bluuebunny/crossref_metadata_2025_split huggingface dataset:
تأثير أسلوب اللعب باستعمال قناع التدريب في بعض المؤشرات الوظيفية وتحمل الاداء للاعبات كرة السلة لـ 3×3 متقدمات
Authors: سلمان حنين صفاء , رفعت لؤي سامي 
Published: February 2021

يتناول البحث أسلوب الهيبوكسيك والتي يعد من الوسائل الحديثه التدريبية نسبياً الذي تناوله الباحثانين والمدربين على حد سواء للكثير من نتائجه الايجابيه على صعيد القابليات الفسسيولوجية و البدنية للرياضيين. اراد الباحثان ومن خلال ارتداء قناع تدريب الارتفاعات والذي يحاكي كل صمام به مستوى ارتفاع معين, ان الخوض في تجربة المزج بين التدريب بالقناع مع اسلوب اللعب حتى لا تبتعد اللاعبات عن الاجواء اللعب التنافسيه. ان تجريب أفكار جديدة من شأنها رفع عجلة التطور البدني والمهاري الى الامام او اختزال الزمن المطلوب او ضعف الإمكانات المادية، ارتأ الباحثان في هذه الدراسة واختبار قدرة تحمل الاداء لدى اللاعبات اثناء أداء المباراة باستخدام أسلوب اللعب مع قناع مقاومة الهواء اثناء التنفس من اجل رفع كفاءة الأداء البدني وقدرته على التحمل اثناء الأداء من خلال الاستدلال بمستوى تراكم حامض اللاكتيك وهو بالتالي أراد الباحثان ان يدمج اللعب وتمارينه مع التمارين البدنية لرفع القدرة وكفاءة الأداء ولذلك لكون اللعبة جديدة وتحتاج الى تطوير طرق وأساليب تدريبها والقدرات المرتبطة بها وذلك لعدم الالمام بقانون هذه اللعبة الجديد. وهدف البحث الى تطوير بعض المتغيرات الوظيفية مثل النبض في الراحة، النبض بعد الجهد، وتركيز حامض اللبنيك بعد الجهد، والمتغير البدني وهو تحمل الأداء للاعبات المتقدمات بكرة السلة لـ 3×3. وأيضا الى تصميم اختبار لقياس تحمل الاداء. استخدم الباحثان المنهج التجريبي باتباع نظام المجموعتين التجريبية والضابطة وذلك لما يناسب طبيعة المشكلة البحث، اذ تكونت عينة البحث من (3 لاعبات) لكل مجموعة وتم اجراء الاختبارات المختارة عليهم في هذه الدراسة. اما تطبيق التمرينات باستخدام أسلوب اللعب بارتداء قناع التدريب فقد تمت خلال (29) وحدة تدريبية ولفتره (10) أسابيع وبواقع ثلاث وحدات تدريبة لكل أسبوع و (35 دقيقة) من القسم الرئيس أي ما يعادل 35% من مجمل اوقت الوحدة التدريبية التي تبلغ (120 دقيقة) وكانت ابرز الاستنتاجات الى ان فاعلية اسلوب اللعب باستخدام قناع التدريب في تطوير القدرات البدنية بشكل عام وتحمل الأداء بشكل خاص. ولم يكن هناك تاثير لاسلوب اللعب باستخدام قناع التدريب في تطوير تركيز حامض اللبنيك في الراحة.
تأثير تمرينات خاصة باستعمال بعض الوسائل التعليمية المساعدة في تعلم بعض المهارات الاساسية في الكرة الطائرة لطلاب الاول متوسط
Authors: خماس رعد خليل , صخي حسين سبهان 
Published: February 2021

