Zooming in on Individual Star Formation: Low- and High-Mass Stars

Rosen, Anna L.; Offner, Stella S. R.; Sadavoy, Sarah; Bhandare, Asmita; Vázquez‐Semadeni, Enrique; Ginsburg, Adam

doi:10.1007/s11214-020-00688-5

Cited by 43 publications

(27 citation statements)

References 376 publications

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“…The development of large telescopes and highly sensitive instruments allows us to investigate star-forming regions within and even outside of the Milky Way in a great detail (for reviews, see, e.g., Larson 1981;Shu et al 1987;Kennicutt 1998;McKee & Ostriker 2007). The study of high-mass star formation (HMSF) is challenging from an observational point of view (for reviews, see, e.g., Beuther et al 2007a;Bonnell 2007;Zinnecker & Yorke 2007;Smith et al 2009;Tan et al 2014;Krumholz 2015;Schilke 2015;Motte et al 2018;Rosen et al 2020). High-mass stars are less common, located typically at large distances of several kiloparsecs and therefore difficult to observe at a high spatial resolution.…”

Section: Introductionmentioning

confidence: 99%

Physical and chemical structure of high-mass star-forming regions

Gieser

Beuther

Semenov

et al. 2021

A&A

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Section: Introductionmentioning

confidence: 99%

Physical and chemical structure of high-mass star-forming regions

Gieser

Beuther

Semenov

et al. 2021

A&A

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“…Massive stars typically form in dense, cold and large molecular clouds with one of the important signatures of massive star formation being giant filament structures and powerful bi-polar outflows when they are embedded in such dense clouds-see the recent review by Rosen et al (2020). After the formation phase, massive stars enter the so-called main sequence phase of stellar evolution, which is defined by the onset of hydrogen fusion in the core via the CNO cycle whilst maintaining hydrostatic equilibrium.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismology of High-Mass Stars: New Insights of Stellar Interiors With Space Telescopes

Bowman

2020

Front. Astron. Space Sci.

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Massive stars are important metal factories in the Universe. They have short and energetic lives, and many of them inevitably explode as a supernova and become a neutron star or black hole. In turn, the formation, evolution and explosive deaths of massive stars impact the surrounding interstellar medium and shape the evolution of their host galaxies. Yet the chemical and dynamical evolution of a massive star, including the chemical yield of the ultimate supernova and the remnant mass of the compact object, strongly depend on the interior physics of the progenitor star. We currently lack empirically calibrated prescriptions for various physical processes at work within massive stars, but this is now being remedied by asteroseismology. The study of stellar structure and evolution using stellar oscillations-asteroseismology-has undergone a revolution in the last two decades thanks to high-precision time series photometry from space telescopes. In particular, the long-term light curves provided by the MOST, CoRoT, BRITE, Kepler/K2, and TESS missions provided invaluable data sets in terms of photometric precision, duration and frequency resolution to successfully apply asteroseismology to massive stars and probe their interior physics. The observation and subsequent modeling of stellar pulsations in massive stars has revealed key missing ingredients in stellar structure and evolution models of these stars. Thus, asteroseismology has opened a new window into calibrating stellar physics within a highly degenerate part of the Hertzsprung-Russell diagram. In this review, I provide a historical overview of the progress made using ground-based and early space missions, and discuss more recent advances and breakthroughs in our understanding of massive star interiors by means of asteroseismology with modern space telescopes.

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“…The high incidence of multiple systems among the moremassive stars indicates that the angular momentum of the natal cloud is preferentially transformed into orbital motion (Larson 2010). The processes involved in massive-star formation are still the subject of active investigation (Rosen et al 2020). The turbulent core model envisions the collapse of a virial natal cloud that creates widely spaced binaries accompanied by a small number of low-mass stars formed by cloud fragmentation (Rosen et al 2019).…”

Section: Multiplicitymentioning

confidence: 99%

“…The multiplicity of massive stars must play an important role in their formation because so many are members of binary systems (Zinnecker & Yorke 2007). Massive stars are formed through the turbulent core collapse of a single cloud or by competitive accretion of multiple stellar seeds in a dense cloud (see the review by Rosen et al 2020), and models of these processes predict a large incidence of binary stars with specific distributions of mass ratio and separation (Peter et al 2012;Gravity Collaboration et al 2018). Therefore, by studying the multiplicity properties of massive stars at an early stage ,we can test the role of companions in formation theories of massive stars.…”

Section: Introductionmentioning

confidence: 99%

A High Angular Resolution Survey of Massive Stars in Cygnus OB2: JHK Adaptive Optics Results from the Gemini Near-Infrared Imager

Caballero-Nieves

Gies

Baines

et al. 2020

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We present results of a high angular resolution survey of massive OB stars in the Cygnus OB2 association that we conducted with the Near-Infrared Imager camera and ALTAIR adaptive optics system of the Gemini North telescope. We observed 74 O-and early-B-type stars in Cyg OB2 in the JHK infrared bands in order to detect binary and multiple companions. The observations are sensitive to equal-brightness pairs at separations as small as  0. 08, and progressively fainter companions are detectable out to = K 9 mag at a separation of 2″. This faint contrast limit due to read noise continues out to 10″ near the edge of the detector. We assigned a simple probability of chance alignment to each companion based upon its separation and magnitude difference from the central target star and upon areal star counts for the general star field of CygOB2. Companion stars with a field membership probability of less than 1% are assumed to be physical companions. This assessment indicates that 47% of the targets have at least one resolved companion that is probably gravitationally bound. Including known spectroscopic binaries, our sample includes 27 binary, 12 triple, and 9 systems with 4 or more components. These results confirm studies of high-mass stars in other environments that find that massive stars are born with a high-multiplicity fraction. The results are important for the placement of the stars in the Hertzsprung-Russell diagram, the interpretation of their spectroscopic analyses, and for future mass determinations through measurement of orbital motion.

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Zooming in on Individual Star Formation: Low- and High-Mass Stars

Cited by 43 publications

References 376 publications

Physical and chemical structure of high-mass star-forming regions

Physical and chemical structure of high-mass star-forming regions

Asteroseismology of High-Mass Stars: New Insights of Stellar Interiors With Space Telescopes

A High Angular Resolution Survey of Massive Stars in Cygnus OB2: JHK Adaptive Optics Results from the Gemini Near-Infrared Imager

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