bluuebunny/crossref_metadata_2025_split huggingface dataset:
ARI SÜTÜNÜN YAPISI, İNSANLAR VE ARILAR İÇİN ÖNEMİ
Authors: Akyol Ethem 
Published: May 2018

Türkiye gerek florası
gerekse koloni varlığı
ile iyi bir
arıcılık potansiyeline sahiptir. Arılar hem bitkilerin tozlaşmalarını sağlamaları hem de ürünleri ile insanlar için büyük bir öneme sahiptirler. Arı sütü 6-15 günlük yaştaki işçi arıların kafalarındaki hypopharyngeal ve mandibular salgı bezlerinden salgıladıkları, ana arı ve genç larvaları besledikleri, beyaz-krem renginde, besin değeri çok yüksek kıvamlı bir gıda maddesidir. İşçi arılar ana arı ve genç larvaları arı sütü ile beslerler. Ana arı ile işçi arılar arasında genetiksel olarak hiç bir farklılık yoktur. Diploit
larvalar; 3 günlük
yaştan sonra nektar- bal ve polen karışımı ile beslenirse işçi, arı sütü ile beslenirse ana arı olarak gelişir. Ana arılar 3-4 yıl işçi arılar ise 6-7 hafta kadar yaşarlar. İşçi arılar dişi olmasına rağmen yumurtalıkları gelişmemiştir ve yumurtlamazlar Kraliçe arıların yumurtalıkları mükemmel bir şekilde gelişmiştir ve günde 1500-2000 yumurta yumurtlarlar. Ana
arı daha iri yapılı
olmasına rağmen gelişmesini
16 günde, işçi arılar ise 21 günde tamamlarlar. İşçi ve ana arı arasındaki tüm bu farklılıkların yegane nedeni beslenme farklılıklarıdır. Arı sütünün arılar üzerindeki bu müthiş etkileri nedeniyle insanlar da kullanmaya başlamışlar ve kullanımı her geçen gün hızla yaygınlaşmaktadır.
Peynirin Raf Ömrünü Uzatmada Bal Mumu Kaplamaların Kullanılması
Authors: GULDAS Metin 
Published: May 2018

Peynir besin bileşeni bakımından konsantre ve tüketimi yaygın olan bir süt ürünüdür. Farklı peynir çeşitlerinin farklı tüketici gruplarının damak zevklerini karşılayabilmesi yanında protein ve madensel maddeler (özellikle kalsiyum ve fosfor) bakımından zengin içeriği tüketici talebini arttıran nedenler olarak sıralanabilir. Peynirin fiziksel, biyokimyasal ve mikrobiyolojik bozulmalara hassas bir gıda olup kolay bozulabilmesi; mikrobiyolojik
açıdan güvenliği arttırmak, raf ömrü ve dayanımı uzatmak için yenilikçi muhafaza yöntemlerinin geliştirilmesine yol açmıştır. Paketleme, gıda maddelerinin farklı amaçlarla tüketime sunulmasına,&nbsp; farklı boyut ve şekillerde korunmasına
olanak veren bir işlemdir. Bazı yapay ambalaj maddeleri tüketici sağlığına zarar verebilmekte ve doğada kolay parçalanmadığından çevre kirliliğine yolaçmaktadır. Bu nedenlerle alternatif ambalaj maddeleri arayışına gidilmiş, kalite kayıplarını azaltmak
ve muhafaza amacıyla yenebilir film kaplamalar geliştirilmiştir. Yenebilir kaplama filmleri; tüketimi güvenli, ucuz&nbsp;
ve üretim teknolojisi basit, dış etkenlere (yağ, nem, O2 ve CO2); biyokimyasal, fizikokimyasal ve mikrobiyolojik bozulmaları dayanıklı olmalıdır. Bunların yanında yenebilir filmlere renk, aroma, besin öğeleri, antioksidant ve antimikrobiyal maddeler de katılabilmektedir. Bu derleme makalede özellikle bal mumu başta olmak üzere; yenebilir film kaplamaların peynirin raf ömrünü arttırmada kullanılabilirliği ele alınmaya çalışılmıştır.
THE EFFECTS OF DIFFERENT POLLEN TRAPPING PERIODS AND INTERVALS ON AMOUNT OF POLLEN AND NUMBER OF POLLEN COLLECTING WORKER HONEYBEES (APIS MELLIFERA L.)
Authors: AKYOL Ethem , NALAN Adnan U 
Published: May 2018

