bluuebunny/crossref_metadata_2025_split huggingface dataset:
UJI EFEKTIVITAS EKSTARK BUNGA PEPAYA TERHADAP KOLESTEROL MENCIT JANTAN YANG DI INDUKSI SUKROSA
Authors: Tampubolon Ester Juanita , Marpaung Febri Sri Astuti , Andika Muhammad Insan , Lubis Yolanda Eliza Putri , Mutia Maya Sari 
Published: March 2021

Abstrak Penelitian ini bertujuan untuk mengetahuiuji efektivitas ekstrak bunga pepaya terhadap kolesterol mencit jantan yang di induksi dengan sukrosa. Kolesterol adalah salah satu lemak tubuh yang berada bentuk dalam asam lemak bebas dan ester serta merupakan komponen utama selaput sel otak dan saraf. Salah satu buah-buahan yang mengandung serat tinggi yang dapat menormalkan tekanan darah adalah buah papaya. Buah pepaya banyak mengandung zat-zat kimia yang bermanfaat bagi tubuh, terutama pada pembuluh darah. Buah papaya kaya Karoten), vitamin C, akan vitamin A ( pektin dan enzim papain). Enzim lipoprotein lipase ini merupakan enzim yang berperan dalam menurunkan kadar trigliserida, sehingga dengan adanya gangguan insulin, hidrolisis trigliserida cenderung meningkat dan menyebabkan meningkatkan kadar trigliserida. Berdasarkan hasil diatas menunjukkan bahwa kelompok perlakuan yang paling besar penurunan kolesterol adalah dengan ekstrak bunga pepaya dosis 400 mg/kgBB turun 4,80 %. Kata Kunci : Carrica papaya, Kolesterol, Sukrosa
Microwave Heat Treatment to Manufacture Foam Glass Gravel
Authors: Paunescu Lucian 
Published: March 2021

Abstract
The paper aimed at the experimental manufacture of a foam glass gravel type by sintering at over 900 ºC a powder mixture composed of recycled glass waste (92%), sodium borate (6%), kaolin (0.3%), silicon carbide (1.7%) and water addition (12%). The originality of the work was the application of the unconventional technique of microwave heating through a predominantly direct heating procedure. The product foamed at 908 ºC had a very fine porous structure (pore size between 0.05-0.20 mm) and a compressive strength above the usual level of foam glass gravels (7.8 MPa). The apparent density of 0.28 g/cm3 corresponding to a bulk density of 0.20 g/cm3 and the thermal conductivity of 0.075 W/m·K ensures the thermal insulating character of the material required for use in the specific field of applications of foam glass gravel. The manufacturing process had an excellent energy efficiency, the specific energy consumption decreasing up to 0.70 kWh/kg.
A Distance-deviation Consistency and Model-independent Method to Test the Cosmic Distance–Duality Relation
Authors: Zhou Chichun , Hu Jian , Li Maocai , Yin Xunchang , Fang Guanwen 
Published: March 2021

Abstract
A distance-deviation consistency and model-independent method to test the cosmic distance–duality relation (CDDR) is provided. This method is worthy of attention for two reasons. First, a distance-deviation consistency method is used to pair subsamples: instead of pairing subsamples with redshift deviations smaller than a value of, say,

. The redshift deviation between subsamples decreases with the redshift to ensure the distance deviation stays the same. The method selects more subsamples at high redshift, up to z = 2.16, and provides 120 subsample pairs. Second, the model-independent method involves the latest data set of 1048 SNe Ia and 205 strong gravitational lensing systems (SGLS), which are used to obtain the luminosity distances D

L
and the ratio of angular diameter distance D

A
, respectively. With the model-independent method, parameters of the CDDR, the SNe Ia light curve, and the SGLS are fitted simultaneously. The result shows that

