Supershells and propagating star formation

McCray, Richard; Kafatos, M.

doi:10.1086/165267

Cited by 411 publications

(422 citation statements)

References 12 publications

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“…The star formation activity results in some hierarchical structure with both spatial and temporal correlations (see, e.g., Elmegreen 2011b), which is important for ISM ecology and evolution (McCray and Kafatos 1987, Mac Low and McCray 1988, Norman and Ikeuchi 1989, Heiles 1990. Young massive SF regions are often clumped Lada and Lada (2003), Portegies Zwart et al (2010).…”

Section: Star Formation In the Milky Way And Other Galaxiesmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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Section: Star Formation In the Milky Way And Other Galaxiesmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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“…In the standard approach based on the Weaver et al (1977) model, H i shells result from the cumulative action of multiple stellar winds and supernovae explosions (see e.g. McCray & Kafatos 1987;Tenorio-Tagle & Bodenheimer 1988;Ott et al 2001). However, it was recognized long ago (see, e.g., Tenorio-Tagle & Bodenheimer 1988;Rhode et al 1999;Kim et al 1999;Simpson at al.…”

Section: Introductionmentioning

confidence: 99%

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Egorov¹,

Lozinskaya²,

Моисеев³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We analyse the ionized gas kinematics in the star formation regions of the supergiant shell (SGS) of the IC 2574 galaxy using observations with the Fabry-Perot interferometer at the 6-m telescope of SAO RAS; the data of the THINGS survey are used to analyze the neutral gas kinematics in the area. We perform the 'derotation' of the Hα and H i data cubes and show its efficiency in kinematics analysis. We confirm the SGS expansion velocity 25 km s −1 obtained by Walter & Brinks (1999) and conclude that the SGS is located at the far side of the galactic disc plane. We determine the expansion velocities, kinematic ages, and the required mechanical energy input rates for four star formation complexes in the walls of the SGS; for the remaining ones we give the limiting values of the above parameters. A comparison with the age and energy input of the complexes' stellar population shows that sufficient energy is fed to all H ii regions except one. We discuss in detail the possible nature of this region and that of another one, which was believed to be an SNR according to radio observations. We measured the expansion velocity of the latter and confirm its identification as an old SNR. Our observations allowed us to identify a faint diffuse Hα emission inside the SGS which was never observed before.

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“…Such a supershell can persist for periods longer than 10 6 yr (McCray and Kafatos 1987), and among other things, could possibly trigger further star formation. Saken et al (1992) discuss such a supershell surrounding Cygnus OBI with dimensions 26 by 65 pc.…”

Section: Star Formation: Coeval Sequential or Contemporaneous?mentioning

confidence: 99%

OB associations: Massive stars in context

Garmany¹

1994

PASP

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ABSTRACT. Massive stars are important in a variety of contexts: individually they are examples of stars that undergo significant mass loss which is driven by line radiation pressure; as denizens of the Galaxy they play a significant role in the galactic recycling effort; as ensembles of stars they contain clues to massive star evolution in general and the question of supernova progenitors in particular. Finally, under extreme conditions of pathological star formation massive stars participate in the star burst phenomena seen in some galaxies. If we wish to understand star bursts, we must first understand locally observed variations in the mass spectrum. But all of these diverse areas of study rely on certain fundamental parameters of the stars themselves-here we include temperature, luminosity, mass, and chemical composition. And central to accurate determinations of these parameters are the distances to the stars. This review will focus on what is known about the loose clustering of massive stars termed OB associations. These associations contain many, but by no means all, of the stars with masses greater than 15Mq. Most of our knowledge of the stellar content of the OB associations in our own Galaxy is surprisingly sketchy due to their large angular size, but large-field CCD detectors are changing this. Magellanic Cloud associations can now be compared with OB associations in our own Galaxy, and the initial mass function shows surprising variations. The physical cause of these variations is still unknown. Another development is the study of embedded star clusters: infrared array detectors have been probing the buried stars in molecular clouds and finding an unexpectedly large population of these objects. Both these young IR clusters, and a sprinkling of evolved red supergiants, suggest that the star-formation history of OB associations may be more complicated than we have supposed.

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Supershells and propagating star formation

Cited by 411 publications

References 12 publications

Nonthermal particles and photons in starburst regions and superbubbles

Nonthermal particles and photons in starburst regions and superbubbles

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

OB associations: Massive stars in context

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