scholarly journals A system of ionized gas dynamics

2019 ◽  
Vol 60 (11) ◽  
pp. 111507 ◽  
Author(s):  
Fumioki Asakura ◽  
Andrea Corli
Keyword(s):  
Gas Dynamics ◽  
Ionized Gas

Gas dynamics and star formation in “isolated” and interacting galaxies using FP observations

2019 ◽  
Vol 14 (S353) ◽  
pp. 264-265
Author(s):  
Isaura Fuentes-Carrera ◽  
Nelli Cárdenas-Martínez ◽  
Martín Nava-Callejas ◽  
Margarita Rosado
Keyword(s):  
Star Formation ◽  
Gas Dynamics ◽  
Equal Mass ◽  
Interacting Galaxies ◽  
Ionized Gas ◽  
Star Forming ◽  
Gas Kinematics ◽  
Fabry Perot ◽  
Different Types

AbstractWe present scanning Fabry-Perot observations of different types of star-forming galaxies from apparently isolated LIRGs to equal mass interacting galaxies. We analyze the ionized gas kinematics, its relation with the morphology of each system and the location of SF regions for different systems.

Near infrared spectroscopy of protostars

1981 ◽  
Vol 303 (1480) ◽  
pp. 487-496
Keyword(s):  
Infrared Spectroscopy ◽  
Near Infrared Spectroscopy ◽  
Gas Dynamics ◽  
Near Infrared ◽  
Molecular Gas ◽  
Orion Nebula ◽  
Ionized Gas ◽  
Physical Conditions ◽  
Vibrational Bands ◽  
Optical Wavelengths

Observational study of protostars and their immediate environs has recently become possible as a result of advances in infrared spectroscopy, especially in the near infrared (A = 2—5 pm). Although such stars are totally obscured at optical wavelengths by the enshrouding dust and gas from which they formed, the near infrared spectroscopy has yielded detection of emission lines from both ionized gas and high excitation molecular gas ( T >2000 K) probably within a few astronomical units of several such sources (e.g. the BN object in the Orion nebula). The former lines provide the first constraints on the spectral type and temperature of the protostar; the latter reveal the physical conditions (density and temperature) and gas dynamics in the immediate protostellar nebula. . Data on the BN object covering the CO, 13 CO, and H 2 vibrational bands and the H II lines are presented as an illustration of these techniques.

scholarly journals The Mass Distribution in the Central Few Parsecs of the Galaxy

1989 ◽  
Vol 136 ◽  
pp. 493-499
Author(s):  
John H. Lacy
Keyword(s):  
Mass Distribution ◽  
Gas Dynamics ◽  
Good Evidence ◽  
Ionized Gas ◽  
Massive Black Hole ◽  
Central Mass ◽  
Magnetic Forces ◽  
Gravitational Forces ◽  
The Galaxy

The determination of the mass distribution in the central few parsecs of the Galaxy, primarily from the ionized gas dynamics, is discussed. The gas motions are described and interpreted assuming that the orbits are determined by gravitational forces. It is shown that there is good evidence for a central mass of ~ 2 × 106 M⊙. The primary uncertainty in this conclusion results from the possibility of significant magnetic forces. In the absence of corroborating evidence, the case for a massive black hole cannot be considered proven.

scholarly journals Gas Dynamics in the Galactic Centre: Gravity vs. Magnetism

1989 ◽  
Vol 136 ◽  
pp. 341-344
Author(s):  
Ralph E. Pudritz
Keyword(s):  
Magnetic Fields ◽  
Gas Dynamics ◽  
Galactic Nuclei ◽  
Galactic Centre ◽  
Ionized Gas ◽  
Gravitational Fields ◽  
Key Points ◽  
Interesting Discussion ◽  
The Many ◽  
The Magnetic Field

This contribution is a summary of an impromptu and extremely interesting discussion on the nature of the forces acting on gas in the galactic centre. The origins of the gas motions in the central few parsecs are crucial for clarifying many important problems about galactic nuclei. Some of the many gas dynamics issues that were raised include: 1. are there explosive events in the galactic centre which produce outward moving gas clouds (see Heyvaerts, these proceedings)? 2. are the streamers of gas due to the tidal disruption of molecular clouds that stray in too deep in the galactic centre's tidal field (see Serabyn, these proceedings)? 3. is there circular gas motion which would be important in constraining the nature of the mass distribution inside scales of a few pc (see review by Townes, these proceedings)?The discussion centered on gas dynamics in the molecular torus and ionized gas streamers on the 2–5 pc scale. Because reliable measurements of the magnetic field strength in the galactic centre are not yet available, several of the key points of contention will not be finally settled until the data are in. Be this as it may, the discussion boiled down to the issue of whether gravity or magnetic fields were responsible for the structures and morphology on this scale. Accordingly I will label the arguments of the two relevant camps by G (for gravitational fields as the predominant shaper of things) and M (for magnetic fields as the important agents).

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.

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