bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Lyα Emission in Solar Flares. I. A Statistical Study on Its Relationship with the 1–8 Å Soft X-Ray Emission
Authors: Jing Zhichen , Pan Wuqi , Yang Yukun , Song Dechao , Tian Jun , Li Y. , Cheng X. , Hong Jie , Ding M. D. 
Published: November 2020

Abstract
We statistically study the relationship between the Lyα and 1–8 Å soft X-ray (SXR) emissions from 658 M- and X-class solar flares observed by the Geostationary Operational Environmental Satellite during 2006–2016. Based on the peak times of the two wave band emissions, we divide the flares into three types. Type I (III) has an earlier (a later) peak time in the Lyα emission than that in the SXR emission, while type II has nearly the same peak time (within the time resolution of 10 s) between the Lyα and SXR emissions. In these 658 flares, we find that there are 505 (76.8%) type I flares, 10 (1.5%) type II flares, and 143 (21.7%) type III flares, and that the three types appear to have no dependence on the flare duration, flare location, or solar cycle. Besides the main peak, the Lyα emission of the three type flares also shows sub-peaks which can appear in the impulsive or gradual phase of the flare. It is found that the main-peak (for type I) and subpeak (for type III) emissions of Lyα that appear in the impulsive phase follow the Neupert effect in general. This indicates that such Lyα emissions are related to the nonthermal electron beam heating. While the main-peak (for type III) and subpeak (for type I) emissions of Lyα that appear in the gradual phase are supposed to be primarily contributed by the thermal plasma that cools down.
The Possibility of the Secondary Object in GW190814 as a Neutron Star
Authors: Huang Kaixuan , Hu Jinniu , Zhang Ying , Shen Hong 
Published: November 2020

Abstract
A compact object was observed with a mass of

by LIGO Scientific and Virgo collaborations (LVC) in GW190814, which provides a great challenge to investigations of supranuclear matter. To study this object, the properties of the neutron star are systematically calculated within the latest density-dependent relativistic mean-field (DDRMF) parameterizations, which are determined by the ground-state properties of spherical nuclei. The maximum masses of the neutron star calculated by DD-MEX and DD-LZ1 sets can be around

with quite stiff equations of state generated by their strong repulsive contributions from vector potentials at high densities. Their maximum speeds of sound c

s
/c are smaller than

at the center of the neutron star, and the dimensionless tidal deformabilities at

are less than 800. Furthermore, the radii of

also satisfy the constraint from the observation of simultaneous mass–radius measurements (Neutron star Interior Composition Explorer). Therefore, we conclude that one cannot exclude the possibility of the secondary object in GW190814 as a neutron star composed of hadron matter from DDRMF models.
X-Ray Constraints on the Spectral Energy Distribution of the z = 5.18 Blazar SDSS J013127.34−032100.1
Authors: An Hongjun , Romani Roger W. 
Published: November 2020

Abstract
We report on X-ray measurements constraining the spectral energy distribution (SED) of the high-redshift z = 5.18 blazar SDSS J013127.34−032100.1 with new XMM-Newton and NuSTAR exposures. The blazar’s X-ray spectrum is well fit by a power law with Γ = 1.9 and

, or a broken power law with

,

, and a break energy

for an expected absorbing column density of

, supported by spectral fitting of a nearby bright source. No additional spectral break is found at higher X-ray energies (1–30 keV). We supplement the X-ray data with lower-energy radio-to-optical measurements and Fermi-LAT gamma-ray upper limits, construct broadband SEDs of the source, and model the SEDs using a synchro-Compton scenario. This modeling constrains the bulk Doppler factor of the jets to ≥7 and ≥6 (90%) for the low- and high-N
H SEDs, respectively. The corresponding beaming implies ≥130 (low N
H) or

(high N
H) high-spin supermassive black holes similar to J0131 exist at similar redshifts.
ALMA and VLA Observations of EX Lupi in Its Quiescent State
Authors: White Jacob Aaron , Kóspál Á. , Hughes A. G. , Ábrahám P. , Akimkin V. , Banzatti A. , Chen L. , de Miera F. Cruz-Sáenz , Dutrey A. , Flock M. , Guilloteau S. , Hales A. S. , Henning T. , Kadam K. , Semenov D. , Sicilia-Aguilar A. , Teague R. , Vorobyov E. I. 
Published: November 2020

