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.

The study of young stellar objects is one of the key studies in astrophysics, as these objects provide a unique window into the processes that occur during the formation of stars and planets. Young stars are often found in clouds of gas and dust, which serve as a kind of "cradle" for their birth. Young stars, especially in massive star clusters, create powerful streams of wind and radiation that knock out dust and gas, creating ring structures, those as bubbles in molecular clouds. Analysis of such structures can provide additional clues about the strength of the interactions between stars and their environment at different stages of their evolution. The main objective of this study was to study the N1 dust bubble region and search for and identify young stellar objects. Searching for young stellar objects (YSOs) using infrared data from astronomical catalogs is an important and effective method for studying star formation. Young stars and their surroundings are often hidden from visible-light observations by dense clouds of gas and dust, but infrared radiation can penetrate these clouds, allowing astronomers to find objects that would otherwise be invisible. The identification of young stellar objects in this study was performed according to the algorithm of Koenig & Leisawitz (2014). The observational data of the WISE spacecraft in the near and mid-infrared bands W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm) and W4 (22 μm) were used. Reliable non-zero fluxes of infrared radiation sources from the 2MASS and AllWISE catalogs were selected for the study. For the studied dust bubble, 7 objects of class I and 11 objects of class II were identified, 32 objects were assigned to the transition disk stage. For all identified young stellar objects, color diagrams were constructed showing the locations of the found objects with the corresponding evolutionary regions. Spectral indexes were calculated and energy distributions in the spectra were constructed for young stellar objects, which also confirmed their evolutionary status. The distribution maps of early-stage YSOs within the dust bubble are analyzed, which indicate the patterns of their distribution along filamentary structures in the dust bubble N1.

Experimental studies of estimation the mutual influence of humidity and flux of cosmic rays in first approximation were carried out. Normalized cross-correlation function of time series of neutron monitors count rate and level of relative atmosphere humidity near cosmic rays registration point is studied. Corrected and uncorrected on pressure minute and hour data of 6NM64 neutron monitor count rate were used for the study. Neutron monitor is located in Al-Farabi Kazakh National University, at an altitude of 850 m above sea level. Also, data from NM64 neutron monitor of Tien Shan mountain research station of Institute of Ionosphere, located at an altitude of 3340 m above sea level were used. Uncorrected on pressure cosmic rays intensity better reflects the changes in relative atmosphere humidity. Average and sometimes strong relationship is often observed by time changes of atmosphere humidity near the point of cosmic rays detection and their intensity: the value of normalized cross-correlation function of respective signals, even in case of their long duration and a large number of data (eg, for minute changes at intervals of up to several months) covers 0.5 - 0.75 range, sometimes falling to ~⃒ 0.4.