The development of bio-derived composites represents a sustainable and cost-effective strategy for advanced energy storage applications. In this work, a porous carbon/nickel oxide (NiO) composite was synthesized from orange peel via carbonization at 500 °C followed by KOH activation at 700 °C and subsequent hydrothermal NiO modification. The resulting material exhibited a hierarchical porous structure with a high specific surface area (2120 m² g⁻¹ for OP_500_700 and 1968 m² g⁻¹ for NiO-modified OP_500_700_0.1M), with both values being significantly higher than that of the non-activated OP_500 (3.40–18.12 m² g⁻¹). Electrochemical evaluation revealed that the NiO-functionalized composite achieved a specific capacitance of 306.0 F g⁻¹ at 5 mV s⁻¹ and 281.5 F g⁻¹ at 2 A g⁻¹, surpassing the pristine activated carbon (281.9 F g⁻¹ and 259.6 F g⁻¹, respectively). In addition, both electrodes demonstrated excellent cycling stability, retaining more than 80% capacitance after 5000 charge–discharge cycles at a high current density of 20 A g⁻¹, while the NiO-modified electrode further benefited from a self-activation effect leading to >100% retention. These findings emphasize the synergistic effects of hierarchical porosity and NiO pseudocapacitance, establishing orange peel-derived carbon/NiO composites as scalable and sustainable electrode materials for next-generation supercapacitors.

We present high-angular resolution observations, conducted with the Atacama Large Millimeter/Submillimeter Array (ALMA) in Band 6, of high-excitation molecular lines of ${\mathrm{CH}}_3\mathrm{CN}$, CH₃OH, and the H29$\alpha$ radio recombination line, towards the G333.6-0.2 ultracompact (UC) H ii region. Our observations reveal three hot molecular cores: A, B, and C, where emission is detected in ten components of the $J=14\to 13$ rotational ladder of ${\mathrm{CH}}_3\mathrm{CN}$ and in the CH₃OH $J=5_{1,4}\to 4_{1,3}$ transition. Rotational diagram analysis of ${\mathrm{CH}}_3\mathrm{CN}$ reveals excitation temperatures ranging from 380 to 430 K. First-order moment maps of ${\mathrm{CH}}_3\mathrm{CN}$ and CH₃OH reveal distinct velocity gradients in all cores, suggesting rotating structures, with core A also showing evidence of expansion motions. The H29$\alpha$ recombination line shows a linewidth of $30.2\pm 0.12$ km s⁻¹, dominated by dynamical and thermal broadening, indicative of large-scale motions in ionized gas. Analysis of the ionized gas properties yields an electron density of $(4.8\pm 0.4)\times {10}^5$ cm⁻³, an emission measure of $(1.23\pm 0.06)\times {10}^9$ pc cm⁻⁶, and a Lyman continuum photon flux consistent with an O5–O6 V (Zero-Age Main Sequence; ZAMS) star. Our results suggest that G333.6-0.2 is in an intermediate evolutionary stage between hypercompact (HC) and ultracompact (UC) H ii regions, hosting active high-mass star formation with rotating hot cores and ionized gas dynamics.

