Massive star formation via torus accretion: the effect of photoionization feedback

Autor(es)

Sartorio, N. S. ^[1] ; Vandenbroucke, B. ^[2] ; Falceta-Goncalves, D. ^{[3, 1]} ; Wood, K. ^[2] ; Keto, E. ^[4]

Afiliação do(s) autor(es)

^[1] INPE, Div Astrofisr, Av Astronautas 1-758, Sao Jose Dos Campos, SP - Brazil

^[2] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife - Scotland

^[3] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, Rua Arlindo Bettio 1000, BR-03828000 Sao Paulo, SP - Brazil

^[4] Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 - USA

• Tipo de documento: Artigo Científico
• Fonte: Monthly Notices of the Royal Astronomical Society; v. 486, n. 4, p. 5171-5183, JUL 2019.
• Citações Web of Science: 1

Resumo

The formation of massive stars is a longstanding problem. Although a number of theories of massive star formation exist, ideas appear to converge to a disc-mediated accretion scenario. Here, we present radiative hydrodynamic simulations of a star-accreting mass via a disc embedded in a torus, We use a Monte Carlo based radiation hydrodynamics code to investigate the impaci that ionizing radiation has on the torus. Ionized regions in the torus midplane are found to be either gravitationally trapped or in pressure-driven expansion depending On whether or not. the size of the ionized region exceeds a critical radius, Trapped Fin regions in the torus plane allow accretion to progress, while expanding H u regions disrupt the accretion torus preventing the central star from aggregating more mass, thereby setting the star's tinal mass. We obtain constraints for the luminosities and torus densities that lead to both scenarios. (AU)

• Processo FAPESP: 13/10559-5 - Investigação de fenômenos de altas energias e plasmas astrofísicos: teoria, simulações numéricas, observações e desenvolvimento de instrumentação para o Cherenkov Telescope Array (CTA)
• Beneficiário: Elisabete Maria de Gouveia Dal Pino
• Linha de fomento: Auxílio à Pesquisa - Temático