kaz29Вестник Казахстанско-Британского технического университетаHerald of the Kazakh-British Technical University1998-66882959-8109Казахстанско-Британский Технический Университет10.55452/1998-6688-2025-22-2-312-321kaz29-2011Research ArticleФИЗИЧЕСКИЕ НАУКИPHYSICAL SCIENCESРАССЕЯННОЕ ЗВЕЗДНОЕ СКОПЛЕНИЕ NGC 2516: МОДЕЛИРОВАНИЕ И МНИМЫЕ НАБЛЮДЕНИЯNGC 2516 OPEN STAR CLUSTER: SIMULATIONS AND MOCK OBSERVATIONShttps://orcid.org/0000-0002-0570-7270ҚаламбайМ. Т.KalambayM. T.

PhD 

г. Актобе

г. Алматы

 PhD

Aktobe

Almaty 

 

M.Kalambay@hw.ac.ukhttps://orcid.org/0000-0003-3041-547XӨтебайА. Б.OtebayA. B.

PhD 

г. Алматы

PhD 

Almaty 

Aigerim.otebay@gmail.comhttps://orcid.org/0000-0001-8829-0556НазарА. Б.NazarA. B.

MSc 

г. Алматы

MSc 

Almaty 

nazar.aruzhan26@gmail.comhttps://orcid.org/0000-0001-6428-2084ӘсілханӘ.AssilkhanA.

MSc 

г. Нью-Йорк, США

г. Алматы

г. Актобе 

MSc 

New York, USAAlmaty

Aktobe 

a.asilhan@aues.kzhttps://orcid.org/0000-0002-4601-7065ШукиргалиевБ. Т.ShukirgaliyevB. T.

 PhD 

г. Актобе

г. Алматы 

г. Астана

PhD 

Aktobe

Almaty 

Astana

Bekdaulet.shukirgaliyev@nu.edu.kzХериот-Уатт Международный факультет, Актюбинский региональный университет им. К.Жубанова; Астрофизический институт им. В.Г. ФесенковаКазахстанHeriot-Watt International Faculty, K. Zhubanov Aktobe Regional University; Fesenkov Astrophysical InstituteKazakhstanАстрофизический институт им. В.Г. ФесенковаКазахстанFesenkov Astrophysical InstituteKazakhstanКафедра астрономии, Колумбийский университет; Кафедра астрофизики, Американский музей естественной истории; Алматинский университет энергетики и связи имени Г. Даукеева,; Актюбинский региональный университет им. К. ЖубановаКазахстанDepartment of Astronomy, Columbia University; Department of Astrophysics, American Museum of Natural History; The Gumarbek Daukeyev Almaty University of Power Engineering and Telecommunications; K. Zhubanov Aktobe Regional UniversityKazakhstanХериот-Уатт Международный факультет, Актюбинский региональный университет им. К.Жубанова; Астрофизический институт им. В.Г. Фесенкова; Энергетическая космическая лаборатория, Назарбаев Университет; Кафедра физики, Назарбаев УниверситетКазахстанHeriot-Watt International Faculty, K. Zhubanov Aktobe Regional University; Fesenkov Astrophysical Institute; Energetic Cosmos Laboratory, Nazarbayev University; Physics Department, Nazarbayev UniversityKazakhstan202506072025222312321Copyright © Қаламбай М.Т., Өтебай А.Б., Назар А.Б., Әсілхан Ә., Шукиргалиев Б.Т., 20252025Қаламбай М.Т., Өтебай А.Б., Назар А.Б., Әсілхан Ә., Шукиргалиев Б.Т.Kalambay M.T., Otebay A.B., Nazar A.B., Assilkhan A., Shukirgaliyev B.T.Данная работа распространяется под лицензией Creative Commons Attribution 4.0.This work is licensed under a Creative Commons Attribution 4.0 License.https://vestnik.kbtu.edu.kz/jour/article/view/2011

В данном исследовании изучается рассеянное звездное скопление NGC 2516 с использованием численных симуляций и сравнений с наблюдательными данными. Используя код phi-GRAPE-GPU, мы восстановили орбиту скопления за последние 123 млн лет, чтобы определить место его рождения в Галактике. Было выполнено более 70 симуляций для уточнения начальных параметров звездного скопления и их приведения в соответствие с современными наблюдениями. Анализ показал, что стандартные параметры функции масс не могут в полной мере отразить уникальные характеристики NGC 2516. В связи с этим мы скорректировали функцию масс для более точного соответствия наблюдаемым звездным свойствам. Результаты демонстрируют морфологические сходства между моделируемыми и наблюдаемыми скоплениями. Однако симуляции также включают дополнительные звезды приливных хвостов, которые отсутствуют в наблюдениях, вероятно, из-за ограничений методов наблюдений. Эти результаты подчеркивают необходимость дальнейших исследований и более глубоких сравнений. В будущих работах мы планируем использовать методы машинного обучения для более точного определения и классификации звезд приливных хвостов.

This study examines the NGC 2516 open star cluster using numerical simulations and comparisons with observational data. By employing the phi-GRAPE-GPU code, we reconstructed the cluster’s orbit over 123 Myr to identify its birthplace within the Galaxy. Over 70 simulations were conducted, refining the initial parameters of the star cluster to better match present-day observations. The analysis revealed that the standard mass function parameters could not fully replicate the unique characteristics of NGC 2516. To address this, we adjusted the mass function to align more closely with the observed stellar properties. The results demonstrate morphological similarities between the simulated and observed clusters. However, the simulations also include additional tidal tail stars that are absent in observational data, possibly due to observational limitations. These findings highlight the need for more detailed analyses and comparisons. In future studies, we plan to apply machine learning techniques to more accurately identify and classify stars in the tidal tails.

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The authors declare that there are no conflicts of interest present.