The Formation of Massive Stars

Bonnell, Ian A.; Smith, Rowan J.

doi:10.1017/s1743921311000184

Cited by 13 publications

(15 citation statements)

References 60 publications

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“…Our discovery of low-mass cores within the accretion reservoir of forming massive stars is consistent with the predictions of competitive accretion-style cluster formation models, in which a cluster environment is required to form high-mass stars (e.g. Bonnell & Smith 2011). The evidence from our ALMA and SMA observations that in G11.92−0.61 high-mass and low-mass stars are forming simultaneouslye.g., are accreting at the same time, from the same clump-scale gas reservoir, as they approach their final massesfurther supports dynamic cluster formation models in which high-mass stars form concurrently with their surrounding clusters.…”

Section: Discussionsupporting

confidence: 87%

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Simultaneous low- and high-mass star formation in a massive protocluster: ALMA observations of G11.92−0.61★

Cyganowski

Brogan

Hunter

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present 1.05 mm ALMA observations of the deeply embedded high-mass protocluster G11.92−0.61, designed to search for low-mass cores within the accretion reservoir of the massive protostars. Our ALMA mosaic, which covers an extent of ∼0.7 pc at sub-arcsecond (∼1400 au) resolution, reveals a rich population of 16 new millimetre continuum sources surrounding the three previously-known millimetre cores. Most of the new sources are located in the outer reaches of the accretion reservoir: the median projected separation from the central, massive (proto)star MM1 is ∼0.17 pc. The derived physical properties of the new millimetre continuum sources are consistent with those of low-mass prestellar and protostellar cores in nearby star-forming regions: the median mass, radius, and density of the new sources are 1.3 M ⊙ , 1600 au, and n H2 ∼10 7 cm −3 . At least three of the low-mass cores in G11.92−0.61 drive molecular outflows, traced by high-velocity 12 CO(3-2) (observed with the SMA) and/or by H 2 CO and CH 3 OH emission (observed with ALMA). This finding, combined with the known outflow/accretion activity of MM1, indicates that high-and low-mass stars are forming (accreting) simultaneously within this protocluster. Our ALMA results are consistent with the predictions of competitive-accretion-type models in which high-mass stars form along with their surrounding clusters.

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Section: Discussionsupporting

confidence: 87%

“…In contrast, competitive accretion-type models require that highmass stars form in a cluster environment (e.g. Bonnell et al 2004;Bonnell & Smith 2011). In cluster-scale models, including those that incorporate (proto)stellar feedback (e.g.…”

mentioning

confidence: 99%

Simultaneous low- and high-mass star formation in a massive protocluster: ALMA observations of G11.92−0.61★

Cyganowski

Brogan

Hunter

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The first one takes advantage of the fact that high-mass stars always form as members of stellar clusters. If the central density in the cluster is high enough, there is a chance that low-mass protostars collide and so successively build up more massive objects (Bonnell et al, 1998). As the radii of protostars usually are considerably larger than the radii of main sequence stars in the same mass range (Hosokawa & Omukai, 2009), this could be a viable option.…”

Section: Massive Star Formationmentioning

confidence: 99%

Physical Processes in the Interstellar Medium

Klessen

Glover

2015

Star Formation in Galaxy Evolution: Connecting Numerical Models to Reality

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Interstellar space is filled with a dilute mixture of charged particles, atoms, molecules and dust grains, called the interstellar medium (ISM). Understanding its physical properties and dynamical behavior is of pivotal importance to many areas of astronomy and astrophysics. Galaxy formation and evolution, the formation of stars, cosmic nucleosynthesis, the origin of large complex, prebiotic molecules and the abundance, structure and growth of dust grains which constitute the fundamental building blocks of planets, all these processes are intimately coupled to the physics of the interstellar medium. However, despite its importance, its structure and evolution is still not fully understood. Observations reveal that the interstellar medium is highly turbulent, consists of different chemical phases, and is characterized by complex structure on all resolvable spatial and temporal scales. Our current numerical and theoretical models describe it as a strongly coupled system that is far from equilibrium and where the different components are intricately linked together by complex feedback loops. Describing the interstellar medium is truly a multi-scale and multi-physics problem. In these lecture notes we introduce the microphysics necessary to better understand the interstellar medium. We review the relations between large-scale and small-scale dynamics, we consider turbulence as one of the key drivers of galactic evolution, and we review the physical processes that lead to the formation of dense molecular clouds and that govern stellar birth in their interior.