Bu çalışma balarısı(Apis mellifera anatoliaca) kolonilerine değişik aralıklarla polen tuzağı takmanın
işçi arıların polen toplama aktiviteleri ve koloninin polen verimine etkisini belirlemek amacıyla
yürütülmüştür. Günlük ortalama en fazla polen’i (75.20±9.12 gr/gün/koloni) her gün tuzak takılı olan I.
Grup koloniler toplarken, bir gün ara ile tuzak takılan II. Grup (40.35±3.15 gr/gün/koloni) ve üç gün ara
ile tuzak takılan III. Grup (37.23±3.45 gr/gün/koloni) koloniler ise daha az polen toplamışlar ve aynı
istatistiki grupta yer almışlardır. Günün değişik saatlerinde polen yükü ile gelen arı sayıları
bakımından hem gruplar hem de saatler arasındaki farklılık istatistiki olarak önemli
bulunmuştur(P&lt;0.01). Tüm gruplardaki koloniler en fazla poleni saat 7:00 (165.81±15.8 adet/10
dakika/koloni) ve 9:00(177.39±20.06 adet/10 dakika/koloni) saatlerinde toplamışlar, en az poleni ise
15:00(19.52±1.68 adet/10 dakika/koloni) saatlerinde topladıkları belirlenmiştir.
Driving Solar Giant Cells through the Self-organization of Near-surface Plumes
Authors: Nelson Nicholas J. , Featherstone Nicholas A. , Miesch Mark S. , Toomre Juri 
Published: May 2018

AbstractGlobal 3D simulations of solar giant-cell convection have provided significant insight into the processes which yield the Sun’s observed differential rotation and cyclic dynamo action. However, as we move to higher-resolution simulations a variety of codes have encountered what has been termed the convection conundrum. As these simulations increase in resolution and hence the level of turbulence achieved, they tend to produce weak or even anti-solar differential rotation patterns associated with a weak rotational influence (high Rossby number) due to large convective velocities. One potential culprit for this convection conundrum is the upper boundary condition applied in most simulations, which is generally impenetrable. Here we present an alternative stochastic plume boundary condition which imposes small-scale convective plumes designed to mimic near-surface convective downflows, thus allowing convection to carry the majority of the outward solar energy flux up to and through our simulated upper boundary. The use of a plume boundary condition leads to significant changes in the convective driving realized in the simulated domain and thus to the convective energy transport, the dominant scale of the convective enthalpy flux, and the relative strength of the strongest downflows, the downflow network, and the convective upflows. These changes are present even far from the upper boundary layer. Additionally, we demonstrate that, in spite of significant changes, giant cell morphology in the convective patterns is still achieved with self-organization of the imposed boundary plumes into downflow lanes, cellular patterns, and even rotationally aligned banana cells in equatorial regions. This plume boundary presents an alternative pathway for 3D global convection simulations where driving is non-local and may provide a new approach toward addressing the convection conundrum.
Chemical Composition of Two Bright, Extremely Metal-poor Stars from the SDSS MARVELS Pre-survey
Authors: Bandyopadhyay Avrajit , Sivarani Thirupathi , Susmitha Antony , Beers Timothy C. , Giridhar Sunetra , Surya Arun , Masseron Thomas 
Published: May 2018

Abstract
SDSS J082625.70+612515.10 (V = 11.4; [Fe/H] = −3.1) and SDSS J134144.60+474128.90 (V = 12.4; [Fe/H] = −3.2) were observed with the SDSS 2.5m telescope as part of the SDSS MARVELS spectroscopic pre-survey and identified as extremely metal-poor (EMP; [Fe/H] < −3.0) stars during the high-resolution follow-up using the Hanle Echelle Spectrograph (HESP) on the 2.0-m Himalayan Chandra Telescope. In this paper, the first science results using HESP, we present a detailed analysis of their chemical abundances. Both stars exhibit under-abundances in their neutron capture elements, while one of them (SDSS J134144.60+474128.90) is clearly enhanced in carbon. Lithium was also detected in this star at a level of about A(Li) = 1.95. The spectra were obtained over a span of 6–24 months, and indicate that both stars could be members of binary systems. We compare the elemental abundances derived for these two stars along with other carbon-enhanced metal-poor (CEMP) and EMP stars, in order to understand the nature of their parent supernovae. We find that CEMP-no stars and EMP-dwarfs show a very similar trend in their lithium abundances at various metallicities. We also find indications of CEMP-no stars having larger abundances of Cr and Co at given metallicities compared to EMP stars.
Two Episodes of Magnetic Reconnections during a Confined Circular-ribbon Flare
Authors: Li Ting , Yang Shuhong , Zhang Qingmin , Hou Yijun , Zhang Jun 
Published: May 2018