ان استعمال التمرينات الخاصة بالوسائل التعليمية المساعدة المتطورة والتكنولوجيا والتقنيات الحديثة والتي تتماشى مع التطور الذي يشهده العالم في مجال التعلم له اهمية كبيرة في تطوير المهارات الاساسية لكرة الطائرة لطلاب المبتدئين , وجد الباحثان هناك ضعف في تعلم وقلة اهتمام في تعلم المهارات الاساسية لكرة الطائرة ومن خلال خبرة الباحث ويعمل كمدرس للتربية الرياضية ومن خلال مشاهدتها اغلب مدرسي التربية الرياضية وجد هناك ضعف وصعوبة تعلم المهارات الاساسية لكرة الطائرة , لذا ارتأى الباحثان باستعمال الوسائل التعليمية المساعدة , وكانت عينة البحث المجتمع من طلاب مديرية تربية بغداد الكرخ الثانية والبالغ عددهم ( 3200 ) طالبا للعام الدراسي 2018-2019 وتم اختيار متوسطة بلاط الشهداء للبنين الوقعة في منطقة الرسالة الاولى بالطريقة العمدية وذلك لتوفر القاعة الداخلية المخصصة للألعاب الفرقية لكرة الطائرة والسلة واليد واستخدم الباحثان المنهج التجريبي بأسلوب المجموعة الواحدة ذات الاختبار القبلي والبعدي , وتمثلت عينة البحث ب (10) طلاب من الاول متوسط , وتم تطبيق المنهج بواقع (8) اسابيع , وكانت الاستنتاجات ظهور تطور ايجابي للتمرينات الخاصة في اداء مهارتي التمرير من الاعلى والاسفل بالكرة الطائرة الذي اتبعه الباحثان , واوصى الباحثان بضرورة اجراء دراسات مشابهة على متغيرات اخرى .
تأثير تمرينات خاصة على وفق جهازHandball R.T في تطوير الاستجابة الحركية وبعض مهارات الصد لحراس المرمى في المركز الوطني لرعاية الموهبة الرياضية لكرة اليد بأعمار (15-16) سنة
Authors: كاظم الشمري محمد جبار , راضي السوداني احمد خميس 
Published: February 2021

تكمن مشكلة البحث في إن إعداد حراس المرمى يعتمد على تمرينات بأدوات تقليدية بعيدة عن استخدام التقنيات والأدوات الحديثة التي تستخدم في مجالات الاعداد العالمية ولهذا فقد لجأ الباحثان في هذه الدراسة إلى تصميم جهاز لتطوير سرعة الاستجابة الحركية الخاصة لدى حراس المرمى في كرة اليد والتي تعتبر ذات الأهمية الكبيرة في مجال حراسة المرمى التي يجب أن تؤخذ بنظر الاعتبار بهدف الارتقاء بمستوى الاداء نحو الافضل، وكانت أهداف الدراسة هي تصميم جهاز Handball R.T)) لتطوير سرعة الاستجابة الحركية الخاصة لدى حراس المرمى في كرة اليد وأعداد تمرينات لتطوير سرعة الاستجابة الحركية الخاصة وبعض مهارات الصد لحراس المرمى بكرة اليد بأعمار 15-16 سنة، ومعرفة تأثير التمرينات في تطوير سرعة الاستجابة الحركية لدى حراس المرمى بكرة اليد بأعمار 15-16 سنة. من الاستنتاجات التي توصل اليها الباحث في ضوء مناقشة النتائج التي حصل عليها من المعالجات الإحصائية أهمها ان الجهاز المصمم من قبل الباحثانHandball R.T)) لهُ تأثير إيجابي عند استخدامه في التمرينات المصممة لتطوير سرعة الاستجابة الحركية لدى عينة البحث، وفي ضوء تلك الاستنتاجات خرج الباحثان بمجموعة من التوصيات أهمها ضرورة استخدام الاجهزة والأَدوات الحديثة في تدريب حراس المرمى وذلك لتأثيرها الايجابي في تطوير المتغيرات قيد البحث ومن ثم تأثيرها على مستوى الاداء لدى حراس المرمى بكرة اليد لكافة الفئات العمرية.
تأثير تمرينات مركبة بوسائل مساعدة في تعلم مهارة التهديف من الجانب لاعبي كرة القدم للصالات باعمار (14-16) سنة
Authors: لواس نور صباح , نعمان مواهب حميد 
Published: February 2021

ارتكز هدف البحث على أعداد تمرينات مركبة بأستخدام وسائل مساعدة لمهارة الدحرجة و التهديف من الجانب للاعبي كرة القدم للصالات فئة الناشئين(14-16) سنة , وقام الباحثان باستخدام المنهج التجريبي , اما مجتمع البحث فتمثل بلاعبي نادي الحرية الرياضي ممن هم بأعمار (14-16)سنة وبالغ عددهم (20) لاعباً , وتم استخراج المعاملات الاحصائية باستخدام الحقيبة الاحصائية الجاهزة (SPSS.Ver14), وبعد ذلك استنتج الباحثان إن التمرينات المركبة بوسائل مساعدة كان لها التأثير الإيجابي في تعلم مهارة التهديف من الجانب في لعبة كرة القدم للصالات, ومن خلال ذلك اوصى الباحثان التأكيد على مدربي الاندية الرياضية باستخدام التمرينات المركبة لتعلم مهارة التهديف من الجانب في لعبة القدم للصالات.
The Young Massive Star Cluster Westerlund 2 Observed with MUSE. III. A Cluster in Motion—The Complex Internal Dynamics
Authors: Zeidler Peter , Sabbi Elena , Nota Antonella , McLeod Anna F. 
Published: February 2021