Abstract
Extreme outbursts in young stars may be a common stage of pre-main-sequence stellar evolution. These outbursts, caused by enhanced accretion and accompanied by increased luminosity, can also strongly impact the evolution of the circumstellar environment. We present Atacama Large Millimeter Array (ALMA) and Very Large Array observations of EX Lupi, a prototypical outburst system, at 100, 45, and 15 GHz. We use these data, along with archival ALMA 232 GHz data, to fit radiative transfer models to EX Lupi’s circumstellar disk in its quiescent state following the extreme outburst in 2008. The best-fit models show a compact disk with a characteristic dust radius of 45 au and a total mass of 0.01 M
⊙. Our modeling suggests grain growth to sizes of at least 3 mm in the disk, possibly spurred by the recent outburst, and an ice line that has migrated inward to 0.2–0.3 au post-outburst. At 15 GHz, we detected significant emission over the expected thermal disk emission which we attribute primarily to stellar (gyro)synchrotron and free–free disk emission. Altogether, these results highlight what may be a common impact of outbursts on the circumstellar dust.
Robustness of the Pairwise Kinematic Sunyaev–Zeldovich Power Spectrum Shape as a Cosmological Gravity Probe
Authors: Zheng Yi 
Published: November 2020

Abstract
We prove from the modified gravity (MG) galaxy/halo mock catalogs that the shape of the pairwise kinematic Sunyaev–Zeldovich (kSZ) power spectrum P
kSZ has constraining power on discriminating different gravity theories on cosmological scales. By varying the effective optical depth τ
T as a free parameter, we verify that the τ
T-f (the linear growth rate) degeneracy in the linear theory of P
kSZ is broken down by the nonlinear structure growth and the scale dependence of f in some MG theories. Equivalently speaking, the shape of P
kSZ alone could be used to tightly constrain the MG theories on cosmological scales. With good knowledge of galaxy density biases, we verify that a combination of the next-generation galaxy spectroscopic redshift and CMB surveys, e.g., BOSS+CMB-S4 or DESI+CMB-S4, could potentially discriminate f(R) models from the general relativity at the ∼5σ level using the shape of the galaxy pairwise kSZ dipole P
kSZ,ℓ = 1 alone, when f

R0 = 10−4.
Measurements of the z ∼ 6 Intergalactic Medium Optical Depth and Transmission Spikes Using a New z > 6.3 Quasar Sample
Authors: Yang Jinyi , Wang Feige , Fan Xiaohui , Hennawi Joseph F. , Davies Frederick B. , Yue Minghao , Eilers Anna-Christina , Farina Emanuele P. , Wu Xue-Bing , Bian Fuyan , Pacucci Fabio , Lee Khee-Gan 
Published: November 2020

Abstract
We report new measurements of the intergalactic medium (IGM) Lyα and Lyβ effective optical depth at 5.3 < z < 6.5, using a new sample of quasar sight lines including 32 quasars at 6.308 ≤ z ≤ 7.00. These quasars provide a large statistical sample to measure the IGM evolution during the transition phase of the reionization epoch. We construct a data set of deep optical spectra of these quasars using VLT, Keck, Gemini, LBT, and MMT. We measure the Lyα effective optical depth at 5.36 < z < 6.57 using the Lyα forests of both individual spectra and the stacked spectrum. The large scatter of individual measurements is consistent with previous work, suggesting an inhomogeneous reionization process. Combining our new measurements and previous results, we obtain a best fit for the Lyα effective optical depth evolution at z > 5.3,

. We then estimate the observed Lyβ effective optical depth using Lyβ forests and convert them to Lyα optical depth for comparison, which provides additional constraints on the evolution of the IGM optical depth. The Lyβ-based measurements are generally in agreement with the best-fit evolution obtained from Lyα forests. Using this new sample, we identify 389 Lyα and 50 Lyβ transmission spikes at 5.5 < z < 6.3. The upper limits of Lyα optical depth estimated using transmission spikes are well consistent with our best-fit evolution. The evolution in number density of these high-redshift transmission spikes suggests a rapid transition phase at the end of the reionization. Comparison of our optical depth measurements with hydrodynamical simulations indicates an IGM neutral hydrogen fraction

at z = 6.
Activity Complexes and a Prominent Poleward Surge during Solar Cycle 24
Authors: Wang Zi-Fan , Jiang Jie , Zhang Jie , Wang Jing-Xiu 
Published: November 2020