Abstract
We analyze a unique event with an M1.8 confined circular-ribbon flare on 2016 February 13, with successive formations of two circular ribbons at the same location. The flare had two distinct phases of UV and extreme ultraviolet emissions with an interval of about 270 s, of which the second peak was energetically more important. The first episode was accompanied by the eruption of a mini-filament and the fast elongation motion of a thin circular ribbon (CR1) along the counterclockwise direction at a speed of about 220 km s−1. Two elongated spine-related ribbons were also observed, with the inner ribbon co-temporal with CR1 and the remote brightenings forming ∼20 s later. In the second episode, another mini-filament erupted and formed a blowout jet. The second circular ribbon and two spine-related ribbons showed similar elongation motions with that during the first episode. The extrapolated three-dimensional coronal magnetic fields reveal the existence of a fan-spine topology, together with a quasi-separatrix layer (QSL) halo surrounding the fan plane and another QSL structure outlining the inner spine. We suggest that continuous null-point reconnection between the filament and ambient open field occurs in each episode, leading to the sequential opening of the filament and significant shifts of the fan plane footprint. For the first time, we propose a compound eruption model of circular-ribbon flares consisting of two sets of successively formed ribbons and eruptions of multiple filaments in a fan-spine-type magnetic configuration.
The Frequency of Intrinsic X-Ray Weakness among Broad Absorption Line Quasars
Authors: Liu Hezhen , Luo B. , Brandt W. N. , Gallagher S. C. , Garmire G. P. 
Published: May 2018

Abstract
We present combined ≈14–37 ks Chandra observations of seven z = 1.6–2.7 broad absorption line (BAL) quasars selected from the Large Bright Quasar Survey (LBQS). These seven objects are high-ionization BAL (HiBAL) quasars, and they were undetected in the Chandra hard band (2–8 keV) in previous observations. The stacking analyses of previous Chandra observations suggested that these seven objects likely contain some candidates for intrinsically X-ray weak BAL quasars. With the new Chandra observations, six targets are detected. We calculate their effective power-law photon indices and hard-band flux weakness, and find that two objects, LBQS 1203+1530 and LBQS 1442–0011, show soft/steep spectral shapes (

and

) and significant X-ray weakness in the hard band (by factors of ≈15 and 12). We conclude that the two HiBAL quasars are good candidates for intrinsically X-ray weak BAL quasars. The mid-infrared-to-ultraviolet spectral energy distributions of the two candidates are consistent with those of typical quasars. We constrain the fraction of intrinsically X-ray weak active galactic nuclei (AGNs) among HiBAL quasars to be ≈7%–10% (2/29–3/29), and we estimate it is ≈6%–23% (2/35–8/35) among the general BAL quasar population. Such a fraction is considerably larger than that among non-BAL quasars, and we suggest that intrinsically X-ray weak quasars are preferentially observed as BAL quasars. Intrinsically X-ray weak AGNs likely comprise a small minority of the luminous type 1 AGN population, and they should not affect significantly the completeness of these AGNs found in deep X-ray surveys.
Motions in Prominence Barbs Observed on the Solar Limb
Authors: Kucera T. A. , Ofman L. , Tarbell T. D. 
Published: May 2018

Abstract
We analyze and discuss an example of prominence barbs observed on the limb on 2016 January 7 by the Hinode/Solar Optical Telescope in Ca ii and Hα, the Interface Region Imaging Spectrograph, with slit jaw images and Mg ii spectral data, and the Solar Dynamics Observatory’s Atmospheric Imaging Assembly. In the recent literature there has been a debate concerning whether these features, sometimes referred to as “tornadoes,” are rotating. Our data analysis provides no evidence for systematic rotation in the barbs. We do find line-of-sight motions in the barbs that vary with location and time. We also discuss observations of features moving along the barbs. These moving features are elongated parallel to the solar limb and tend to come in clusters of features moving along the same or similar paths in the plane of the sky during a period of 10 minutes to an hour, moving toward or away from the limb. The motion may have a component along the line of sight as well. The spectral data indicate that the features are Doppler shifted. We discuss possible explanations for these features.
In Situ Observations of Harmonic Alfvén Waves and Associated Heavy Ion Heating
Authors: Chen Huayue , Gao Xinliang , Lu Quanming , Wang Shui 
Published: May 2018