Abstract
Analyzing the dynamical state of nearby young massive star clusters is essential for understanding star cluster formation and evolution during their earliest stages. In this work we analyze the stellar and gas kinematics of the young massive star cluster Westerlund 2 (Wd2) using data from the integral field unit Multi Unit Spectroscopic Explorer (MUSE) and complement them with proper motions from the Gaia DR2. The mean gas radial velocity of 15.9 km s−1 agrees with the assumption that Wd2 is the result of a cloud–cloud collision. The gas motions show the expansion of the H ii region, driven by the radiation from the many OB stars in the cluster center. The velocity profile of the cluster member stars reveals an increasing velocity dispersion with decreasing stellar mass and that the low-mass stars show five distinct velocity groups. Based on their spatial correlation with the cluster’s two clumps, we concluded that this is the imprint of the initial cloud collapse that formed Wd2. A thorough analysis of the dynamical state of Wd2, which determines a dynamical mass range of M
dyn,Wd2 = (7.5 ± 1.9) × 104 − (4.4 ± 1.1) × 105
M
⊙ and exceeds the photometric mass by at least a factor of two, leads to the conclusion that Wd2 is not massive enough to remain gravitationally bound. Additionally we also identify 22 runaway candidates with peculiar velocities between 30 and 546 km s−1.
Threaded-field-line Model for the Low Solar Corona Powered by the Alfvén Wave Turbulence
Authors: Sokolov Igor V. , Holst Bart van der , Manchester Ward B. , Su Ozturk Doga Can , Szente Judit , Taktakishvili Aleksandre , Tóth Gábor , Jin Meng , Gombosi Tamas I. 
Published: February 2021

Abstract
We present an updated global model of the solar corona, including the transition region. We simulate the realistic three-dimensional (3D) magnetic field using the data from the photospheric magnetic field measurements and assume the magnetohydrodynamic (MHD) Alfvén wave turbulence and its nonlinear dissipation to be the only source for heating the coronal plasma and driving the solar wind. In closed-field regions, the dissipation efficiency in a balanced turbulence is enhanced. In the coronal holes, we account for a reflection of the outward-propagating waves, which is accompanied by the generation of weaker counterpropagating waves. The nonlinear cascade rate degrades in strongly imbalanced turbulence, thus resulting in colder coronal holes. The distinctive feature of the presented model is the description of the low corona as almost-steady-state low-beta plasma motion and heat flux transfer along the magnetic field lines. We trace the magnetic field lines through each grid point of the lower boundary of the global corona model, chosen at some heliocentric distance, R = R

b
∼ 1.1R
⊙, well above the transition region. One can readily solve the plasma parameters along the magnetic field line from 1D equations for the plasma motion and heat transport together with the Alfvén wave propagation, which adequately describe the physics within the heliocentric distance range R
⊙ < R < R

b
, in the low solar corona. By interfacing this threaded-field-line model with the full MHD global corona model at r = R

b
, we find the global solution and achieve a faster-than-real-time performance of the model on ∼200 cores.
GHOST: Using Only Host Galaxy Information to Accurately Associate and Distinguish Supernovae
Authors: Gagliano Alex , Narayan Gautham , Engel Andrew , Kind Matias Carrasco ,   (The LSST Dark Energy Science Collaboration)
Published: February 2021

