3D Simulation of Interstellar Cloud Collision and Triggered Star Formation

1987 ◽  
pp. 438-440
Author(s):  
Mikio Nagasawa ◽  
Shoken M. Miyama
Keyword(s):  
Star Formation ◽  
Interstellar Cloud ◽  
3D Simulation

Star formation in a galactic cluster

1979 ◽  
Vol 291 (1380) ◽  
pp. 219-252 ◽  
Keyword(s):  
Angular Momentum ◽  
Star Formation ◽  
Differential Equations ◽  
Theoretical Prediction ◽  
Massive Stars ◽  
Planetary Systems ◽  
Interstellar Cloud ◽  
Dissipation Of Energy ◽  
Galactic Cluster ◽  
The Masses

A model has been developed for the collapse of an interstellar cloud with turbulence. The differential equations which describe the evolution of the cloud include ionic and dust cooling and also the dissipation of energy due to the collision of turbulent elements moving at supersonic speeds. Under some conditions the collision of two elements can give rise to a star and the rate of star formation and the mass of the stars formed changes as the cloud collapses. The pattern found is that the stars first produced have masses of about 1.4 M . and the masses get less as star formation continues. Stars produced by this mechanism have little associated angular momentum. Some of the stars which happen to move in high density regions of the cloud may increase their mass greatly by accretion; these stars will be the more massive stars and they will also rotate most rapidly, a theoretical prediction which agrees with observation. On the basis of the model the proportion of stars which would have planetary systems is estimated. This shows that there should be of order 10 6 planetary systems per galaxy.

The Role of Grain Motions in Star Formation

1977 ◽  
Vol 3 (2) ◽  
pp. 168-169
Author(s):  
M. J. KrautSChneider
Keyword(s):  
Star Formation ◽  
Magnetic Fields ◽  
Interstellar Cloud ◽  
Centre Of Mass ◽  
Thermal Pressure ◽  
Gas Cloud ◽  
Number Of Authors

A number of authors (Reddish, 1968, 1969, Reddish and Wickramasinghe 1969) have stressed the importance for star formation of the role of condensation of H2, onto solid grains inside the cool dark regions of a large interstellar cloud. However, although the thermodynamic consequences of the existence of grains have been extensively studied, the dynamical implications have received little attention. Solid grains of course do not possess a thermal pressure as their gaseous counterpart does, neither do they directly experience the magnetic fields which thread the ions and electrons of the gas cloud. The grains therefore, as soon as they are formed, are free to fall toward their common centre of mass, relatively unrestricted by the constraints on the gas cloud.

scholarly journals Tracing the Interstellar Medium in Ophiuchus Across 14 Orders of Magnitude in Frequency

1998 ◽  
Vol 179 ◽  
pp. 175-176
Author(s):  
S.W. Digel ◽  
S.D. Hunter ◽  
S.L. Snowden
Keyword(s):  
Star Formation ◽  
Interstellar Medium ◽  
Spectral Range ◽  
Angular Size ◽  
Interstellar Cloud ◽  
Galactic Emission ◽  
Cloud Complex ◽  
Extended Emission ◽  
Complex Well

The spectral range of ground and space-based observations has expanded rapidly in recent years. Essentially complete sky coverage is available in bands spanning more than 14 orders of magnitude in frequency, with varying sensitivities and resolutions. Remarkably, extended emission (and absorption) associated with the interstellar medium can be seen across this range. This poster illustrated the range of information now at hand for just a single interstellar cloud complex, that in Ophiuchus. This complex, well known for its abundant on-going star formation, is relatively nearby (∼125 pc), and well removed from the plane, offering the advantages of large angular size and little confusion in most bands from background Galactic emission.

scholarly journals 3D Simulation of Interstellar Cloud Collision and Triggered Star Formation

1987 ◽  
Vol 115 ◽  
pp. 438-440
Author(s):  
Mikio Nagasawa ◽  
Shoken M. Miyama
Keyword(s):  
Star Formation ◽  
Critical Mass ◽  
Three Dimensional ◽  
Particle Method ◽  
Initial Distribution ◽  
Interstellar Cloud ◽  
Three Dimensions ◽  
Interstellar Clouds ◽  
Smoothed Particle ◽  
Hydrodynamic Code

Cloud-cloud collision has been regarded as one of the important mechanisms which triggers star formation. But a detailed analysis on the change of the critical mass has been absent due to the poor resolution of numerical experiments or limited by the assumption of a geometrical symmetry. We simulate the collisions between isothermal interstellar clouds using a three-dimensional hydrodynamic code (Smoothed Particle Method). The simulation in three dimensions gives us not only the criterion for the trigger of star formation but also the information about the origin of the interstellar cloud rotation and its initial distribution of angular momentum.

Supernovae and interstellar gas dynamics

1967 ◽  
Vol 31 ◽  
pp. 117-119
Author(s):  
F. D. Kahn ◽  
L. Woltjer
Keyword(s):  
Lower Limit ◽  
High Velocity ◽  
Gas Dynamics ◽  
Interstellar Cloud ◽  
Interstellar Gas ◽  
Random Motions ◽  
Relativistic Particles

The efficiency of the transfer of energy from supernovae into interstellar cloud motions is investigated. A lower limit of about 0·002 is obtained, but values near 0·01 are more likely. Taking all uncertainties in the theory and observations into account, the energy per supernova, in the form of relativistic particles or high-velocity matter, needed to maintain the random motions in the interstellar gas is estimated as 1051·4±1ergs.

The role of interstellar filaments in shaping the IMF and regulating star formation

2015 ◽  
Vol 75-76 ◽  
pp. 137-141
Author(s):  
P. André ◽  
V. Könyves ◽  
A. Roy
Keyword(s):  
Star Formation ◽  
The Imf
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