Россия
УДК 53 Физика
УДК 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
УДК 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
УДК 523 Солнечная система
УДК 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
УДК 52-1 Метод изучения
УДК 52-6 Излучение и связанные с ним процессы
ГРНТИ 41.00 АСТРОНОМИЯ
ГРНТИ 29.35 Радиофизика. Физические основы электроники
ГРНТИ 29.31 Оптика
ГРНТИ 29.33 Лазерная физика
ГРНТИ 29.27 Физика плазмы
ГРНТИ 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
ОКСО 03.06.01 Физика и астрономия
ОКСО 03.05.01 Астрономия
ОКСО 03.04.03 Радиофизика
ББК 2 ЕСТЕСТВЕННЫЕ НАУКИ
ББК 223 Физика
ТБК 614 Астрономия
ТБК 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
The knowledge of systematic velocity radial profiles in the star-forming cores is important for theoretical models. We analyzed the HCO$^+$(1-0) spectral maps of five massive cores from the MALT90 database associated with the regions of high-mass star formation at different stages of evolution. We fitted the maps calculated in the framework of spherically symmetric model into observed ones. An approach based on the principal component analysis and the k-nearest neighbors method was used to find minimum of the error function between model and observed spectral maps. Radial profiles of density, turbulent and systematic velocity are obtained. Densities in the cores decrease with radial distance with power-law indices ranging from 1.5 to 2.5, turbulent velocities decrease with power-law indices ranging from 0.3 to 0.45. Systematic (infall) velocity profiles in the cores are close to $r^{-0.1}$ which differs from what is expected for free fall. Analysis of the $^{13}$CO (2-1) SEDIGISM data for three sample objects has revealed the V-shape features on the position-velocity profiles which implies motions from surrounding gas to the cores. Taken together, the results support the scenario of globally contracting cores which interact with their surroundings.
stars: formation, dense cores; methods: laboratory: molecular, modelling
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