocity dispersion as a proxy to stellar velocity dispersion and dynamical mass measurement through inclined disk modeling, we find that the quasar host galaxies are undermassive relative to their central supermassive black hole mass, with all systems residing off the local scaling (M
•–σ, M
•–M
*) relationship. These quasar host galaxies require substantial growth, up to an order of magnitude in stellar mass, to grow into present-day massive elliptical galaxies. Combining these results with part I of our sample paper, we find evidence for winds capable of causing feedback before the AGN host galaxies land on the local scaling relation between black hole and galaxy stellar mass, and before the enrichment of the interstellar medium to a level observed in local galaxies with AGN.
Observational Constraints in Delta-gravity: CMB and Supernovae
Authors: Martín Marco San , Alfaro Jorge , Rubio Carlos 
Published: March 2021

Abstract
Delta-gravity (DG) is a gravitational model based on an extension of general relativity given by a new symmetry called

. In this model, new matter fields are added to the original matter fields, motivated by the additional symmetry. We call them

matter fields. This model predicts an accelerating universe without the need to introduce a cosmological constant. In this work, we study the scalar cosmic microwave background (CMB) temperature (TT) power spectrum predicted by DG using an analytical hydrodynamic approach. To fit the Planck satellite’s data with the DG model, we used a Markov Chain Monte Carlo analysis. We also include a study about the compatibility between Type Ia supernovae (SNe Ia) and CMB observations in the DG context. Finally, we obtain the scalar CMB TT power spectrum and the fitted parameters needed to explain both SN Ia data and CMB measurements. The results are in reasonable agreement with both observations considering the analytical approximation. We also discuss whether the Hubble constant and the accelerating universe are in concordance with the observational evidence in the DG context.
The Peculiar Transient AT2018cow: A Possible Origin of a Type Ibn/IIn Supernova
Authors: Xiang Danfeng , Wang Xiaofeng , Lin Weili , Mo Jun , Lin Han , Burke Jamison , Hiramatsu Daichi , Hosseinzadeh Griffin , Howell D. Andrew , McCully Curtis , Valenti Stefan , Vinkó József , Wheeler J. Craig , Ehgamberdiev Shuhrat A. , Mirzaqulov Davron , Bódi Attila , Bognár Zsófia , Cseh Borbála , Hanyecz Ottó , Ignácz Bernadett , Kalup Csilla , Könyves-Tóth Réka , Kriskovics Levente , Ordasi András , Pál András , Sárneczky Krisztián , Seli Bálint , Szakáts Róbert , Arranz-Heras T. , Benavides-Palencia R. , Cejudo-Martínez D. , De la Fuente-Fernández P. , Escartín-Pérez A. , la Cuesta F. García-De , González-Carballo J. L. , González-Farfán R. , Limón-Martínez F. , Mantero A. , Naves-Nogués R. , Morales-Aimar M. , Ruíz-Ruíz V. R. , Soldán-Alfaro F. C. , Valero-Pérez J. , Violat-Bordonau F. , Zhang Tianmeng , Zhang Jujia , Li Xue , Chen Zhihao , Sai Hanna , Li Wenxiong 
Published: March 2021

Abstract
We present our photometric and spectroscopic observations of the peculiar transient AT2018cow. The multiband photometry covers from peak to ∼70 days, and the spectroscopy ranges from 5 to ∼50 days. The rapid rise (t
r ≲ 2.9 days), high luminosity (M

V,peak ∼ −20.8 mag), and fast decline after peak make AT2018cow stand out from any other optical transients, whereas we find that its light curves show a high resemblance to those of Type Ibn supernovae. Moreover, the spectral energy distribution remains at a high temperature of ∼14,000 K at t > 15 days after discovery. The spectra are featureless in the first 10 days, while some broad emission lines due to H, He, C, and O emerge later, with velocity declining from ∼14,000 to ∼3000 km s−1 at the end of our observations. Narrow and weak He I emission lines emerge in the spectra at t > 20 days after discovery. These emission lines are reminiscent of the features seen in interacting supernovae like the Type Ibn and IIn subclasses. We fit the bolometric light curves with a model of circumstellar interaction and radioactive decay of 56Ni and find a good fit with ejecta mass M
ej ∼ 3.16 M
⊙, circumstellar medium (CSM) mass M
CSM ∼ 0.04 M
⊙, and ejected 56Ni mass