Abstract
Long-lasting activity complexes (ACs), characterized as a series of closely located, continuously emerging solar active regions (ARs), are considered generating prominent poleward surges from observations. The surges lead to significant variations of the polar field, which are important for the modulation of solar cycles. We aim to study a prominent poleward surge during solar cycle 24 on the southern hemisphere, and analyze its originating ACs and the effect on the polar field evolution. We automatically identify and characterize ARs based on synoptic magnetograms from the Solar Dynamics Observatory. We assimilate these ARs with realistic magnetic configuration into a surface flux transport model, and simulate the creation and migration of the surge. Our simulations well reproduce the characteristics of the surge and show that the prominent surge is mainly caused by the ARs belonging to two ACs during Carrington rotations 2145–2159 (2013 December–2015 January). The surge has a strong influence on the polar field evolution of the southern hemisphere during the latter half of cycle 24. Without the about one-year-long flux emergence in the form of ACs, the polar field around the cycle minimum would have remained at a low level and even reversed to the polarity at cycle 23 minimum. Our study also shows that the long-lived unipolar regions due to the decay of the earlier emerging ARs cause an intrinsic difficulty of automatically identifying and precisely quantifying later emerging ARs in ACs.
Lyman Continuum Escape Fraction from Low-mass Starbursts at z = 1.3*
Authors: Alavi Anahita , Colbert James , Teplitz Harry I. , Siana Brian , Scarlata Claudia , Rutkowski Michael , Mehta Vihang , Henry Alaina , Dai 戴 Y. Sophia 昱 , Haardt Francesco , Bagley Micaela 
Published: November 2020

Abstract
We present a new constraint on the Lyman continuum (LyC) escape fraction at

. We obtain deep, high sensitivity far-UV imaging with the Advanced Camera for Surveys Solar Blind Channel on the Hubble Space Telescope, targeting 11 star-forming galaxies at 1.2 < z < 1.4. The galaxies are selected from the 3D-HST survey to have high Hα equivalent width (EW) with an EW > 190 Å, low stellar mass (M
* < 1010
M
⊙), and U-band magnitude of U < 24.2. These criteria identify young, low metallicity star-bursting populations similar to the early star-forming galaxies believed to have reionized the universe. We do not detect any LyC signal (with a signal-to-noise ratio > 3) in the individual galaxies or in the stack in the far-UV images. We place 3σ limits on the relative escape fraction of individual galaxies to be

and a stacked 3σ limit of

. Measuring various galaxy properties, including stellar mass, dust attenuation, and star formation rate, we show that our measured values fall within the broad range of values covered by the confirmed LyC emitters from the literature. In particular, we compare the distribution of Hα and [O III] EWs of confirmed LyC emitters and non-detections, including the galaxies in this study. Finally, we discuss if a dichotomy seen in the distribution of Hα EWs can perhaps distinguish the LyC emitters from the non-detections.
The Effect of Supernovae on the Turbulence and Dispersal of Molecular Clouds
Authors: Lu Zu-Jia , Pelkonen Veli-Matti , Padoan Paolo , Pan Liubin , Haugbølle Troels , Nordlund Åke 
Published: November 2020

Abstract
We study the impact of supernovae on individual molecular clouds, using a high-resolution magnetohydrodynamic simulation of a 250 pc region where we resolve the formation of individual massive stars. The supernova feedback is implemented with real supernovae, meaning supernovae that are the natural evolution of the resolved massive stars, so their position and timing are self-consistent. We select a large sample of molecular clouds from the simulation to investigate the supernova energy injection and the resulting properties of molecular clouds. We find that molecular clouds have a lifetime of a few dynamical times, less than half of them contract to the point of becoming gravitationally bound, and the dispersal time of bound clouds of order one dynamical time is a factor of 2 shorter than that of unbound clouds. We stress the importance of internal supernovae, that is, massive stars that explode inside their parent cloud, in setting the cloud dispersal time, and their huge overdensity compared to models where the supernovae are randomly distributed. We also quantify the energy injection efficiency of supernovae as a function of supernova distance to the clouds. We conclude that intermittent driving by supernovae can maintain molecular cloud turbulence and may be the main process for cloud dispersal and that the full role of supernovae in the evolution of molecular clouds cannot be fully accounted for without a self-consistent implementation of the supernova feedback.
An Investigation of Fragmentation in the Disk Instability Model for Giant Planet Formation
Authors: Jin Liping , Liu Fenglei , Jiang Tao , Tang Pengfei , Yang Jingxi 
Published: November 2020