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“…O modelo de coalescência, proposto por Bonnell et al (1998) surgiu como um cenário alternativo para a formação desses objetos.…”

Section: Coalescência De Estrelas De Baixa Massaunclassified

“…Resumidamente, o cenário de coalescência proposto por Bonnell et al (1998) Galáxia e seu númeroé insuficiente para explicar a origem de todas as estrelas de alta massa conhecidas.…”

Section: Coalescência De Estrelas De Baixa Massaunclassified

Procura de Estrelas de Alta Massa em Formação

Navarete¹

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Aos meus pais, Donizeti e Lidia, com todo o meu amor e gratidão. AgradecimentosA elaboração deste trabalho não teria sido possível sem a colaboração, estímulo e empenho de diversas pessoas. Gostaria de expressar minha gratidão a todos aqueles que contribuíram para que esta tarefa se tornasse uma realidade. A todos, aqui citados ou não, quero manifestar os meus sinceros agradecimentos.Aos meus pais, Donizeti e Lidia, pelo amor, carinho e as lições de vida que recebi ao longo de toda a minha existência. Palavras não são capazes de expressar a minha eterna gratidão e, a eles dedico este trabalho.Ao meu orientador, Prof. Dr. Augusto Damineli, pela oportunidade de trabalhar com um tema encantador, por sua paciência, amizade e imprescindível orientação acadêmica.Ao meu relator, Prof. Dr. Marcos Diaz, pelas suas críticas construtivas e sugestões.Aos professores Dr. Cássio Leandro, Dr. Francisco Jablonski, Dr. Gabriel Hickel e Dr.Alessandro Moisés, pelos ensinamentos e discussões durante a realização deste trabalho.Aos colegas do IAG, em especial ao Mairan Teodoro, Marcus Duarte, Bruno Quint, Diana Gama, Márcio Avellar, Paulo Jakson, Fellipy Silva, Bruno Mota, Oscar Cavicha, Pedro Beaklini, Tiago Ricci, Leonardo Almeida, Rafael Santucci, Luciene Coelho; pelas conversas, risadas, os cafés (principalmente os cafés!) e aventuras que enfrentamos juntos ao longo desses anos. Um agradecimento especialà equipe técnica e administrativa do Depto. de Astronomia, que contribuíram para o andamento deste trabalho.Aos queridos colegas do IQ-USP: Erich Tahara, Cleverson Busso, Ariel Cardoso, Bruno Queliconi, Bruno Chausse, Camille Caldeira, Fernanda Cunha, Fernanda Cerqueira, Graciele Oliveira, Maynara Fornazari, Phillipe Pessoa; que acompanharam de perto o meu primeiro contato com a ciência e sempre foram meus exemplos de grandes pessoas e pesquisadores. Não poderia deixar de agradecerà Prof a . Dr a . Alicia J. Kowaltowski, por guiar meus primeiros passos na pesquisa acadêmica e por todo o incentivo e disposição em orientar um físico "perdido" no fascinante universo das mitocôndrias.Aos companheiros de república Marco Antônio, Paulo Bianchi e Jonathan Sena; pela amizade, companheirismo e pelo apoio nas horas mais difíceis. Aos amigos, de longe e de perto: André Teruya, Adriano Campanhola, Cecilia Garcia, Mario Ageu, Natália Monteiro e Vitor Aguiar. Ao meu querido professor do ensino médio, Máximo A. Faggian, que me incentivou desde muito cedo a seguir na Astronomia. Agradeçoà Marcela, que esteve ao meu lado nos momentos mais difíceis e decisivos deste trabalho, sendo tão companheira e carinhosa. parcialmente baseado em observações obtidas pelo telescópio SOAR, um projeto conjunto do Ministério da Ciência, Tecnologia, e Inovação (Brasil), National Optical Astronomy Observatory (Estados Unidos), Universidade da Carolina do Norte (Estados Unidos), e Universidade de Michigan (Estados Unidos). A los amigos deEsta dissertação foi escrita em L A T E X com a classe IAGTESE, para teses e dissertações do IAG."Mesmo que a rota da minha vida me...

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The Formation of Massive Stars

Cited by 13 publications

References 60 publications

Simultaneous low- and high-mass star formation in a massive protocluster: ALMA observations of G11.92−0.61★

Simultaneous low- and high-mass star formation in a massive protocluster: ALMA observations of G11.92−0.61★

Physical Processes in the Interstellar Medium

Procura de Estrelas de Alta Massa em Formação

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