M
⊙. The CSM shell might be formed in an eruptive mass ejection of the progenitor star. Furthermore, the host environment of AT2018cow implies a connection of AT2018cow with massive stars. Combining observational properties and the light-curve fitting results, we conclude that AT2018cow might be a peculiar interacting supernova that originated from a massive star.
Multiwavelength Observations of the Formation and Eruption of a Complex Filament
Authors: Zhang Y. , Bastian T. S. , Liu J. H. , Yu S. J. , Feng S. , Chen J. , Yan Y. H. 
Published: March 2021

Abstract
We present an analysis of the formation and eruption of a filament and fast coronal mass ejection associated with a flare that occurred in active region 11429 using observations in the ultraviolet, extreme ultraviolet, X-ray, and radio wavelength bands. Precursor activity began as an interaction between two filaments, F1 and F2, that are identified as having twisted magnetic flux ropes (MFRs). Transient brightenings in all wavelengths are observed as a result of this interaction, likely the result of magnetic reconnection between the two filaments. This interaction results in a reconfiguration of the two filaments into a long overlying filament and a shorter low-lying filament. The upper filament subsequently undergoes a partial confined eruption. Plasma flows originating near the east footpoint of F1 lead to an extension of the upper filament into the filament channel to the west, resulting in a new active region filament (ARF). This new filament begins a slow rise and expansion. During its slowly rising phase, the MFR in which the filament is embedded becomes visible, with both the filament and flux rope rising and expanding simultaneously. The twist of the magnetic rope is determined as four turns. The erupting configuration changes from a twisted arch shape to a reversed γ shape within ∼75 s at the beginning of the fast-rise phase, representing a transformation from twist to writhe. The observations provide a clear example of filament formation via the tether-cutting reconnection of two nearby filaments. A helical kink instability may be the trigger of the ARF eruption.
Large-scale Gravitational Lens Modeling with Bayesian Neural Networks for Accurate and Precise Inference of the Hubble Constant
Authors: Park Ji Won , Wagner-Carena Sebastian , Birrer Simon , Marshall Philip J. , Lin Joshua Yao-Yu , Roodman Aaron ,   (The LSST Dark Energy Science Collaboration)
Published: March 2021

Abstract
We investigate the use of approximate Bayesian neural networks (BNNs) in modeling hundreds of time delay gravitational lenses for Hubble constant (H
0) determination. Our BNN was trained on synthetic Hubble Space Telescope quality images of strongly lensed active galactic nuclei with lens galaxy light included. The BNN can accurately characterize the posterior probability density functions (PDFs) of model parameters governing the elliptical power-law mass profile in an external shear field. We then propagate the BNN-inferred posterior PDFs into an ensemble H
0 inference, using simulated time delay measurements from a plausible dedicated monitoring campaign. Assuming well-measured time delays and a reasonable set of priors on the environment of the lens, we achieve a median precision of 9.3% per lens in the inferred H
0. A simple combination of a set of 200 test lenses results in a precision of 0.5 km s−1 Mpc−1 (0.7%), with no detectable bias in this H
0 recovery test. The computation time for the entire pipeline—including the generation of the training set, BNN training and H
0 inference—translates to 9 minutes per lens on average for 200 lenses and converges to 6 minutes per lens as the sample size is increased. Being fully automated and efficient, our pipeline is a promising tool for exploring ensemble-level systematics in lens modeling for H
0 inference.
Connecting the Gravity Field, Moment of Inertia, and Core Properties in Jupiter through Empirical Structural Models
Authors: Neuenschwander Benno A. , Helled Ravit , Movshovitz Naor , Fortney Jonathan J. 
Published: March 2021