Abstract
We investigate a few issues regarding fragmentation in the disk instability model for giant planet formation—specifically, initial clump mass (M
p), fragmentation region, and fragmentation starting time, ending time, and duration. By running calculations over a wide parameter space and using an evolutionary model of protoplanetary disks, we study dependence on properties of the parent cloud core of the protostar+disk system. We investigate evolution of M
p–R relationship for clumps forming at different times during the disk evolution. We find that, in general, for the same radius, M
p changes slightly with time, first decreasing and then increasing. In different disks, for the same radius, M
p does not change significantly with ω, decreases with M
MCC, and increases with T
MCC, where ω, M
MCC, and T
MCC are angular velocity, mass, and temperature of a parent core. Fragmentation might occur most probably at 20–200 au, at 200–450 au with less probability, and at >450 au with small probability. M
p might be most probably between 3–35M
J, between 35–80M
J with less probability, and >80M
J with small probability. The ranges of the fragmentation starting time, ending time, and duration are (1–3) × 105 yr,

(
2
–
25
)
×

10

5

yr

, and

(
0.1
–
25
)
×

10

5

yr

, respectively. We derive an analytical formula that shows dependence of

M

p

on disk properties and can be used to understand numerical calculations. We tentatively use our calculations to understand exoplanet observations.
Il faut une équipe ( un village ) pour élever un bébé ( un enfant )
Authors: Garnier Anne-Marie , Mosca Francesca 
Published: November 2020

La prise en compte des besoins des bébés est déterminante pour leur développement. Or, c’est une période de grande vulnérabilité pour les mères, où l’étayage autour de la dyade est essentiel. Si « le bébé n’existe pas, seul », comme le dit Winnicott, les mères trop seules existent, et ne s’en portent pas bien, qu’elles souffrent de pathologies psychiatriques, d’isolement dû à la migration, d’histoires marquées par la carence. Comment faire équipe avec des familles en difficulté avec leurs bébés ? Quelles sont les particularités de ce travail ? Nous présenterons le travail de deux équipes de périnatalité, rattachées à deux services de psychiatrie de l’enfant et de l’adolescent de la banlieue parisienne. De nombreux exemples cliniques viendront étayer notre propos.
Assessing Variability of Control Within a Single Day in Intermittent Exotropia
Authors: Prile Sharlene Marie , Kim Jinhyun , Moon Yeji , Lim Hyun Taek 
Published: November 2020

Purpose:
To assess intra-individual hour-to-hour variability of control in intermittent exotropia using a simple office scale: Look And Cover, then Ten seconds of Observation Scale for Exotropia (LACTOSE).

Methods:
In this prospective cross-sectional study, the degree of control for distance and near was measured using the LACTOSE, a 5-point scale ranging from 0 to 4. A single investigator performed multiple measurements of the control of each patient with at least an hour interval between measurements.

Results:

Of the 95 patients with intermittent exotropia enrolled, 66 (69.5%) were assessed two times and 29 (30.5%) were assessed three times for their control. Most patients had consistent control scores across multiple assessments for distance (n = 63, 66.3%) and near (n = 70, 73.7%). Forty-five (47.4%) patients demonstrated variable control for either distance or near, mostly (n = 27, 60.0%) showing a one-step difference. None presented with more than a two-step difference in the control score on repeated measurements. An initial LACTOSE score of 4 (very poor control) or 1 (very good control) remained unchanged in subsequent assessments for both distance (
P
= .049) and near (
P
< .001).

Conclusions:
One-third of patients with intermittent exotropia showed variable control scores even during a single day across multiple measurements using the LACTOSE scale. Those who showed consistent control had very good or very poor control, whereas those with variable control had not had very good or very poor control on their initial LACTOSE measurements.

