scholarly journals Shear instabilities in the dust layer of the solar nebula I. The linear analysis of a non-gravitating one-fluid model without the Coriolis and the solar tidal forces

2000 ◽  
Vol 52 (7) ◽  
pp. 517-526 ◽  
Author(s):  
Minoru Sekiya ◽  
Naoki Ishitsu
Keyword(s):  
Solar Nebula ◽  
Fluid Model ◽  
Linear Analysis ◽  
Dust Layer ◽  
Tidal Forces ◽  
Shear Instabilities

Linear Analysis of the Interaction of Rotating Helical Magnetic Perturbations with Tokamak Plasmas Based on the Reduced Two-Fluid Model

2006 ◽  
Vol 46 (7-9) ◽  
pp. 539-544 ◽  
Author(s):  
Y. Kikuchi ◽  
K. H. Finken ◽  
M. Jakubowski ◽  
M. Lehnen ◽  
D. Reiser ◽  
...  
Keyword(s):  
Fluid Model ◽  
Linear Analysis ◽  
Tokamak Plasmas ◽  
Magnetic Perturbations ◽  
Two Fluid Model ◽  
Two Fluid

scholarly journals 3D Modeling of absorption by various species for hot jupiter HD209458b

2019 ◽  
Author(s):  
I F Shaikhislamov ◽  
M L Khodachenko ◽  
H Lammer ◽  
A G Berezutsky ◽  
I B Miroshnichenko ◽  
...  
Keyword(s):  
3D Modeling ◽  
Loss Rate ◽  
Fluid Model ◽  
Mass Loss Rate ◽  
2D Modeling ◽  
Tidal Forces ◽  
Stellar Radiation ◽  
Solar Abundances ◽  
First Time ◽  
2D Model

ABSTRACT The absorption of stellar radiation observed at transits of HD209458b in resonant lines of OI and CII has not yet been satisfactorily modeled. In our previous 2D simulations we have shown that hydrogen-dominated upper atmosphere of HD209458b, heated by XUV radiation, expands supersonically beyond the Roche lobe and drags heavier species along with it. Assuming solar abundances, OI and CII particles accelerated by tidal forces to velocities up to 50 km/s should produce the absorption due to Doppler resonance at the level of 6–10 per cent, consistent with the observations. Since the 2D geometry does not take into account the Coriolis force in a planet reference frame, the question remained to which extent the spiraling of escaping planetary material and actually achieved velocity may influence the conclusions made on basis of 2D modeling. In the present paper we apply for the first time in studies of HD209458b a global 3D hydrodynamic multi-fluid model. The results confirm our previous findings that the velocity of the planetary flow is sufficiently high to match the widths of OI and CII resonant lines. To match absorption in those lines, including HI, with observations, the mass loss rate of HD209458b should be about 2.5·1011 g/s which is 3.5 times larger than that revealed by the 2D model. The other novel finding is that matching of the absorption measured in MgII and SiIII lines requires at least 10 times lower abundances of these elements than the Solar values.

Linear analysis of sheared flow stabilization of global magnetohydrodynamic instabilities based on the Hall fluid model

2002 ◽  
Vol 9 (3) ◽  
pp. 913-922 ◽  
Author(s):  
V. I. Sotnikov ◽  
I. Paraschiv ◽  
V. Makhin ◽  
B. S. Bauer ◽  
J. N. Leboeuf ◽  
...  
Keyword(s):  
Fluid Model ◽  
Linear Analysis ◽  
Sheared Flow ◽  
Flow Stabilization ◽  
Sheared Flow Stabilization

Heliopause Instabilities Driven by Plasma-Neutral Interaction: Linear Analysis from Fluid Model

2011 ◽  
Author(s):  
B. Dasgupta ◽  
V. Florinski ◽  
G. P. Zank ◽  
A. Bandyopadhyay ◽  
K. Avinash ◽  
...  
Keyword(s):  
Fluid Model ◽  
Linear Analysis

The Infancy of Solar-Type Stars and its Relevance for the Origin of Life

1997 ◽  
Vol 161 ◽  
pp. 267-282 ◽  
Author(s):  
Thierry Montmerle
Keyword(s):  
Main Sequence ◽  
Solar Nebula ◽  
Circumstellar Disks ◽  
T Tauri Stars ◽  
Necessary Condition ◽  
Sequence Evolution ◽  
T Tauri ◽  
Solar Type ◽  
Optical Domain ◽  
The Origin Of Life

AbstractFor life to develop, planets are a necessary condition. Likewise, for planets to form, stars must be surrounded by circumstellar disks, at least some time during their pre-main sequence evolution. Much progress has been made recently in the study of young solar-like stars. In the optical domain, these stars are known as «T Tauri stars». A significant number show IR excess, and other phenomena indirectly suggesting the presence of circumstellar disks. The current wisdom is that there is an evolutionary sequence from protostars to T Tauri stars. This sequence is characterized by the initial presence of disks, with lifetimes ~ 1-10 Myr after the intial collapse of a dense envelope having given birth to a star. While they are present, about 30% of the disks have masses larger than the minimum solar nebula. Their disappearance may correspond to the growth of dust grains, followed by planetesimal and planet formation, but this is not yet demonstrated.

DUAL-MODE LINEAR ANALYSIS OF TEMPORAL INSTABILITY FOR POWER-LAW LIQUID SHEET

2016 ◽  
Vol 26 (4) ◽  
pp. 319-347 ◽  
Author(s):  
Han-Yu Deng ◽  
Feng Feng ◽  
Xiao-Song Wu
Keyword(s):  
Power Law ◽  
Linear Analysis ◽  
Liquid Sheet ◽  
Dual Mode ◽  
Temporal Instability
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