Abstract
Constraining Jupiter’s internal structure is crucial for understanding its formation and evolution history. Recent interior models of Jupiter that fit Juno’s measured gravitational field suggest an inhomogeneous interior and potentially the existence of a diluted core. These models, however, strongly depend on the model assumptions and the equations of state used. A complementary modeling approach is to use empirical structural models. These can later be used to reveal new insights into the planetary interior and be compared to standard models. Here we present empirical structural models of Jupiter where the density profile is constructed by piecewise-polytropic equations. With these models we investigate the relation between the normalized moment of inertia (MoI) and the gravitational moments J
2 and J
4. Given that only the first few gravitational moments of Jupiter are measured with high precision, we show that an accurate and independent measurement of the MoI value could be used to further constrain Jupiter’s interior. An independent measurement of the MoI with an accuracy better than ∼0.1% could constrain Jupiter’s core region and density discontinuities in its envelope. We find that models with a density discontinuity at ∼1 Mbar, as would produce a presumed hydrogen–helium separation, correspond to a fuzzy core in Jupiter. We next test the appropriateness of using polytropes, by comparing them with empirical models based on polynomials. We conclude that both representations result in similar density profiles and ranges of values for quantities like core mass and MoI.
Thermonuclear X-Ray Bursts with Late Secondary Peaks Observed from 4U 1608–52
Authors: Güver Tolga , Boztepe Tuğba , Göğüş Ersin , Chakraborty Manoneeta , Strohmayer Tod E. , Bult Peter , Altamirano Diego , Jaisawal Gaurava K. , Kocabıyık Tuğçe , Malacaria C. , Kashyap Unnati , Gendreau Keith C. , Arzoumanian Zaven , Chakrabarty Deepto 
Published: March 2021

Abstract
We report the temporal and spectral analysis of three thermonuclear X-ray bursts from 4U 1608−52, observed by the Neutron Star Interior Composition Explorer (NICER) during and just after the outburst observed from the source in 2020. In two of the X-ray bursts, we detect secondary peaks 30 and 18 s after the initial peaks. The secondary peaks show a fast rise exponential decay-like shape resembling a thermonuclear X-ray burst. Time-resolved X-ray spectral analysis reveals that the peak flux, blackbody temperature, and apparent emitting radius values of the initial peaks are in agreement with X-ray bursts previously observed from 4U 1608−52, while the same values for the secondary peaks tend toward the lower end of the distribution of bursts observed from this source. The third X-ray burst, which happened during much lower accretion rates, did not show any evidence for a deviation from an exponential decay and was significantly brighter than the previous bursts. We present the properties of the secondary peaks and discuss the events within the framework of short recurrence time bursts or bursts with secondary peaks. We find that the current observations do not fit in standard scenarios and challenge our understanding of flame spreading.
Deciphering the Kinematic Structure of the Small Magellanic Cloud through Its Red Giant Population
Authors: Zivick Paul , Kallivayalil Nitya , van der Marel Roeland P. 
Published: March 2021

Abstract
We present a new kinematic model for the Small Magellanic Cloud (SMC), using data from the Gaia Data Release 2 catalog. We identify a sample of astrometrically well-behaved red giant (RG) stars belonging to the SMC and cross-match with publicly available radial velocity (RV) catalogs. We create a 3D spatial model for the RGs, using RR Lyrae for distance distributions, and apply kinematic models with varying rotation properties and a novel tidal expansion prescription to generate mock proper motion (PM) catalogs. When we compare this series of mock catalogs to the observed RG data, we find that a combination of moderate rotation (with a magnitude of ∼10–20 km s−1 at 1 kpc from the SMC center, inclination between ∼50 and 80°, and a predominantly north-to-south line-of-nodes position angle of ∼180°) and tidal expansion (with a scaling of ∼10 km s−1 kpc−1) is required to explain the PM signatures. The exact best-fit parameters depend somewhat on whether we assess only the PMs or include the RVs as a qualitative check, leaving some tension remaining between the PM and RV conclusions. In either case, the parameter space preferred by our model is different from previously inferred rotational geometries, including from the SMC H i gas, and from the RG RV-only analyses and new SMC PM analyses, which conclude that a rotation signature is not detectable. Taken together this underscores the need to treat the SMC as a series of different populations with distinct kinematics.