Abstract
We present GHOST, a database of 16,175 spectroscopically classified supernovae (SNe) and the properties of their host galaxies. We have constructed GHOST using a novel host galaxy association method that employs deep postage stamps of the field surrounding a transient. Our gradient ascent method achieves fewer misassociations for low-z hosts and higher completeness for high-z hosts than previous methods. Using dimensionality reduction, we identify the host galaxy properties that distinguish SN classes. Our results suggest that the host galaxies of superluminous SNe, Type Ia SNe, and core-collapse SNe can be separated by brightness and derived extendedness measures. Next, we train a random forest model to predict SN class using only host galaxy information and the radial offset of the SN. We can distinguish Type Ia SNe and core-collapse SNe with ∼70% accuracy without any photometric or spectroscopic data from the event itself. Vera C. Rubin Observatory will usher in a new era of transient population studies, demanding improved photometric tools for rapid identification and classification of transient events. By identifying the host features with high discriminatory power, we will maintain SN sample purities and continue to identify scientifically relevant events as data volumes increase. The GHOST database and our corresponding software for associating transients with host galaxies are both publicly available through the astro_ghost package.
Far-Infrared Line Diagnostics: Improving N/O Abundance Estimates for Dusty Galaxies
Authors: Peng B. , Lamarche C. , Stacey G. J. , Nikola T. , Vishwas A. , Ferkinhoff C. , Rooney C. , Ball C. , Brisbin D. , Higdon J. , Higdon S. J. U. 
Published: February 2021

Abstract
The nitrogen-to-oxygen (N/O) abundance ratio is an important diagnostic of galaxy evolution because the ratio is closely tied to the growth of metallicity and the star formation history in galaxies. Estimates for the N/O are traditionally made with optical lines that could suffer from extinction and excitation effects, so the N/O is arguably measured better through far-infrared (far-IR) fine-structure lines. Here we show that the [N iii]57 μm/[O iii]52 μm line ratio, denoted N3O3, is a physically robust probe of N/O. This parameter is insensitive to gas temperature and only weakly dependent on electron density. Although it has a dependence on the hardness of the ionizing radiation field, we show that it is well corrected when the [Ne iii]15.5 μm/[Ne ii]12.8 μm line ratio is included. We verify the method, and characterize its intrinsic uncertainties by comparing the results to photoionization models. We then apply our method to a sample of nearby galaxies using new observations obtained with SOFIA/FIFI-LS in combination with available Herschel/PACS data, and the results are compared with optical N/O estimates. We find evidence for a systematic offset between the far-IR and optically derived N/O. We argue that the likely reason is that our far-IR method is biased toward younger and denser H ii regions, while the optical methods are biased toward older H ii regions as well as diffuse ionized gas. This work provides a local template for studies of the abundance of interstellar medium in the early Universe.
Nitrogen Dioxide Pollution as a Signature of Extraterrestrial Technology
Authors: Kopparapu Ravi , Arney Giada , Haqq-Misra Jacob , Lustig-Yaeger Jacob , Villanueva Geronimo 
Published: February 2021

Abstract
Nitrogen dioxide (NO2) on Earth today has biogenic and anthropogenic sources. During the Covid-19 pandemic, observations of global NO2 emissions have shown a significant decrease in urban areas. Drawing upon this example of NO2 as an industrial byproduct, we use a one-dimensional photochemical model and synthetic spectral generator to assess the detectability of NO2 as an atmospheric technosignature on exoplanets. We consider cases of an Earth-like planet around Sun-like, K-dwarf, and M-dwarf stars. We find that NO2 concentrations increase on planets around cooler stars because there are fewer short-wavelength photons that can photolyze NO2. In cloud-free results, present Earth-level NO2 on an Earth-like planet around a Sun-like star at 10 pc can be detected with signal-to-noise ratio ∼5 within ∼400 hr with a 15 m LUVOIR-like telescope when observed in the 0.2–0.7 μm range where NO2 has a strong absorption. However, clouds and aerosols can reduce the detectability and could mimic the NO2 feature. Historically, global NO2 levels were 3× higher, indicating the capability of detecting a civilization at the stage where Earth’s civilization was 40 yr ago. Transit and direct imaging observations to detect infrared spectral signatures of NO2 on habitable planets around M-dwarfs would need several hundred hours of observation time, both due to weaker NO2 absorption in this region and because of masking features by dominant H2O and CO2 bands in the infrared part of the spectrum. Non-detection at these levels could be used to place upper limits on the prevalence of NO2 as a technosignature.
Extremely Low Molecular Gas Content in the Vicinity of a Red Nugget Galaxy at z = 1.91
Authors: Morishita T. , D’Amato Q. , Abramson L. E. , Abdurro’uf  , Stiavelli M. , Lucas R. A. 
Published: February 2021

