Size Distribution of Dust grains in Vortices in a Protoplanetary Disk

2009 ◽  
Author(s):  
Eri Kawamura ◽  
Sei-ichiro Watanabe ◽  
Tomonori Usuda ◽  
Motohide Tamura ◽  
Miki Ishii
Keyword(s):  
Size Distribution ◽  
Protoplanetary Disk ◽  
Dust Grains

Effect of dust grains size distribution on the Bohm sheath criterion in plasmas

2020 ◽  
Vol 27 (9) ◽  
pp. 093701
Author(s):  
N. Rebiai ◽  
A. Tahraoui ◽  
Z. Kechidi
Keyword(s):  
Size Distribution ◽  
Dust Grains

Effect of dust size distribution on ion-acoustic solitons in dusty plasmas with different dust grains

2017 ◽  
Vol 43 (2) ◽  
pp. 212-217
Author(s):  
Dong-Ning Gao ◽  
Yang Yang ◽  
Qiang Yan ◽  
Xiao-Yun Wang ◽  
Wen-Shan Duan
Keyword(s):  
Size Distribution ◽  
Dusty Plasmas ◽  
Dust Grains ◽  
Dust Size Distribution ◽  
Ion Acoustic ◽  
Ion Acoustic Solitons

On the size distribution and physical properties of interplanetary dust grains

Icarus ◽  
1980 ◽  
Vol 43 (3) ◽  
pp. 350-372 ◽  
Author(s):  
L.B. Le Sergeant D'Hendecourt ◽  
Ph.L. Lamy
Keyword(s):  
Physical Properties ◽  
Size Distribution ◽  
Interplanetary Dust ◽  
Dust Grains

scholarly journals From grains to pebbles: the influence of size distribution and chemical composition on dust emission properties

2019 ◽  
Vol 631 ◽  
pp. A88 ◽  
Author(s):  
N. Ysard ◽  
M. Koehler ◽  
I. Jimenez-Serra ◽  
A. P. Jones ◽  
L. Verstraete
Keyword(s):  
Chemical Composition ◽  
Size Distribution ◽  
Spectral Index ◽  
Thermal Emission ◽  
Spectral Energy ◽  
Internal Source ◽  
Dust Grains ◽  
Grain Composition ◽  
Dust Mass ◽  
Dust Composition

Context. The size and chemical composition of interstellar dust grains are critical in setting the dynamical, physical, and chemical evolution of all the media in which they are present. Thanks to facilities such as the Atacama Large Millimeter/submillimeter Array (ALMA) and, in the future, the Square Kilometer Array (SKA), thermal emission in the (sub)millimetre to centimetre domain has become a very convenient way to trace grain properties. Aims. Our aim is to understand the influence of the composition and size distribution of dust grains on the shape of their spectral energy distribution (peak position, spectral index) in dense interstellar regions such as molecular clouds, prestellar cores, young stellar objects, and protoplanetary discs. Methods. Starting from the optical constants defined in The Heterogeneous dust Evolution Model for Interstellar Solids (THEMIS) for amorphous hydrogenated carbon grains and amorphous silicates in addition to water ice, we defined six material mixtures that we believe are representative of the expected dust composition in dense interstellar regions. The optical properties of 0.01 μm to 10 cm grains were then calculated with effective medium and Mie theories. The corresponding spectral energy distributions were subsequently calculated for isolated clouds either externally heated by the standard interstellar radiation field alone or in addition to an internal source. Results. The three main outcomes of this study are as follows. Firstly, the dust mass absorption coefficient strongly depends on both grain composition and size distribution potentially leading to errors in dust mass estimates by factors up to ~3 and 20, respectively. Secondly, it appears almost impossible to retrieve the grain composition from the (sub)millimetre to centimetre thermal emission shape alone as its spectral index for λ ≳ 3 mm does not depend on dust composition. Thirdly, using the “true” dust opacity spectral index to estimate grain sizes may lead to erroneous findings as the observed spectral index can be highly modified by the dust temperature distribution along the line of sight, which depends on the specific heating source and on the geometry of the studied interstellar region. Conclusions. Based on the interpretation of only the spectral shape of (sub)millimetre to centimetre observational data, the determination of the dust masses, compositions, and sizes are highly uncertain.