and CDDR is validated at the 1σ confidence level in the form of

.
Search for Low-energy Electron Antineutrinos in KamLAND Associated with Gravitational Wave Events
Authors: Abe S. , Asami S. , Gando A. , Gando Y. , Gima T. , Goto A. , Hachiya T. , Hata K. , Hayashida S. , Hosokawa K. , Ichimura K. , Ieki S. , Ikeda H. , Inoue K. , Ishidoshiro K. , Kamei Y. , Kawada N. , Kishimoto Y. , Kinoshita T. , Koga M. , Maemura N. , Mitsui T. , Miyake H. , Nakamura K. , Nakamura K. , Nakamura R. , Ozaki H. , Sakai T. , Sambonsugi H. , Shimizu I. , Shirai J. , Shiraishi K. , Suzuki A. , Suzuki Y. , Takeuchi A. , Tamae K. , Ueshima K. , Wada Y. , Watanabe H. , Yoshida Y. , Obara S. , Kozlov A. , Chernyak D. , Takemoto Y. , Yoshida S. , Umehara S. , Fushimi K. , Ichikawa A. K. , Nakamura K. Z. , Yoshida M. , Berger B. E. , Fujikawa B. K. , Learned J. G. , Maricic J. , Axani S. N. , Winslow L. A. , Fu Z. , Ouellet J. , Efremenko Y. , Karwowski H. J. , Markoff D. M. , Tornow W. , Li A. , Detwiler J. A. , Enomoto S. , Decowski M. P. , Grant C. , O’Donnell T. , Dell’Oro S. ,   (KamLAND Collaboration)
Published: March 2021

Abstract
We present the results of a search for MeV-scale electron antineutrino events in KamLAND coincident with the 60 gravitational wave events/candidates reported by the LIGO/Virgo collaboration during their second and third observing runs. We find no significant coincident signals within a ±500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antineutrino fluence between 108 and 1013 cm−2 for neutrino energies in the energy range of 1.8–111 MeV.
Planets Across Space and Time (PAST). I. Characterizing the Memberships of Galactic Components and Stellar Ages: Revisiting the Kinematic Methods and Applying to Planet Host Stars
Authors: Chen Di-Chang , Xie Ji-Wei , Zhou Ji-Lin , Dong Subo , Liu Chao , Wang Hai-Feng , Xiang Mao-Sheng , Huang Yang , Luo Ali , Zheng Zheng 
Published: March 2021

Abstract
Over 4000 exoplanets have been identified and thousands of candidates are to be confirmed. The relations between the characteristics of these planetary systems and the kinematics, Galactic components, and ages of their host stars have yet to be well explored. To address these questions, we conduct a research project, dubbed Planets Across Space and Time (PAST). To do this, one of the key steps is to accurately characterize the planet host stars. In this paper, Paper I of the PAST series, we revisit the kinematic method for classification of Galactic components and extend the applicable range of velocity ellipsoid from ∼100 pc to ∼1500 pc from the Sun in order to cover most known planet hosts. Furthermore, we revisit the age–velocity dispersion relation (AVR), which allows us to derive kinematic ages with a typical uncertainty of 10–20% for an ensemble of stars. Applying the above revised methods, we present a catalog of kinematic properties (i.e., Galactic positions, velocities, and the relative membership probabilities among the thin disk, thick disk, Hercules stream, and the halo) as well as other basic stellar parameters for 2174 host stars of 2872 planets by combining data from Gaia, LAMOST, APOGEE, RAVE, and the NASA exoplanet archive. The revised kinematic method and AVR, as well as the stellar catalog of kinematic properties and ages, lay the foundation for future studies of exoplanets in space and time in the Galactic context.
Statistical Survey of Reservoir Phenomenon in Energetic Proton Events Observed by Multiple Spacecraft
Authors: Wang Yang , Lyu Dan , Xiao Boxi , Qin Gang , Zhong Yushui , Lian Lele 
Published: March 2021

Abstract
In this work, reservoir phenomenon in the decay phase of gradual solar energetic particle (SEP) events are investigated with two Helios and the IMP 8 spacecraft from 1976 January to 1980 March and two STEREO and the SOHO spacecraft from 2010 January to 2014 September. Using these data, 62 reservoir events of solar energetic protons were identified, and the effects of perpendicular diffusion and magnetic mirroring on the formation of the reservoir phenomenon have been studied. We find that the reservoir events could be observed in almost all longitudes in the ecliptic at 1 au; thus, the perpendicular diffusion in interplanetary space is an important mechanism to explain the uniform distribution of SEPs. Furthermore, in the 1976 April 30 event, the effects of magnetic mirroring associated with an interplanetary coronal mass ejection were observed during the reservoir phenomenon. Therefore, the effects of magnetic mirroring could also help to form the reservoir phenomenon. This study could improve the understanding of the propagation of SEPs in interplanetary space.
Rigorous Theory for Secondary Cosmic-Ray Ionization
Authors: Ivlev Alexei V. , Silsbee Kedron , Padovani Marco , Galli Daniele 
Published: March 2021

Abstract
The energy spectrum of electrons produced in molecular gas by interstellar cosmic rays (CRs) is rigorously calculated as a function of gas column density N traversed by the CRs. This allows us to accurately compute the local value of the secondary ionization rate of molecular hydrogen,