Abstract
We present Atacama Large Millimeter/submillimeter Array Band 5 observations of a galaxy at z = 1.91, GDS24569, in search of molecular gas in its vicinity via the [C i] 3P1–3P0 line. GDS24569 is a massive (

), passively evolving galaxy, characterized by compact morphology with an effective radius of ∼0.5 kpc. We apply two blind detection algorithms to the spectral data cubes and find no promising detection in or around GDS24569 out to a projected distance of ∼320 kpc, while a narrow tentative line (4.1σ) is identified at +1200 km s−1 by one of the algorithms. From the nondetection of [C i], we place a 3σ upper limit on molecular hydrogen mass, ∼ 7.1 × 109
M
⊙, which converts to an extremely low gas-to-stellar mass fraction of ≲ 5%. We conduct a spectral energy distribution modeling by including optical to far-infrared data and find a considerably high ( ∼ 0.1%) dust-to-stellar mass ratio, i.e., ∼10–100× higher than those of local early-type galaxies. In combination with a previous result of an insufficient number of surrounding satellite galaxies, it is suggested that GDS24569 is unlikely to experience significant size evolution via satellite mergers. We discuss possible physical mechanisms that quenched GDS24569.
Deciphering the 3D Orion Nebula. III. Structure on the NE Boundary of the Orion-S Embedded Molecular Cloud
Authors: O’Dell C. R. , Abel N. P. , Ferland G. J. 
Published: February 2021

Abstract
We have extended the work of Papers I and II of this series to determine at a higher spatial resolution the properties of the embedded Orion-S Molecular Cloud that lies within the ionized cavity of the Orion Nebula and of the thin ionized layer that lies between the Cloud and the observer. This was done using existing and new [N ii] (658.3 nm) and [O iii] (500.7 nm) spectra that map the central region of the Orion Nebula (the Huygens region). Although our observations show that the surface brightness of the ionized layer on the Orion-S Molecular Cloud and that of the nearer foreground ionized layer are linked, the process by which this is done is unclear. It is shown that the Cloud modifies the outer parts of the Huygens region in the direction of the extended hot X-ray gas.
Measurement of Absolute Single and Double Electron Capture Cross Sections for O6+ Ion Collisions with CO2, CH4, H2, and N2
Authors: Han J. , Wei L. , Wang B. , Ren B. , Yu W. , Zhang Y. , Zou Y. , Chen L. , Xiao J. , Wei B. 
Published: February 2021

Abstract
The absolute electron capture cross sections for single and double charge exchanges (CEs) between the highly charged ion O6+ and CO2, CH4, H2, and N2, the dominant collision processes in the solar wind, have been measured in the energies from 7 keV · q (2.63 keV u−1) to 52 keV · q (19.5 keV u−1). These measurements were carried out in the new experimental instrument setup at Fudan University, and the errors of the cross sections for single and double CEs at the 1σ confidence level were about 11% and 16%, respectively. Limited agreement is achieved with single electron capture results calculated by the classical overbarrier model. These cross section data are useful for the simulation of ion–neutral processes in astrophysical environments and to improve the present theoretical model of fundamental atomic processes.
ALMA Reveals a Cloud–Cloud Collision that Triggers Star Formation in the Small Magellanic Cloud
Authors: Neelamkodan Naslim , Tokuda Kazuki , Barman Susmita , Kondo Hiroshi , Sano Hidetoshi , Onishi Toshikazu 
Published: February 2021

Abstract
We present the results of Atacama Large Millimeter/submillimeter Array observations in 12CO(1–0) emission at 0.58 × 0.52 pc2 resolution toward the brightest H ii region N66 of the Small Magellanic Cloud (SMC). The 12CO(1–0) emission toward the north of N66 reveals clumpy filaments with multiple velocity components. Our analysis shows that a blueshifted filament at a velocity range of 154.4–158.6 km s−1 interacts with a redshifted filament at a velocity of 158.0–161.8 km s−1. A third velocity component at a velocity range of 161–165.0 km s−1 constitutes hub-filaments. An intermediate-mass young stellar object (YSO) and a young pre-main-sequence star cluster have hitherto been reported in the intersection of these filaments. We find a V-shape distribution in the position–velocity diagram at the intersection of two filaments. This indicates the physical association of those filaments due to a cloud–cloud collision. We determine the collision timescale ∼0.2 Myr using the relative velocity (∼5.1 km s−1) and displacement (∼1.1 pc) of those interacting filaments. These results suggest that the event occurred about 0.2 Myr ago and triggered the star formation, possibly an intermediate-mass YSO. We report the first observational evidence for a cloud–cloud collision that triggers star formation in N66N of the low metallicity ∼0.2 Z
⊙ galaxy, the SMC, with similar kinematics as in N159W-South and N159E of the Large Magellanic Cloud.
Eight Blue E+A Galaxy Candidates Located inside a Large-scale Filament in the Coma Cluster
Authors: Ostling William , Wurmser Serena , Kerrison Nicole , Liu Charles 
Published: February 2021

