Interaction of an acceleration wave with a characteristic shock in Interstellar gas clouds

2021 ◽  
Author(s):  
Kajal Sharma ◽  
Rajan Arora
Keyword(s):  
Acceleration Wave ◽  
Interstellar Gas ◽  
Characteristic Shock

Interaction of a singular surface with a strong shock in the interstellar gas clouds

2021 ◽  
Vol 63 ◽  
pp. 342-358
Author(s):  
Jasobanta Jena ◽  
Sheena Mittal
Keyword(s):  
Strong Shock ◽  
Singular Surface ◽  
Acceleration Wave ◽  
Interstellar Gas ◽  
Surface Theory ◽  
Expansion Waves ◽  
Lie Group Of Transformations ◽  
Compression And Expansion ◽  
Particular Solution ◽  
Flow Variables

We investigate the interaction between a singular surface and a strong shock in the self-gravitating interstellar gas clouds with the assumption of spherical symmetry. Using the method of the Lie group of transformations, a particular solution of the flow variables and the cooling–heating function for an infinitely strong shock is obtained. This paper explores an application of the singular surface theory in the evolution of an acceleration wave front propagating through an unperturbed medium. We discuss the formation of an acceleration, considering the cases of compression and expansion waves. The influence of the cooling–heating function on a shock formation is explained. The results of a collision between a strong shock and an acceleration wave are discussed using the Lax evolutionary conditions.   doi:10.1017/S1446181121000328

INTERACTION OF A SINGULAR SURFACE WITH A STRONG SHOCK IN THE INTERSTELLAR GAS CLOUDS

2021 ◽  
pp. 1-17
Author(s):  
J. JENA ◽  
S. MITTAL
Keyword(s):  
Strong Shock ◽  
Singular Surface ◽  
Acceleration Wave ◽  
Interstellar Gas ◽  
Surface Theory ◽  
Expansion Waves ◽  
Lie Group Of Transformations ◽  
Compression And Expansion ◽  
Particular Solution ◽  
Flow Variables

Abstract We investigate the interaction between a singular surface and a strong shock in the self-gravitating interstellar gas clouds with the assumption of spherical symmetry. Using the method of the Lie group of transformations, a particular solution of the flow variables and the cooling–heating function for an infinitely strong shock is obtained. This paper explores an application of the singular surface theory in the evolution of an acceleration wave front propagating through an unperturbed medium. We discuss the formation of an acceleration, considering the cases of compression and expansion waves. The influence of the cooling–heating function on a shock formation is explained. The results of a collision between a strong shock and an acceleration wave are discussed using the Lax evolutionary conditions.

Interstellar gas in the central region of the Galaxy

1967 ◽  
Vol 31 ◽  
pp. 239-251 ◽  
Author(s):  
F. J. Kerr
Keyword(s):  
Central Region ◽  
Galactic Plane ◽  
Neutral Hydrogen ◽  
Continuum Emission ◽  
Galactic Centre ◽  
Interstellar Gas ◽  
Hydrogen Recombination ◽  
The Galaxy ◽  
Centre Region ◽  
The Relationship

A review is given of information on the galactic-centre region obtained from recent observations of the 21-cm line from neutral hydrogen, the 18-cm group of OH lines, a hydrogen recombination line at 6 cm wavelength, and the continuum emission from ionized hydrogen.Both inward and outward motions are important in this region, in addition to rotation. Several types of observation indicate the presence of material in features inclined to the galactic plane. The relationship between the H and OH concentrations is not yet clear, but a rough picture of the central region can be proposed.

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.

Remarks on the diffuse interstellar lines

1967 ◽  
Vol 31 ◽  
pp. 91-93 ◽  
Author(s):  
G. Herzberg
Keyword(s):  
Hydrogen Atoms ◽  
Interstellar Gas

It is suggested that the diffuse interstellar lines are produced in the interstellar gas by molecules consisting of a few hydrogen atoms and one other atom, such as CH4+ or NH4. Diffuseness of the lines is assumed to result from predissociation of these molecules.

NEW BACKGROUND INFRARED SOURCES FOR STUDYING THE GALACTIC CENTER'S INTERSTELLAR GAS

2015 ◽  
Author(s):  
Thomas Geballe ◽  
C Westrick ◽  
Miwa Goto ◽  
B. Schlegelmilch ◽  
S. Yeh ◽  
...  
Keyword(s):  
Interstellar Gas ◽  
Infrared Sources
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