Over the past decade, the most important observations of the interstellar medium have been made in the infrared and radio regions of electromagnetic radiation. Of particular interest were GLIMPSE (Galactic Legacy Infrared Midplane Survey Extraordinaire), MIPSGAL and WISE (Wide-field Infrared Survey Explorer) surveys of several areas of star formation. Distinctive features of the infrared view of the Galactic disk at wavelengths from 3.4 μm to 22 μm include regions of ionized hydrogen HII, infrared bubbles, young stellar objects, massive star formation, infrared dark clouds, diffuse dust, include hydrocarbons and radiation from millions of stars. Based on current literature, infrared signatures in hot regions around young massive stars have been identified as dust bubbles, so in this paper, the regions around bubble N10, one of the northern infrared bubbles included in Churchwell's catalog, were investigated. Using archival data from the WISE and 2MASS catalogs, we searched for candidates for young stellar objects around the N10 dust bubble and found 117 emission objects. Koenig et al. (2014) plotted diagrams of their color indices and energy distribution in the spectrum for each studied object under different classification conditions. According to the results of studies around the infrared dust bubble N10, objects at an early stage of evolution were discovered: 13 objects are young class I stars and 13 objects are young class II stars, 3 objects are classified as transitional disks. За последнее десятилетие важнейшие наблюдения межзвездной среды выполнены в инфракрасном и радиодиапазонах электромагнитного излучения. Особый интерес представляли обзоры GLIMPSE (экстраординарный инфракрасный обзор срединной плоскости галактики), MIPSGAL и WISE (Wide-field Infrared Survey Explorer) нескольких областей звездообразования. Отличительные особенности инфракрасного изображения галактического диска на длинах волн от 3,4 мкм до 22 мкм включают области ионизированного водорода HII, инфракрасные пузыри, молодые звездные объекты, массивное звездообразование, инфракрасные темные облака, диффузную пыль, включают углеводороды и излучение миллионов звезды. Основываясь на современной литературе, инфракрасные сигнатуры в горячих областях вокруг молодых массивных звезд были идентифицированы как пылевые пузыри, поэтому в этой статье были исследованы области вокруг пузыря N10, одного из северных инфракрасных пузырей, включенных в каталог Черчвелла. Используя архивные данные из каталогов WISE и 2MASS, мы провели поиск кандидатов в молодые звездные объекты вокруг пылевого пузыря N10 и нашли 117 эмиссионных объектов. Кениг и др. (2014) построили графики их показателей цвета и распределения энергии в спектре для каждого исследуемого объекта при разных условиях классификации. По результатам исследований вокруг инфракрасного пылевого пузыря N10 были обнаружены объекты, находящиеся на ранней стадии эволюции: 13 объектов — молодые звезды I класса и 13 объектов — молодые звезды II класса, 3 объекта относятся к категории переходных дисков. Соңғы онжылдық ішінде жұлдызаралық ортадағы ең маңызды бақылаулар электромагниттік сәулеленудің инфрақызыл және радио аймақтарында жасалды. Жұлдыздардың түзілуінің бірнеше бағыттары бойынша GLIMPSE (Galactic Legacy Infrared Midplane Survey Extraordinaire), MIPSGAL және WISE (Wide-field Infrared Survey Explorer) барлаулары ерекше қызығушылық тудырды. 3,4 мкм-ден 22 мкм-ге дейінгі толқын ұзындығындағы Галактикалық дискінің инфрақызыл көрінісінің ерекше белгілеріне иондалған сутегі аймақтары HII, инфрақызыл көпіршіктер, жас жұлдыздар объектілері, жұлдыздардың жаппай түзілуі, инфрақызыл қара бұлттар, диффуздық шаң, көмірсутектер мен миллиондаған жұлдыздардың сәулеленуін жатқызуға болады. Заманауи әдебиеттерге талдау жасау арқылы жас массивті жұлдыздардың айналасындағы қыздырылған аймақтардағы инфрақызыл белгілер шаң көпіршіктер екені анықталды, сол себепті бұл жұмыста Churchwell каталогына енгізілген солтүстік инфрақызыл көпіршіктердің бірі – N10...

In recent years, the researchof bubbles,partially circular structures in the interstellar medium, consisting of dust and gas, has received the considerable attention. The analysis of the structure and evolution of bubbles provides insight into the conditions under which stars and planets form inthe interstellar medium. Dust bubbles are inextricably linked with star formation regions and are powerful tools for studying the interaction of young stellar objects with their environment at various stages of evolution.The main goal of this articleisto study the region of the N126 dust bubble, search for and identify young stellar objects. Identification of young stellar objects by their fluxes at infrared wavelengths is relatively recent, and identification criteria are still at the stage of improvement. Therefore, in this article, the criteria for identifying young stellar objects were used according to the works of Koenig X.P. (2012), Koenig X.P. & Leisawitz D.V. (2014) and Fischer W.J. (2016), which are based on analysis of WISE observational datain the near-and mid-infrared bands W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm), and W4 (22 μm). The datafrom the 2MASS and AllWISE catalogswith reliable non-zero fluxes of infrared radiation sourceswere used in that work. For the researched dust bubble, young stellar objects of class 0 (protostars) and class I were not detected. 4 objects of class II, 1 object of the class of transition disks and 48 objects of class III were identified. Energy distributions in the spectra for class II objectswere constructed, which also confirmed their evolutionary status. For all identified YSOs, color diagrams were constructed showing the locations of the found objects with their corresponding areas of evolution. Maps of the distribution of YSOs in space are analyzed, which indicate possible signs of an initiated star formation process in the N126 dust bubble.

