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The Formation of Massive Stars
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Massive stars have a profound influence on the Universe, but their formation remains poorly understood. We review the current status of observational and theoretical research in this field, describing the various stages of an evolutionary sequence that begins with cold, massive gas cores and ends with the dispersal and ionization of gas by the newly-formed star. The physical processes in massive star formation are described and related to their observational manifestations. Feedback processes and the relation of massive stars to star cluster formation are also discussed. We identify key observational and theoretical questions that future studies should address.
Forward citations
Cited by 11 Pith papers
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Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 $\mu$m Dark Massive Clumps
Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.
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Formation of massive multiple-star systems: early migration and mergers
In a simulated 1200 M_sun cluster, all massive binaries that end up with separations below 10 au pass through a circumbinary-disc phase, while repeated mergers produce extreme mass-ratio systems.
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Physical properties and gas kinematics of massive star forming region G328.24$-$0.55
ALMA data reveal five protostellar cores in G328.24 minus 0.55, with MM1a as a line-rich, hot, early-stage massive protostar that appears to drive a bipolar outflow and host a rotating envelope.
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The Young Ages of 70 {\mu}m-dark Clumps Inferred from Carbon Chain Chemistry
Carbon-chain chemistry in 11 massive 70 micron dark clumps implies chemical ages below about 1 Myr, indicating the clumps are young rather than incapable of forming high-mass stars.
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The ALMA-QUARKS Survey: Properties of Hot Molecular Fragments in the Massive Protocluster IRAS 17233-3606
ALMA resolves the hot core MM1 in IRAS 17233-3606 into 11 hot molecular fragments whose mean separation (1.8e3 au) is about half the thermal Jeans length (3.3e3 au), implying fragmentation by thermal instability and s...
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ALMAGAL IX. The chemical complexity of AG318.9477-00.1960: A line-identification template for ALMAGAL
LTE analysis of ALMA data for AG318-c9 yields molecular parameters and spatial maps for three COMs, compared to G31 as a line-identification template for the ALMAGAL survey.
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Image Profile (IMPRO) Fitting of Massive Protostars. I. Method Development and Test Cases of Cepheus A and G35.20-0.74N
Combining 1D image profile fitting along the outflow axis with SED fitting constrains the viewing angle of Cepheus A to about 34 degrees, but does not improve constraints for the poorly resolved G35.20-0.74N.
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The Chemical Clock of High-mass Star-forming Regions: N2H+/CCS
The N2H+ to CCS column density ratio increases across three evolutionary stages of high-mass star-forming regions and is proposed as a chemical clock.
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Constraining eV-scale axion-like particle dark matter: insights from the M87 Galaxy
Using M87's infrared-to-ultraviolet observations, the authors constrain the axion-photon coupling for eV-scale axion-like particle dark matter, claiming order-of-magnitude improvements over previous bounds at masses f...
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Measuring Magnetic Field Strengths in Galactic Star-forming Regions via the Zeeman Effect with the SKA
The paper presents predictions and observational plans for Zeeman effect measurements with SKA to provide statistical data on magnetic field strengths across scales in molecular clouds.
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The Impact and Environment of Massive Stars and Stellar Clusters
This review summarizes the role of massive star feedback and projects how SKA radio observations will advance studies of HII regions, stellar winds, cosmic ray acceleration, and magnetic fields.
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