Abstract
Resonant ion heating by high-frequency Alfvén waves has long been believed to be the primary dissipation mechanism for solar coronal heating, and these high-frequency Alfvén waves are considered to be generated via cascade from low-frequency Alfvén waves. In this study, we report an unusual harmonic Alfvén event from in situ observations by the Van Allen Probes in the magnetosphere, having an environment similar to that in the solar corona. The harmonic Alfvén waves, which propagate almost along the wave vector of the fundamental waves, are considered to be generated due to the interaction between quasi-parallel Alfvén waves and plasma density fluctuations with almost identical frequency. These high-frequency harmonic Alfvén waves can then cyclotron resonantly heat the heavy ions. Our observations provide an important insight into solar corona heating by Alfvén waves.
Planet-driven Spiral Arms in Protoplanetary Disks. II. Implications
Authors: Bae Jaehan , Zhu Zhaohuan 
Published: May 2018

Abstract
We examine whether various characteristics of planet-driven spiral arms can be used to constrain the masses of unseen planets and their positions within their disks. By carrying out two-dimensional hydrodynamic simulations varying planet mass and disk gas temperature, we find that a larger number of spiral arms form with a smaller planet mass and a lower disk temperature. A planet excites two or more spiral arms interior to its orbit for a range of disk temperatures characterized by the disk aspect ratio

, whereas exterior to a planet’s orbit multiple spiral arms can form only in cold disks with

. Constraining the planet mass with the pitch angle of spiral arms requires accurate disk temperature measurements that might be challenging even with ALMA. However, the property that the pitch angle of planet-driven spiral arms decreases away from the planet can be a powerful diagnostic to determine whether the planet is located interior or exterior to the observed spirals. The arm-to-arm separations increase as a function of planet mass, consistent with previous studies; however, the exact slope depends on disk temperature as well as the radial location where the arm-to-arm separations are measured. We apply these diagnostics to the spiral arms seen in MWC 758 and Elias 2–27. As shown in Bae et al., planet-driven spiral arms can create concentric rings and gaps, which can produce a more dominant observable signature than spiral arms under certain circumstances. We discuss the observability of planet-driven spiral arms versus rings and gaps.
The Circumstellar Disk and Asymmetric Outflow of the EX Lup Outburst System
Authors: Hales A. S. , Pérez S. , Saito M. , Pinte C. , Knee L. B. G. , Gregorio-Monsalvo I. de , Dent B. , López C. , Plunkett A. , Cortés P. , Corder S. , Cieza L. 
Published: May 2018

Abstract
We present Atacama Large Millimeter/submillimeter Array (ALMA) observations at 0.″3 resolution of EX Lup, the prototype of the EXor class of outbursting pre-main-sequence stars. The circumstellar disk of EX Lup is resolved for the first time in 1.3 mm continuum emission and in the J = 2–1 spectral line of three isotopologues of CO. At the spatial resolution and sensitivity achieved, the compact dust continuum disk shows no indications of clumps, fragments, or asymmetries above the 5σ level. Radiative transfer modeling constrains the characteristic radius of the dust disk to 23 au and the total dust mass to 1.0 × 10−4
M
⊙ (33 M
⊕), similar to other EXor sources. The 13CO and C18O line emissions trace the disk rotation and are used to constrain the disk geometry, kinematics, and a total gas disk mass of 5.1 × 10−4
M
⊙. The 12CO emission extends out to a radius of 200 au and is asymmetric, with one side deviating from Keplerian rotation. We detect blueshifted, 12CO arc-like emission located 0.″8 to the northwest and spatially disconnected from the disk emission. We interpret this extended structure as the brightened walls of a cavity excavated by an outflow, which are more commonly seen in FUor sources. Such outflows have also been seen in the borderline FU/EXor object V1647 Ori, but not toward EXor objects. Our detection provides evidence that the outflow phenomenon persists into the EXor phase, suggesting that FUor and EXor objects are a continuous population in which outflow activity declines with age, with transitional objects such as EX Lup and V1647 Ori.
The Origin of the Relation between Metallicity and Size in Star-forming Galaxies
Authors: Almeida J. Sánchez , Vecchia C. Dalla 
Published: May 2018