, as a function of the local primary ionization rate, ζ

p
(N). The ratio

increases monotonically with N, and can considerably exceed the value of ≈0.67 commonly adopted in the literature. For sufficiently soft interstellar spectra, the dependence

versus N is practically insensitive to their particular shape and thus is a general characteristic of the secondary CR ionization in dense gas.
A ΔR ∼ 9.5 mag Superflare of an Ultracool Star Detected by the SVOM/GWAC System
Authors: Xin L. P. , Li H. L. , Wang J. , Han X. H. , Xu Y. , Meng X. M. , Cai H. B. , Huang L. , Lu X. M. , Qiu Y. L. , Wang X. G. , Liang E. W. , Dai Z. G. , Wang X. Y. , Wu C. , Zhang J. B. , Li G. W. , Turpin D. , Feng Q. C. , Deng J. S. , Sun S. S. , Zheng T. C. , Yang Y. G. , Wei J. Y. 
Published: March 2021

Abstract
We report the detection and follow-up of a superstellar flare GWAC 181229A with an amplitude of ΔR ∼ 9.5 mag on an M9-type star by SVOM/GWAC and the dedicated follow-up telescopes. The estimated bolometric energy E
bol is (5.56–9.25) × 1034 erg, which makes the event one of the most powerful flares seen on ultracool stars. The magnetic strength is inferred to be 3.6–4.7 kG. Thanks to sampling with a cadence of 15 s, a new component near the peak time with a very steep decay is detected in the R-band light curve, followed by the two-component flare template given by Davenport et al. An effective temperature of 5340 ± 40 K is measured by fitting a blackbody shape to the spectrum in the shallower phase during the flare. The filling factors of the flare are estimated to be ∼30% and 19% at the peak time and at 54 minutes after the first detection. The detection of this particular event with large amplitude, huge emitted energy, and a new component demonstrates that high-cadence sky monitoring cooperation with fast follow-up observations is very important for understanding the violent magnetic activity.
Transient Formation of Loops in the Core of an Active Region
Authors: Tripathi Durgesh 
Published: March 2021

Abstract
We study the formation of transient loops in the core of the AR 11890. For this purpose, we have used the observations recorded by the Atmospheric Imaging Assembly (AIA) and the Interface Region Imaging Spectrograph (IRIS). For photospheric field configuration, we have used the line-of-sight (LOS) magnetograms obtained from the Helioseismic and Magnetic Imager. The transient is simultaneously observed in all the UV and EUV channels of AIA and the three slit-jaw images from IRIS. The coexistence of the transient in all AIA and IRIS SJI channels suggests the transient’s multithermal nature. The transient consists of short loops located at the base of the transient, as well as long loops. A differential emission measure analysis shows that the transient has a clumpy structure. The highest emission observed at the base is within the temperature bin of

. We observe the longer loops at a similar temperature, albeit very feeble. Using LOS magnetograms, we conclude that the magnetic reconnection may have caused the transient. Our observations further suggest that the physics of the formation of such transients may be similar to those of typical coronal jets, albeit in different topological configurations. Such multiwavelength observations shed light on the formation of hot plasma in the solar corona and provide further essential constraints on modeling the thermodynamics of such transients.
Modeling the in-orbit Background of PolarLight
Authors: Huang Jiahui , Feng Hua , Li Hong , Long Xiangyun , Yang Dongxin , Zeng Weihe , Wu Qiong , Jiang Weichun , Minuti Massimo , Costa Enrico , Muleri Fabio , Citraro Saverio , Nasimi Hikmat , Yu Jiandong , Jin Ge , Zeng Zhi , Zeng Ming , An Peng , Baldini Luca , Bellazzini Ronaldo , Brez Alessandro , Latronico Luca , Sgrò Carmelo , Spandre Gloria , Pinchera Michele , Soffitta Paolo 
Published: March 2021