HII regions are ionized regions of interstellar gas, which ionized by intensive ultraviolet radiation from nearby hot stars. Radio recombination line is one of the main tools for investigating the HII region, in particular, the distribution of HII is obtained and the main physical conditions of the interstellar matter are determined from hydrogen lines. This study was carried out based on the analysis of the H110a recombination emission line toward the W40 HII region, which is one of the most active star-forming regions in the Aquila Molecular Cloud. We used archival observational data of the H110a radio recombination line in the Aquila Molecular Cloud, obtained during February in 2015 using the 26m NanShan radiotelescope in the Xinjiang Astronomical Observatory of the Chinese Academy of Sciences. During the period of the study, an integrated intensity map of H110a toward the W40 HII region and the corresponding spectra were constructed. The electron density and temperature of the HII region, the emission measure, the optical thickness, the Lyman continuum flux, the excitation parameter, the radius of the Strömgren sphere, and the mass of ionized hydrogen inside the sphere were calculated. The values of the emission measure and optical thickness indicate that the H110a recombination radio line is optically thin and traces a very dense region (<6462 AU) with a high electron temperature. The numbers of photons of the Lyman continuum indicates the presence of a massive O9.5 star, that equivalent to a zero-age main-sequence star located within the HII region. The obtained values of the physical parameters indicate that the region of ionized hydrogen under study is an ultracompact region. The results of this article lay the foundation for further research aimed at studying the evolution of HII regions, as well as their role in the processes of starformation. Области HII - это ионизированные области межзвездного газа, которые были ионизированы интенсивным ультрафиолетовым излучением близлежащих горячих звезд. Для изучения области НІІ одним из основных инструментов являются радиорекомбинационные линии, в частности по линиям водорода получают распределение НІІ и определяют основные физические условия межзвездной среды. Данное исследование проведено на основе анализа рекомбинационной линии излучения H110a в направлении региона W40 НІІ, который является одним из самых активных областей звездообразования в молекулярном облаке Aquila. Для проведения данного исследования нами были использованы архивные данные наблюдений радиорекомбинационной линии Н110a в молекулярном облаке Aquila, полученные в течение февраля 2015 года на 26-м радиотелескопе Нань-Шань Синьцзянской астрономической обсерватории Китайской академии наук. В ходе исследования построена карта интегральной интенсивности излучения H110a в направлении области W40 НІІ и соответствующие спектры. В исследовании были определены электронная плотность и температура региона НІІ, мера эмиссии, оптическая толщина, поток лаймановского континуума, параметр возбуждения, радиус сферы Стремгрена и масса ионизированного водорода внутри сферы. Значения меры эмиссии и оптической толщины указывают на то, что рекомбинационная радиолиния H110a оптически тонкая и прослеживает очень плотную область (<6462 а.е.) с высокой электронной температурой. Число фотонов континуума Лаймана показывает наличие массивной звезды типа О9.5, эквивалентной звезде главной последовательности нулевого возраста, расположенной внутри области HII. Полученные значения физических параметров указывают на то, что исследуемая область ионизированного водорода является ультракомпактной областью. Результаты проведенного исследования закладывают основу для дальнейших исследований, направленных на изучение природы и эволюции областей HII, а также их роли в более широком контексте в процессах звездообразования. HII аймақтары – жақын маңдағы ыстық жұлдыздардың қарқынды ультракүлгін сәулеленуімен иондалған жұлдызаралық газдың иондалған аймақтары. HII аймағын зерттеу үшін радиорекомбинациялық сызықтар негізгі құралдардың бірі болып табылады, атап...

The study of young stellar objects is one of the priority areas in modern astrophysics, since these objects serve as key indicators of the processes accompanying the formation of stars and planetary systems. In the process of evolution, especially in the conditions of massive star clusters, they generate intense ultraviolet radiation and stellar winds that are capable to scatter the surrounding matter and forming expanding cavities that are infrared bubble structures in molecular clouds. The study of these structures allows us to obtain valuable information about the mechanisms of interaction of stars with their surrounding environment at various stages of evolutionary development. The aim of this work is to study the region of the dust bubble N22 in order to identify and classify young stellar objects. The main observational material was data obtained by the Wide-Field Infrared Survey Explorer space telescope in the near and mid-infrared range: W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm), and W4 (22 μm). As a result of the analysis, new candidates for young stellar objects were identified within the studied region: 15 objects belonging to class I, 7 objects - class II, and 13 objects demonstrating the characteristics of transition disks. For all selected candidates for young stellar objects, color diagrams were constructed displaying their position relative to the characteristic regions of the evolutionary stages of young stars. In addition, spectral indices were calculated and the energy distribution in the spectrum was modeled, which confirmed the classification of objects by evolutionary stages.