Lyα emitters at z = 6.5 in the SSA22 field: A large-scale fluctuation of the neutral hydrogen fraction at the end of the reionizaion epoch?

2010 ◽  
Author(s):  
A. K. Inoue ◽  
E. Nakamura ◽  
T. Hayashino ◽  
M. Horie ◽  
K. Kousai ◽  
...  
2001 ◽  
Vol 8 (12) ◽  
pp. 5171-5180 ◽  
Author(s):  
O. Grulke ◽  
T. Klinger ◽  
M. Endler ◽  
A. Piel ◽  

2006 ◽  
Vol 18 (1) ◽  
pp. 015103 ◽  
Author(s):  
Hideaki Mouri ◽  
Masanori Takaoka ◽  
Akihiro Hori ◽  
Yoshihide Kawashima

2005 ◽  
Vol 201 ◽  
pp. 449-450
Author(s):  
Z.-G. Deng ◽  
X.-Y. Xia

Subsamples of galaxies with different morphological types have been sorted out from Stromlo-APM redshift survey. Two-point correlation function for each subsample has been calculated. The two-point correlation functions for all subsamples show very large scale fluctuation. We show that the two-point correlation function with fluctuation could be fitted by a modified power spectrum with power excess at wave number comparable to the scale of the fluctuation.


2002 ◽  
Vol 54 (3) ◽  
pp. 327-352 ◽  
Author(s):  
Akihiro Kushino ◽  
Yoshitaka Ishisaki ◽  
Umeyo Morita ◽  
Noriko Y. Yamasaki ◽  
Manabu Ishida ◽  
...  

A numerical study on the transition from laminar to turbulent of two-dimensional fuel jet flames developed in a co-flowing air stream was made by adopting the flame surface model of infinite chemical reaction rate and unit Lewis number. The time dependent compressible Navier–Stokes equation was solved numerically with the equation for coupling function by using a finite difference method. The temperature-dependence of viscosity and diffusion coefficient were taken into account so as to study effects of increases of these coefficients on the transition. The numerical calculation was done for the case when methane is injected into a co-flowing air stream with variable injection Reynolds number up to 2500. When the Reynolds number was smaller than 1000 the flame, as well as the flow, remained laminar in the calculated domain. As the Reynolds number was increased above this value, a transition point appeared along the flame, downstream of which the flame and flow began to fluctuate. Two kinds of fluctuations were observed, a small scale fluctuation near the jet axis and a large scale fluctuation outside the flame surface, both of the same origin, due to the Kelvin–Helmholtz instability. The radial distributions of density and transport coefficients were found to play dominant roles in this instability, and hence in the transition mechanism. The decreased density in the flame accelerated the instability, while the increase in viscosity had a stabilizing effect. However, the most important effect was the increase in diffusion coefficient. The increase shifted the flame surface, where the large density decrease occurs, outside the shear layer of the jet and produced a thick viscous layer surrounding the jet which effectively suppressed the instability.


2019 ◽  
Vol 2019 (11) ◽  
pp. 023-023 ◽  
Author(s):  
Chirag Modi ◽  
Martin White ◽  
Anže Slosar ◽  
Emanuele Castorina

1999 ◽  
Vol 190 ◽  
pp. 37-44
Author(s):  
L. Staveley-Smith ◽  
S. Kim ◽  
S. Stanimirović

We review observations of neutral atomic hydrogen (HI) in the Magellanic Clouds (MCs). Being the nearest gas-rich neighbours of the Milky Way the MCs give us an excellent opportunity to study in detail the structure and evolution of the interstellar medium (ISM) and the effect of interactions between galaxies. HI in emission provides a probe of the structure and velocity field of the Clouds, allowing the study of their velocity dispersion, 3-D structure, and large-scale total-mass distribution. Recent data from Australia Telescope Compact Array surveys reveal a morphology (for both Clouds) which is heavily dominated by the effects of local star-formation, rotational shear, fragmentation, self-gravity and turbulence. The new data, which has a spatial resolution down to 10 pc, also allows the study of the distribution functions in velocity and mass for HI clouds. We discuss the morphology, dynamics and giant shell population of the LMC and SMC.


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