scholarly journals Quasilinear saturation of the aperiodic ordinary mode streaming instability

2015 ◽  
Vol 22 (9) ◽  
pp. 092301 ◽  
Author(s):  
A. Stockem Novo ◽  
P. H. Yoon ◽  
M. Lazar ◽  
R. Schlickeiser ◽  
S. Poedts ◽  
...  
Keyword(s):  
Ordinary Mode ◽  
Streaming Instability

Streaming instability of dust-acoustic mode with helical wavefronts

2019 ◽  
Vol 62 ◽  
pp. 144-150
Author(s):  
S. Bukhari ◽  
M. Naqash ◽  
S. Ali ◽  
Muhammad Rafique
Keyword(s):  
Acoustic Mode ◽  
Streaming Instability ◽  
Dust Acoustic ◽  
Dust Acoustic Mode

Scattering of ordinary‐mode electromagnetic waves by density fluctuations in tokamaks

1993 ◽  
Vol 5 (12) ◽  
pp. 4299-4311 ◽  
Author(s):  
Gary R. Smith ◽  
Daniel R. Cook ◽  
Allan N. Kaufman ◽  
Arnold H. Kritz ◽  
Steven W. McDonald
Keyword(s):  
Electromagnetic Waves ◽  
Density Fluctuations ◽  
Ordinary Mode

scholarly journals A Lagrangian model for dust evolution in protoplanetary disks: formation of wet and dry planetesimals at different stellar masses

2018 ◽  
Vol 620 ◽  
pp. A134 ◽  
Author(s):  
Djoeke Schoonenberg ◽  
Chris W. Ormel ◽  
Sebastiaan Krijt
Keyword(s):  
Accretion Rate ◽  
Protoplanetary Disks ◽  
Particle Method ◽  
Solid Particles ◽  
Lagrangian Model ◽  
Low Mass Stars ◽  
Streaming Instability ◽  
Mass Fluxes ◽  
Gas Accretion ◽  
Stellar Masses

We introduce a new Lagrangian smooth-particle method to model the growth and drift of pebbles in protoplanetary disks. The Lagrangian nature of the model makes it especially suited to following characteristics of individual (groups of) particles, such as their composition. In this work we focus on the water content of solid particles. Planetesimal formation via streaming instability is taken into account, partly based on previous results on streaming instability outside the water snowline that were presented in a recent publication. We validated our model by reproducing earlier results from the literature and apply our model to steady-state viscous gas disks (with constant gas accretion rate) around stars with different masses. We also present various other models where we explore the effects of pebble accretion, the fragmentation velocity threshold, the global metallicity of the disk, and a time-dependent gas accretion rate. We find that planetesimals preferentially form in a local annulus outside the water snowline, at early times in the lifetime of the disk (≲105 yr), when the pebble mass fluxes are high enough to trigger the streaming instability. During this first phase in the planet formation process, the snowline location hardly changes due to slow viscous evolution, and we conclude that assuming a constant gas accretion rate is justified in this first stage. The efficiency of converting the solids reservoir of the disk to planetesimals depends on the location of the water snowline. Cooler disks with a closer-in water snowline are more efficient at producing planetesimals than hotter disks where the water snowline is located further away from the star. Therefore, low-mass stars tend to form planetesimals more efficiently, but any correlation may be overshadowed by the spread in disk properties.

scholarly journals Lepton-driven Nonresonant Streaming Instability

2021 ◽  
Vol 923 (2) ◽  
pp. 208
Author(s):  
Siddhartha Gupta ◽  
Damiano Caprioli ◽  
Colby C. Haggerty
Keyword(s):  
Magnetic Field ◽  
Laboratory Experiments ◽  
Magnetized Plasma ◽  
Ion Current ◽  
Pulsar Wind Nebulae ◽  
Particle In Cell ◽  
Streaming Instability ◽  
Electrons And Positrons ◽  
Pulsar Wind ◽  
The Magnetic Field

Abstract A strong super-Alfvénic drift of energetic particles (or cosmic rays) in a magnetized plasma can amplify the magnetic field significantly through nonresonant streaming instability (NRSI). While the traditional analysis is done for an ion current, here we use kinetic particle-in-cell simulations to study how the NRSI behaves when it is driven by electrons or by a mixture of electrons and positrons. In particular, we characterize the growth rate, spectrum, and helicity of the unstable modes, as well the level of the magnetic field at saturation. Our results are potentially relevant for several space/astrophysical environments (e.g., electron strahl in the solar wind, at oblique nonrelativistic shocks, around pulsar wind nebulae), and also in laboratory experiments.

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