Abstract
For the same stellar mass, physically smaller star-forming galaxies are also metal richer. What causes the relation remains unclear. The central star-forming galaxies in the EAGLE cosmological numerical simulation reproduce the observed trend. We use them to explore the origin of the relation assuming that the physical mechanism responsible for the anticorrelation between size and gas-phase metallicity is the same in the simulated and the observed galaxies. We consider the three most likely causes: (1) metal-poor gas inflows feeding the star formation (SF) process, (2) metal-rich gas outflows particularly efficient in shallow gravitational potentials, and (3) enhanced efficiency of the SF process in compact galaxies. Outflows (cause 2) and enhanced SF efficiency (cause 3) can be discarded. Metal-poor gas inflows (cause 1) produce the correlation in the simulated galaxies. Galaxies grow in size with time, so those that receive gas later are both metal poorer and larger, giving rise to the observed anticorrelation. As expected within this explanation, larger galaxies have younger stellar populations. We explore the variation with redshift of the relation, which is maintained up to, at least, redshift 8.
Extended Millimeter Emission in the HD 141569 Circumstellar Disk Detected with ALMA
Authors: White Jacob Aaron , Boley A. C. 
Published: May 2018

Abstract
We present archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of the HD 141569 circumstellar disk at 345, 230, and 100 GHz. These data detect extended millimeter emission that is exterior to the inner disk. We find through simultaneous visibility modeling of all three data sets that the system’s morphology is described well by a two-component disk model. The inner disk ranges from approximately 16–45 au with a spectral index of 1.81 (q = 2.95), and the outer disk ranges from 95 to 300 au with a spectral index of 2.28 (q = 3.21). Azimuthally averaged radial emission profiles derived from the continuum images at each frequency show potential emission that is consistent with the visibility modeling. The analysis presented here shows that at ∼5 Myr, HD 141569's grain size distribution is steeper and therefore possibly more evolved in the outer disk than in the inner disk.
Gemini/GMOS Spectroscopy of Globular Clusters in the Merger Remnant Galaxy M85
Authors: Ko Youkyung , Lee Myung Gyoon , Park Hong Soo , Sohn Jubee , Lim Sungsoon , Hwang Narae 
Published: May 2018

Abstract
M85 is a peculiar S0 galaxy in Virgo and a well-known merger remnant. We present the first spectroscopic study of globular clusters (GCs) in M85. We obtain spectra for 21 GC candidates and the nucleus of M85 using the Gemini Multi-Object Spectrograph on the Gemini North 8.1 m telescope. From their radial velocities, 20 of the GCs are found to be members of M85. We find a strong rotation signal of the M85 GC system with a rotation amplitude of 235 km s−1. The rotation axis of the GC system has a position angle of about 161°, which is 51.°5 larger than that of the stellar light. The rotation-corrected radial velocity dispersion of the GC system is estimated to be

km s−1. The rotation parameter

of the GC system is derived to be

, which is one of the largest among known early-type galaxies. The ages and metallicities of the GCs, which show the same trend as the results based on Lick indices, are derived from full spectrum fitting (ULySS). About half of the GCs are an intermediate-age population whose mean age is ∼3.7 ± 1.9 Gyr, having a mean [Fe/H] value of −0.26. The other half are old and metal-poor. These results suggest that M85 experienced a wet merging event about 4 Gyr ago, forming a significant population of star clusters. The strong rotational feature of the GC system can be explained by an off-center major merging.
The Importance of the 13C(α,n)16O Reaction in Asymptotic Giant Branch Stars
Authors: Cristallo S. , Cognata M. La , Massimi C. , Best A. , Palmerini S. , Straniero O. , Trippella O. , Busso M. , Ciani G. F. , Mingrone F. , Piersanti L. , Vescovi D. 
Published: May 2018

Abstract
Low-mass asymptotic giant branch stars are among the most important polluters of the interstellar medium. In their interiors, the main component (A ≳ 90) of the slow neutron capture process (the s-process) is synthesized, the most important neutron source being the 13C(α,n)16O reaction. In this paper, we review its current experimental status, discussing possible future synergies between some experiments currently focused on the determination of its rate. Moreover, in order to determine the level of precision needed to fully characterize this reaction, we present a theoretical sensitivity study, carried out with the FUNS evolutionary stellar code and the NEWTON post-process code. We modify the rate up to a factor of 2 with respect to a reference case. We find that variations of the 13C(α,n)16O rate do not appreciably affect s-process distributions for masses above 3 M
⊙ at any metallicity. Apart from a few isotopes, in fact, the differences are always below 5%. The situation is completely different if some 13C burns in a convective environment: this occurs in FUNS models with M < 3 M
⊙ at solar-like metallicities. In this case, a change of the 13C(α,n)16O reaction rate leads to nonnegligible variations of the element surface distribution (10% on average), with larger peaks for some elements (such as rubidium) and neutron-rich isotopes (such as 86Kr and 96Zr). Larger variations are found in low-mass, low-metallicity models if protons are mixed and burned at very high temperatures. In this case, the surface abundances of the heavier elements may vary by more than a factor of 50.