Abstract
PolarLight is a gas pixel X-ray polarimeter mounted on a CubeSat, which was launched into a Sun-synchronous orbit in 2018 October. We build a mass model of the whole CubeSat with the Geant4 toolkit to simulate the background induced by the cosmic X-ray background (CXB) and high-energy charged particles in the orbit. The simulated energy spectra and morphologies of event images both suggest that the background measured with PolarLight is dominated by high-energy electrons, with a minor contribution from protons and the CXB. The simulation reveals that, in the energy range 2–8 keV, roughly 28% of background events are caused by energy deposited by a secondary electron with an energy of a few keV, in a physical process identical to the detection of X-rays. Thus, this fraction of the background cannot be discriminated from X-ray events. The background distribution is uneven on the detector plane, with an enhancement near the edges. The edge effect occurs because high-energy electrons tend to produce long tracks, which are discarded by the readout electronics unless energy is partially deposited near the edges. The internal background rate is expected to be around 6 × 10−3 counts s−1 cm−2 at 2–8 keV if an effective particle discrimination algorithm can be applied. This indicates that the internal background should be negligible for future focusing X-ray polarimeters with a focal size of the order of millimeters.
X-Ray Intraday Variability of the TeV Blazar PKS 2155–304 with Suzaku during 2005–2014
Authors: Zhang Zhongli , Gupta Alok C. , Gaur Haritma , Wiita Paul J. , An Tao , Lu Yang , Fan Shida , Xu Haiguang 
Published: March 2021

Abstract
We have examined 13 pointed observations of the TeV-emitting high synchrotron peak blazar PKS 2155−304, taken by the Suzaku satellite throughout its operational period. We found that the blazar showed large-amplitude intraday variabilities in the soft (0.8–1.5 keV) and the hard (1.5–8.0 keV) bands in the light curves. Spectral variability on intraday timescales is estimated using the hardness ratio. The blazar usually becomes harder when brighter and vice versa, following the typical behavior of high synchrotron peak blazars. The power spectral density analyses of 11 out of 13 light curves in the total energy (0.8–8.0 keV) are found to be dominated by red noise, with power-law spectral indices that span a large range, from −2.81 to −0.88. Discrete correlation function analyses of all the 13 light curves between the soft and the hard bands show that they are well correlated and peak at, or very close to, zero lag. This indicates that the emissions in soft and hard bands are probably cospatial and emitted from the same population of leptons. Considering fluxes versus variability timescales, we found no correlation on intraday timescales, implying that X-ray emission from PKS 2155−304 is not dominated by simple changes in the Doppler factor. We briefly discuss the most likely emission mechanisms responsible for the observed flux and spectral variabilities and place constraints on magnetic field strength and Lorentz factors of the electrons emitting the X-rays in the most likely scenario.
The Neupert Effect of Flare Ultraviolet and Soft X-Ray Emissions
Authors: Qiu Jiong 
Published: March 2021

Abstract
We model the Neupert effect that relates flare heating energy with the observed soft X-ray (SXR) emission. The traditional form of the Neupert effect refers to the correlation between the time-integrated hard X-ray or microwave light curve and the SXR light curve. In this paper, we instead use as the proxy for heating energy the ultraviolet (UV) emission at the footpoints of flare loops and modify the model of the Neupert effect by taking into account the discrete nature of flare heating, as well as cooling. In the modified empirical model, spatially resolved UV light curves from the transition region or upper chromosphere are each convolved with a kernel function characterizing the decay of the flare loop emission. Contributions by all loops are summed to compare with the observed total SXR emission. The model has successfully reproduced the observed SXR emission from its rise to decay. To estimate the heating energies in flare loops, we also employ the UV footpoint calorimeter (UFC) method that infers heating rates in flare loops from these UV light curves and models the evolution of flare loops with a zero-dimensional hydrodynamic code. The experiments show that a multitude of impulsive heating events do not well reproduce the observed flare SXR light curve, but a two-phase heating model leads to better agreement with observations. Comparison of the two models of the Neupert effect further allows us to calibrate the UFC method and improve the estimate of heating rates in flare loops continuously formed by magnetic reconnection throughout the flare evolution.
The Evolution of NGC 7465 as Revealed by Its Molecular Gas Properties
Authors: Young Lisa M. , Meier David S. , Bureau Martin , Crocker Alison , Davis Timothy A. , Topal Selçuk 
Published: March 2021

Abstract
We present ALMA observations of CO isotopologues and high-density molecular tracers (HCN, HCO+, CN, etc.) in NGC 7465, an unusually gas-rich early-type galaxy that acquired its cold gas recently. In the inner 300 pc, the molecular gas kinematics are misaligned with respect to all other galaxy components; as the gas works its way inward, it is torqued into polar orbits about the stellar kinematically decoupled core (KDC), indicating that the stellar KDC is not related to the current gas accretion event. The galaxy also exhibits unusually high 12CO/13CO line ratios in its nucleus but typical 13CO/C18O ratios. Our calculations show that this result does not necessarily indicate an unusual [12CO/13CO] abundance ratio but rather that 12CO (1–0) is optically thin due to high temperatures and/or large line widths associated with the inner decoupled, misaligned molecular structure. Line ratios of the higher-density tracers suggest that the densest phase of molecular gas in NGC 7465 has a lower density than is typical for nearby galaxies, possibly as a result of the recent gas accretion. All of the observed molecular properties of NGC 7465 are consistent with it having acquired its molecular (and atomic) gas from a spiral galaxy. Further detailed studies of the CO isotopologues in other early-type galaxies would be valuable for investigating the histories of those that may have acquired their gas from dwarfs. Finally, these ALMA data also show an unidentified line source that is probably a background galaxy similar to those found at z = 1–3 in blind CO surveys.
Deciphering the 3D Orion Nebula-IV: The HH 269 Flow Emerges from the Orion-S Embedded Molecular Cloud
Authors: O’Dell C. R. , Abel N. P. , Ferland G. J. 
Published: March 2021