scholarly journals PROTOPLANETARY DISK MASSES IN IC348: A RAPID DECLINE IN THE POPULATION OF SMALL DUST GRAINS AFTER 1 Myr

2011 ◽  
Vol 736 (2) ◽  
pp. 135 ◽  
Author(s):  
Nicholas Lee ◽  
Jonathan P. Williams ◽  
Lucas A. Cieza
Keyword(s):  
Protoplanetary Disk ◽  
Rapid Decline ◽  
Dust Grains ◽  
Small Dust

scholarly journals Rapid elimination of small dust grains in molecular clouds

2020 ◽  
Vol 641 ◽  
pp. A39 ◽  
Author(s):  
Kedron Silsbee ◽  
Alexei V. Ivlev ◽  
Olli Sipilä ◽  
Paola Caselli ◽  
Bo Zhao
Keyword(s):  
Size Distribution ◽  
Cosmic Ray ◽  
Ionization Rate ◽  
Microwave Emission ◽  
Dust Grains ◽  
Gas Temperature ◽  
Neutral Gas ◽  
Cloud Cores ◽  
The Impact ◽  
Small Dust

We argue that impact velocities between dust grains with sizes of less than ∼0.1 μm in molecular cloud cores are dominated by drift arising from ambipolar diffusion. This effect is due to the size dependence of the dust coupling to the magnetic field and the neutral gas. Assuming perfect sticking in collisions up to ≈50 m s−1, we show that this effect causes rapid depletion of small grains, consistent with starlight extinction and IR and microwave emission measurements, both in the core center (n ∼ 106 cm−3) and envelope (n ∼ 104 cm−3). The upper end of the size distribution does not change significantly if only velocities arising from this effect are considered. We consider the impact of an evolved grain-size distribution on the gas temperature, and argue that if the depletion of small dust grains occurs as expected from our model, then the cosmic ray ionization rate must be well below 10−16 s−1 at a number density of 105 cm−3.

scholarly journals The Evidence of Radio Polarization Induced by the Radiative Grain Alignment and Self-scattering of Dust Grains in a Protoplanetary Disk

2017 ◽  
Vol 844 (1) ◽  
pp. L5 ◽  
Author(s):  
Akimasa Kataoka ◽  
Takashi Tsukagoshi ◽  
Adriana Pohl ◽  
Takayuki Muto ◽  
Hiroshi Nagai ◽  
...  
Keyword(s):  
Protoplanetary Disk ◽  
Dust Grains ◽  
Grain Alignment

scholarly journals Effect of lift force on the aerodynamics of dust grains in the protoplanetary disk

2014 ◽  
Vol 66 (1) ◽  
pp. 132 ◽  
Author(s):  
Masaki S Yamaguchi ◽  
Shigeo S Kimura
Keyword(s):  
Lift Force ◽  
Protoplanetary Disk ◽  
Dust Grains

Effects of dust size distribution on nonlinear magnetosonic wave in a dusty plasma

2020 ◽  
pp. 2150121
Author(s):  
Bo Liu ◽  
Juan Fang Han ◽  
Wen Shan Duan
Keyword(s):  
Solitary Wave ◽  
Size Distribution ◽  
Dusty Plasma ◽  
Propagation Velocity ◽  
Magnetosonic Wave ◽  
Dust Grains ◽  
Minimum Radius ◽  
Dust Size Distribution ◽  
The Difference ◽  
Dust Grain

Both the linear and the nonlinear magnetosonic wave in a multi-component dusty plasma are studied in the present paper. The dependence of the dispersion relation of the linear waves on the dust size distribution are given. It seems that the larger the difference between the maximum and the minimum radius of the dust grains, the lower the wave frequency for all cases of the dust size distribution. Furthermore, it is noted that the width, the amplitude and the propagation velocity of the KdV solitary wave depend on the dust size distribution, especially it depend on whether the number density of the larger sized dust grain is larger or smaller than that of the smaller sized dust grain. For the power law dust size distribution, the width and the propagation velocity of the KdV solitary wave between the maximum and the minimum radius of the dust grains is larger than that of mono-sized dusty plasma.

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