Massive Star Formation Triggered by Collision between Galactic and Accreted Intergalactic Clouds

Wang, Jun Jie; Chen, Wen-Ping; Miller, M.; Qin, Sheng; Wu, Yue

doi:10.1086/425657

Cited by 14 publications

(11 citation statements)

References 21 publications

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“…While the magnetic breakout model is found to be consistent with most observations, alternative models with emerging flux and small-scale reconnection in the chromosphere -35were found to explain some surge-CME events (Liu et al 2005d). The newly emerging flux that triggers a CME often emerges with an opposite sign in the helicity than that of the pre-existing active region (Wang et al 2004).…”

Section: Magnetic Field Configuration Of Cmesmentioning

confidence: 99%

Astrophysics in 2005

Trimble

Aschwanden

Hansen

2006

PUBL ASTRON SOC PAC

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ABSTRACT. We bring you, as usual, the Sun and Moon and stars, plus some galaxies and a new section on astrobiology. Some highlights are short (the newly identified class of gamma-ray bursts, and the Deep Impact on Comet 9P/Tempel 1), some long (the age of the universe, which will be found to have the Earth at its center), and a few metonymic, for instance the term "down-sizing" to describe the evolution of star formation rates with redshift.

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Section: Magnetic Field Configuration Of Cmesmentioning

confidence: 99%

Astrophysics in 2005

Trimble

Aschwanden

Hansen

2006

PUBL ASTRON SOC PAC

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“…The Interstellar Medium (ISM) is a complex ensemble of gas, large molecules and dust coupled through the action of the magnetic fields permeating the Galaxy. In some parts of the Galaxy, molecular clouds are formed due to galactic stresses (Elmegreen (1990); Franco et al (2002)) or eventual accretion from the intergalactic medium (Mirabel (1982); Wang et al (2004)). In the outskirts of these clouds the dust size distribution varies due to density gradients that determine the characteristics of the stars that will be formed inside them (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Interstellar extinction in Orion. Variation of the strength of the UV bump across the complex

Beitia-Antero,

de Castro

2017

Preprint

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There is growing observational evidence of dust coagulation in the dense filaments within molecular clouds. Infrared observations show that the dust grains size distribution gets shallower and the relative fraction of small to large dust grains decreases as the local density increases. Ultraviolet (UV) observations show that the strength of the 2175 Å feature, the so-called UV bump, also decreases with cloud density. In this work, we apply the technique developed for the Taurus study to the Orion molecular cloud and confirm that the UV bump decreases over the densest cores of the cloud as well as in the heavily UV irradiated λ Orionis shell. The study has been extended to the Rosette cloud with uncertain results given the distance (1.3 kpc).

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“…Indeed, collisions between neutral molecular clouds are frequently mentioned as a possible mechanism for initiating the star formation process. For instance, based on observed carbon molecular lines, [2] suggested that the formation of the stars in the IRAS04000 + 5052 cluster was induced by the collision of two molecular clouds.…”

Section: Introductionmentioning

confidence: 99%

Simulations of Colliding Uniform Density H2 Clouds

Arreaga‐García

Klapp²,

Morales

2014

IJAA

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In this paper we present a set of numerical simulations designed to study the interaction process of H II molecular clouds. For the initial conditions we assume head-on and oblique collisions of binary identical clouds placed adjacent to one another, with their surfaces just in contact. The colliding initial clouds are uniform density molecular gas spheres with rigid body rotation. The cloud initial conditions are chosen to favor its gravitational collapse as an isolated system. To study the effect of the self-gravity of the cloud in the collision process, we consider several models in which the approaching speed of the colliding clouds increases from zero up to several times the initial sound speed of the barotropic gas. We present the outcome of these collision models for several values of the impact parameter b, which depends on the initial radius of the cloud. We have explored the parameter space of the approaching velocity Vapp of the colliding clouds for configurations that may result in seeds for the formation of more complex systems. Such systems are expected to include filaments and gas clumps, where the star formation process is still possible despite the occurrence of the collision. We show hereby that collisions may have a major and favorable influence on the star formation process.

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Massive Star Formation Triggered by Collision between Galactic and Accreted Intergalactic Clouds

Cited by 14 publications

References 21 publications

Astrophysics in 2005

Astrophysics in 2005

Interstellar extinction in Orion. Variation of the strength of the UV bump across the complex

Simulations of Colliding Uniform Density H2 Clouds

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