Abstract
E+A galaxies are post-starburst galaxies that have recently undergone quenching of their star formation, making them a valuable source for studying the evolution of galaxies. Using the SDSS Data Release 16, we found 13 “blue” E+A galaxy candidates and 117 “green” E+A galaxy candidates in and around the Coma cluster of galaxies. Blue E+A galaxies tend to be younger than green E+A galaxies, giving us a picture of how young galaxies transform into E+A galaxies. Based on their positions in R.A./decl./velocity space, we found that 8 of the blue E+A galaxy candidates seem to be located inside a large-scale galactic filament emanating from the center of the Coma Cluster. Their locations suggest there is an unusually high number of E+A galaxies throughout the filament. We have not yet determined whether these E+A galaxy candidates formed through merging or ram pressure stripping.
The Correlated Response of the Narrow FeKα Emission Line to the Primary Continuum Changes in the Seyfert Galaxy NGC 2992
Authors: Ghosh Ritesh , Pal Main 
Published: February 2021

Abstract
The intensely varying Active Galactic nucleus (AGN) NGC 2992, on timescales of days to years, provides us with a unique testbed to study the response of the narrow FeKα emission line to the changes in the primary 2–10  keV AGN continuum. We find a strong correlation between the narrow FeKα line flux and the 2–10  keV flux with a Spearman correlation coefficient s = 0.70 and probability p < 0.001, over a period of ∼20 yr. There is no evidence of such a correlation in <1 yr, but the FeKα flux responds at ∼3 yr timescales, allowing us to put the reprocessor distance scale to 0.3 pc ≤ d ≤ 1 pc, consistent with that of torus reflection. The primary 2–10  keV continuum of NGC 2992 undergoes a high-low-high transition in ∼16 yr (2003–2019). Future long term monitoring will be crucial.
Elaboração de iogurte com adição de aveia e linhaça dourada
Authors: De Carvalho Gabriela Nantes , Morato Priscila Neder , Benedetti Silvia 
Published: February 2021

O iogurte é um alimento obtido através da coagulação e diminuição do pH do leite, através da fermentação láctea mediante a ação proto-simbiótica de Lactobacillus delbrueckii ssp. Bulgaricus e Streptococcus salivarius ssp. thermophilus. O presente trabalho teve como objetivo a elaboração, avaliação físico-química, microbiológica e sensorial de iogurtes com adição de aveia e linhaça dourada. Foram elaboradas três formulações: sem adição de aveia e linhaça dourada (Padrão), com adição de 1% de aveia e 1% linhaça dourada (A1) e outra com adição de 3% de aveia e 3% de linhaça dourada (A2). Foram realizadas análises físico-químicas de umidade, cinzas, lipídeos, proteínas, pH, sólidos totais, acidez titulável e fibra alimentar total. Também foram realizadas análises microbiológicas de coliformes a 35 °C e coliformes a 45 °C; e teste sensorial de aceitabilidade, utilizando escala hedônica de 9 pontos, com avaliação dos atributos cor, sabor, odor, textura e impressão global. Comparando os resultados físico-químicos das formulações, pode-se observar que a formulação A2 apresentou conteúdos significativamente maiores de proteínas, lipídeos e cinzas. Os resultados das análises microbiológicas mostraram que nenhuma das formulações apresentou contagem superior ao limite estabelecido pela legislação vigente. Na análise sensorial pode-se observar diferença significativa entre as formulações apenas para o atributo cor. Embora a formulação A1 tenha recebido melhores notas na avaliação sensorial, não pode ser classificada como fonte de fibra alimentar, conforme é estabelecido na RDC nº 54, de 12 de novembro de 2012, podendo-se considerar que A1 como um produto apenas enriquecido com fibras. Dessa forma, a adição de aveia e farinha de linhaça mostrou-se uma boa alternativa para adição em iogurte.