Abstract
We have extended the membership and determined the 3D structure of the large (0.19 pc) HH 269 sequence of shocks in the Orion Nebula. All of the components lie along a track that is highly tilted to the plane of the sky and emerge from within the Orion-S embedded molecular cloud. Their source is probably either the highly obscured mm 9 source associated with a high N2H+ density core (more likely) or the more distant star COUP 632 (less likely). The former must be located in the photon dominated region (PDR) underlying the ionized surface of the Orion-S Cloud, while the latter would be embedded within the Orion-S Cloud. The flows seem to be episodic, with intervals of 1900–2600 yr or 700–2600 yr if COUP 632 is the source.
Eight-year Simultaneous Monitoring Observations of H2O and SiO Masers toward V627 Cas
Authors: Yang Haneul , Cho Se-Hyung , Yun Youngjoo , Yoon Dong-Hwan , Kim Jaeheon 
Published: March 2021

Abstract
Simultaneous monitoring observations of H2O 61,6 − 52,3 and SiO v = 1, 2, J = 1 → 0, v = 1, J = 2 → 1, J = 3 → 2 masers were performed toward the suspected D-type symbiotic star V627 Cas from 2011 October to 2020 March using the Korean Very Long Baseline Interferometry (VLBI) Network (KVN) single-dish telescopes. All spectra of the H2O masers showed highly redshifted emissions with respect to the stellar velocity of −52 km s−1 with high asymmetries. In addition, the spectra of the H2O maser showed three components which varied according to observational dates. On the other hand, the SiO v = 1, 2, J = 1 → 0 and v = 1, J = 2 → 1 masers exhibited a predominantly blueshifted emission in most epochs. The SiO v = 1, J = 3 → 2 maser has arisen around the stellar velocity from 2016 November 19 and shows a predominantly redshifted emission from 2018 June 15. We analyze time variations of the H2O and SiO maser intensities, their intensity ratios, peak and mean velocities, and full width zero power. Based on these analyses, the asymmetries of the H2O and SiO masers’ spectra in V627 Cas and the variation characteristics of the maser properties of the different maser lines are discussed. As a possible cause of asymmetries, the influence of a hot component located at the eastern part of the red giant can be suggested based on the KVN VLBI results. The differences in the variation characteristics of the maser properties may originate from the differences in their locations and excitation conditions.
Giant Radio Quasars: Sample and Basic Properties
Authors: Kuźmicz Agnieszka , Jamrozy Marek 
Published: March 2021

Abstract
We present the largest sample of giant radio quasars (GRQs), which are defined as having a projected linear size greater than 0.7 Mpc. The sample consists of 272 GRQs, of which 174 are new objects discovered through cross-matching the NRAO Very Large Array Sky Survey and the Sloan Digital Sky Survey 14th Data Release Quasar Catalog (DR14Q) and confirmed using Faint Images of the Radio Sky at Twenty-Centimeters (FIRST) radio maps. In our analysis we compare the GRQs with 367 smaller, lobe-dominated radio quasars found using our search method, as well as with quasars from the SDSS DR14Q, investigating the parameters characterizing their radio emission (i.e., total and core radio luminosity, radio core prominence), optical properties (black hole masses, accretion rates, distribution in Eigenvector 1 plane) and infrared colors. For the GRQs and smaller radio quasars we find a strong correlation between [O III] luminosity and radio luminosity at 1.4 GHz, indicating a strong connection between radio emission and conditions in the narrow-line region. We spot no significant differences between GRQs and smaller radio quasars, however we show that most extended radio quasars belong to a quasar population of evolved active galactic nuclei with large black hole masses and low accretion rates. We also show that GRQs have bluer W2–W3 colors compared to SDSS quasars with FIRST detections, indicating differences in the structure of the dusty torus.