Пожалуйста, используйте этот идентификатор, чтобы цитировать или ссылаться на этот ресурс:
http://elar.urfu.ru/handle/10995/103144
Название: | Parameter study for the burst mode of accretion in massive star formation |
Авторы: | Meyer, D. M. -A. Vorobyov, E. I. Elbakyan, V. G. Eislöffel, J. Sobolev, A. M. Stöhr, M. |
Дата публикации: | 2021 |
Издатель: | Oxford University Press |
Библиографическое описание: | Parameter study for the burst mode of accretion in massive star formation / D. M. -A. Meyer, E. I. Vorobyov, V. G. Elbakyan, et al. — DOI 10.1093/mnras/staa3528 // Monthly Notices of the Royal Astronomical Society. — 2021. — Vol. 500. — Iss. 4. — P. 4448-4468. |
Аннотация: | It is now a widely held view that, in their formation and early evolution, stars build up mass in bursts. The burst mode of star formation scenario proposes that the stars grow in mass via episodic accretion of fragments migrating from their gravitationally unstable circumstellar discs, and it naturally explains the existence of observed pre-main-sequence bursts from high-mass protostars. We present a parameter study of hydrodynamical models of massive young stellar objects (MYSOs) that explores the initial masses of the collapsing clouds (Mc = 60-200 Modot) and ratio of rotational-to-gravitational energies (β = 0.005-0.33). An increase in Mc and/or β produces protostellar accretion discs that are more prone to develop gravitational instability and to experience bursts. We find that all MYSOs have bursts even if their pre-stellar core is such that β ≤ 0.01. Within our assumptions, the lack of stable discs is therefore a major difference between low- and high-mass star formation mechanisms. All our disc masses and disc-to-star mass ratios Md/M⊙ > 1 scale as a power law with the stellar mass. Our results confirm that massive protostars accrete about 40, -, 60 percent of their mass in the burst mode. The distribution of time periods between two consecutive bursts is bimodal: there is a short duration (∼ 1, -, 10 yr) peak corresponding to the short, faintest bursts and a long-duration peak (at ∼ 103 104 yr) corresponding to the long, FU-Orionis-type bursts appearing in later disc evolution, i.e. around 30 kyr after disc formation. We discuss this bimodality in the context of the structure of massive protostellar jets as potential signatures of accretion burst history. © 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. |
Ключевые слова: | METHODS: NUMERICAL STARS: CIRCUMSTELLAR MATTER STARS: EVOLUTION STARS: FLARE |
URI: | http://elar.urfu.ru/handle/10995/103144 |
Условия доступа: | info:eu-repo/semantics/openAccess |
Идентификатор РИНЦ: | 44994567 |
Идентификатор SCOPUS: | 85099693270 |
Идентификатор WOS: | 000606297700013 |
Идентификатор PURE: | 20515472 d7f4e63f-65b4-4bd8-8462-0bd3e7f78f6e |
ISSN: | 358711 |
DOI: | 10.1093/mnras/staa3528 |
Располагается в коллекциях: | Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC |
Файлы этого ресурса:
Файл | Описание | Размер | Формат | |
---|---|---|---|---|
2-s2.0-85099693270.pdf | 3,3 MB | Adobe PDF | Просмотреть/Открыть |
Все ресурсы в архиве электронных ресурсов защищены авторским правом, все права сохранены.