Formation and structure of magnetized protostellar jets

2007 ◽  
pp. 298-311
Author(s):  
Christian Fendt ◽  
Max Camenzind
Keyword(s):  
Protostellar Jets

Synthetic Images and Long-Slit Spectra of Protostellar Jets

1998 ◽  
Vol 493 (2) ◽  
pp. L91-L94 ◽  
Author(s):  
Hsien Shang ◽  
Frank H. Shu ◽  
Alfred E. Glassgold
Keyword(s):  
Protostellar Jets ◽  
Synthetic Images

scholarly journals CORRELATING THE INTERSTELLAR MAGNETIC FIELD WITH PROTOSTELLAR JETS AND ITS SOURCES

2011 ◽  
Vol 743 (1) ◽  
pp. 54 ◽  
Author(s):  
C. G. Targon ◽  
C. V. Rodrigues ◽  
A. H. Cerqueira ◽  
G. R. Hickel
Keyword(s):  
Magnetic Field ◽  
Protostellar Jets

scholarly journals First detection of acceleration and deceleration in protostellar jets?

2009 ◽  
Vol 502 (2) ◽  
pp. 579-597 ◽  
Author(s):  
A. Caratti o Garatti ◽  
J. Eislöffel ◽  
D. Froebrich ◽  
B. Nisini ◽  
T. Giannini ◽  
...  
Keyword(s):  
Protostellar Jets ◽  
Acceleration And Deceleration

scholarly journals Cooling and instabilities in colliding flows

2021 ◽  
Author(s):  
R N Markwick ◽  
A Frank ◽  
J Carroll-Nellenback ◽  
B Liu ◽  
E G Blackman ◽  
...  
Keyword(s):  
Thermal Instability ◽  
Three Dimensional ◽  
Oscillation Period ◽  
Three Dimensions ◽  
Temperature Dependent ◽  
Radiative Shock ◽  
Hydrodynamic Simulations ◽  
Protostellar Jets ◽  
The One ◽  
Cooling Function

Abstract Collisional self-interactions occurring in protostellar jets give rise to strong shocks, the structure of which can be affected by radiative cooling within the flow. To study such colliding flows, we use the AstroBEAR AMR code to conduct hydrodynamic simulations in both one and three dimensions with a power law cooling function. The characteristic length and time scales for cooling are temperature dependent and thus may vary as shocked gas cools. When the cooling length decreases sufficiently rapidly the system becomes unstable to the radiative shock instability, which produces oscillations in the position of the shock front; these oscillations can be seen in both the one and three dimensional cases. Our simulations show no evidence of the density clumping characteristic of a thermal instability, even when the cooling function meets the expected criteria. In the three-dimensional case, the nonlinear thin shell instability (NTSI) is found to dominate when the cooling length is sufficiently small. When the flows are subjected to the radiative shock instability, oscillations in the size of the cooling region allow NTSI to occur at larger cooling lengths, though larger cooling lengths delay the onset of NTSI by increasing the oscillation period.

Magnetohydrodynamic Models of Axisymmetric Protostellar Jets

2000 ◽  
Vol 540 (1) ◽  
pp. 192-210 ◽  
Author(s):  
James M. Stone ◽  
Philip E. Hardee
Keyword(s):  
Protostellar Jets ◽  
Magnetohydrodynamic Models
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