[
J Pediatr Ophthalmol Strabismus.
2020;57(6):378–383.]
Iniciativa popular estadual no Brasil
Authors: Sgarbossa Luís Fernando , Bittencourt Laura Cabrelli 
Published: November 2020

A iniciativa legislativa popular ou autolegislação, apresentando-se como uma forma de exercício direto de poder pelo povo, é instituição relativamente recente no sistema constitucional brasileiro e tema relevante no âmbito do Direito Constitucional. Apesar de razoavelmente estudada em nível federal, a iniciativa popular estadual ainda é pouco explorada pela literatura nacional. O presente estudo, resultado parcial de projeto de pesquisa em andamento, examina tal temática a partir de pesquisa básica, de levantamento, quantitativa, qualitativa e comparativa. Após uma análise de tal instituto nas 27 normas fundamentais subnacionais em vigor no país, em nível estadual e distrital, foi possível constatar que todas as constituições estaduais e a Lei Orgânica do Distrito Federal prevêem iniciativa popular de lei; que dezenove Estados contemplam iniciativa popular de Emendas à Constituição; que dez Estados adotam o mesmo procedimento para ambas as espécies em termos de iniciativa, em termos dispersão, quóruns e formalidades exigidas; que oito Estados, no entanto, estabelecem critérios distintos para o exercício do referido direito quanto à iniciativa voltada à produção de normas constitucionais ou infraconstitucionais. A partir dos resultados da pesquisa foi possível verificar razoável grau de inovação no âmbito da iniciativa popular por parte dos constituintes estaduais, notadamente no que diz respeito ao estabelecimento de modalidade de iniciativa inexistente em nível federal, a saber, a iniciativa popular de Emendas à Constituição. Foi possível evidenciar significativo grau de autonomia do constituinte estadual, em disposições relativas a regime prioritário ou favorecido de tramitação da espécie legislativa em questão; a criação de instituições inovadoras, como ini ciativa popular de CPI e veto popular; a previsão de referendo e plebiscito por iniciativa popular, a previsão de iniciativa popular específica em matéria orçamentária e financeira e iniciativa popular reforçada por consulta popular, entre outros aspectos.
EDUKASI KESEHATAN TENTANG RESIKO ANEMIA TERHADAP KESEHATAN REPRODUKSI REMAJA PUTRI DI GOR CANDRABAGA KOTA BEKASI TAHUN 2019
Authors: Nisa Hainun , Telaumbanua Linda , Nurmah Nurmah , Wati Puri Kresna , Akhiriyanti Evi Nur , Rupdi Rupdi 
Published: November 2020

Anemia yang dialami remaja putri akan berdampak lebih serius, mengingat mereka adalah para calon ibu yang akan hamil dan melahirkan seorang bayi, sehingga memperbesar risiko kematian ibu melahirkan, bayi lahir prematur dan berat bayi lahir rendah (BBLR). Anemia dapat dihindari dengan konsumsi makanan tinggi zat besi, asam folat, vitamin A, vitamin C dan zink, dan pemberian tablet tambah darah (TTD). Pemerintah memiliki program rutin terkait pendistribusian TTD bagi wanita usia subur (WUS), termasuk remaja dan ibu hamil.
Banyak faktor yang berhubungan dengan perilaku konsumsi makanan pada remaja, salah satunya adalah pengetahuan, Pengetahuan remaja tentang anemia defisiensi besi akan berpengaruh terhadap sikap dan perilaku remaja dalam pemilihan makanan dan selanjutnya akan berpengaruh terhadap keadaan gizi remaja termasuk status anemia defisiensi besi. Oleh karena itu diperlukan informasi masalah gizi pada remaja serta fakor-faktor yang mempengaruhinya. Informasi ini sangat berguna sebagai dasar penetapan strategi program perbaikan kesehatan dan gizi pada kelompok remaja (Mubin Halim, 2007).
Berdasarkan hal diatas, pelaksana abdimas merasa penting untuk melaksanakan kegiatan pengabdian kepada masyarakat dengan judul “edukasi kesehatan tentang resiko anemia terhadap kesehatan reproduksi remaja putri Di GOR Candrabaga Kota Bekasi tahun 2019”