Effects of magnetic field on pulse and CW operation of the large bore ionized gas laser

1967 ◽  
Vol 55 (5) ◽  
pp. 691-692 ◽  
Author(s):  
S.A. Ahmed ◽  
T.J. Faith ◽  
G.W. Hoffman
Keyword(s):  
Magnetic Field ◽  
Ionized Gas ◽  
Gas Laser ◽  
Cw Operation

scholarly journals Survival of molecular gas in a stellar feedback-driven outflow witnessed with the MUSE TIMER project and ALMA

2019 ◽  
Vol 488 (3) ◽  
pp. 3904-3928 ◽  
Author(s):  
Ryan Leaman ◽  
Francesca Fragkoudi ◽  
Miguel Querejeta ◽  
Gigi Y C Leung ◽  
Dimitri A Gadotti ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Star Formation ◽  
Mechanical Energy ◽  
Molecular Gas ◽  
Ionized Gas ◽  
Star Forming ◽  
Stellar Feedback ◽  
Dominant Component ◽  
The Galaxy ◽  
Field Lines

ABSTRACT Stellar feedback plays a significant role in modulating star formation, redistributing metals, and shaping the baryonic and dark structure of galaxies – however, the efficiency of its energy deposition to the interstellar medium is challenging to constrain observationally. Here we leverage HST and ALMA imaging of a molecular gas and dust shell ($M_{\mathrm{ H}_2} \sim 2\times 10^{5}\, {\rm M}_{\odot }$) in an outflow from the nuclear star-forming ring of the galaxy NGC 3351, to serve as a boundary condition for a dynamical and energetic analysis of the outflowing ionized gas seen in our MUSE TIMER survey. We use starburst99 models and prescriptions for feedback from simulations to demonstrate that the observed star formation energetics can reproduce the ionized and molecular gas dynamics – provided a dominant component of the momentum injection comes from direct photon pressure from young stars, on top of supernovae, photoionization heating, and stellar winds. The mechanical energy budget from these sources is comparable to low luminosity active galactic neuclei, suggesting that stellar feedback can be a relevant driver of bulk gas motions in galaxy centres – although here ≲10−3 of the ionized gas mass is escaping the galaxy. We test several scenarios for the survival/formation of the cold gas in the outflow, including in situ condensation and cooling. Interestingly, the geometry of the molecular gas shell, observed magnetic field strengths and emission line diagnostics are consistent with a scenario where magnetic field lines aided survival of the dusty ISM as it was initially launched (with mass-loading factor ≲1) from the ring by stellar feedback. This system’s unique feedback-driven morphology can hopefully serve as a useful litmus test for feedback prescriptions in magnetohydrodynamical galaxy simulations.

Exploring the nonextensive thermodynamics of partially ionized gas in magnetic field

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
June Young Kim ◽  
Hyo-Chang Lee ◽  
Geunwoo Go ◽  
Yeong Hwan Choi ◽  
Y. S. Hwang ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Ionized Gas ◽  
Nonextensive Thermodynamics ◽  
Partially Ionized

scholarly journals 9. Waves in a hot ionized gas in a magnetic field

1958 ◽  
Vol 6 ◽  
pp. 81-86 ◽  
Author(s):  
Ernst åström
Keyword(s):  
Magnetic Field ◽  
Charge Density ◽  
Linear Relation ◽  
Zero Temperature ◽  
Ionized Gas ◽  
Solid Media ◽  
New Form ◽  
Image Position

The electromagnetic state of vacuum is characterized by two vector quantities, namely E and B. They are related to current and charge density by the equations Sometimes it is suitable and possible to introduce two new quantities, H and D, so defined that the equations (1) and (2) appear in the new form (Strattonm) and with a linear relation between E and D and also between B and H. This formalism is common when dealing with fluid and solid media, and has also been introduced to ionized media of zero temperature (Nichols and Schelleng[2], Alfven[3], p. 85, Astrom[4]). Here we shall say a few words about this matter for ionized media of non-zero temperature. In this connexion we also get an opportunity to discuss the meaning of the conception of diamagnetism.

scholarly journals Magnetic Fields & Ionized Gas in Elliptical Galaxy Halos

1990 ◽  
Vol 140 ◽  
pp. 459-462
Author(s):  
Richard G. Strom
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Elliptical Galaxy ◽  
Radio Sources ◽  
Early Type ◽  
Ionized Gas ◽  
X Ray ◽  
Galaxy Halos ◽  
Field Strengths

Faraday depolarization estimates of thermal densities within the components of double radio sources agree well with estimates from X-ray observations of hot halos around early-type galaxies, provided magnetic field strengths are close to their equipartition values. Internal Faraday dispersion is the main cause of the depolarization observed.

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