scholarly journals Celestial mechanics and polarization optics of the Kordylewski dust cloud in the Earth–Moon Lagrange point L5 – I. Three-dimensional celestial mechanical modelling of dust cloud formation

2018 ◽  
Vol 480 (4) ◽  
pp. 5550-5559 ◽  
Author(s):  
Judit Slíz-Balogh ◽  
András Barta ◽  
Gábor Horváth
Keyword(s):  
Celestial Mechanics ◽  
Dust Cloud ◽  
Three Dimensional ◽  
Cloud Formation ◽  
Lagrange Point ◽  
The Earth ◽  
Mechanical Modelling ◽  
Polarization Optics

THREE DIMENSIONAL THERMO-MECHANICAL MODELLING OF CARBON FOAM

Equipment ◽  
2006 ◽  
Author(s):  
M. K. Alam ◽  
C. Druma ◽  
M. Anghelescu ◽  
B. Maruyama
Keyword(s):  
Three Dimensional ◽  
Carbon Foam ◽  
Mechanical Modelling

scholarly journals A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres

2008 ◽  
Vol 391 (4) ◽  
pp. 1854-1873 ◽  
Author(s):  
Ch. Helling ◽  
A. Ackerman ◽  
F. Allard ◽  
M. Dehn ◽  
P. Hauschildt ◽  
...  
Keyword(s):  
Dust Cloud ◽  
Cloud Formation

scholarly journals The particle and magnetic environments surrounding close-in exoplanets

2015 ◽  
Vol 11 (S320) ◽  
pp. 397-402
Author(s):  
A. A. Vidotto ◽  
R. Fares ◽  
M. Jardine ◽  
C. Moutou ◽  
J.-F. Donati
Keyword(s):  
Magnetic Fields ◽  
Radio Emission ◽  
Magnetic Field Intensity ◽  
Three Dimensional ◽  
Stellar Winds ◽  
Local Conditions ◽  
Hot Jupiters ◽  
The Earth ◽  
Weather Events ◽  
Host Stars

AbstractThe proper characterisation of stellar winds is essential for the study of propagation of eruptive events (flares, coronal mass ejections) and the study of space weather events on exoplanets. Here, we quantitatively investigate the nature of the stellar winds surrounding the hot Jupiters HD46375b, HD73256b, HD102195b, HD130322b, HD179949b. We simulate the three-dimensional winds of their host stars, in which we directly incorporate their observed surface magnetic fields. With that, we derive the wind properties at the position of the hot-Jupiters’ orbits (temperature, velocity, magnetic field intensity and pressure). We show that the exoplanets studied here are immersed in a local stellar wind that is much denser than the local conditions encountered around the solar system planets (e.g., 5 orders of magnitude denser than the conditions experienced by the Earth). The environment surrounding these exoplanets also differs in terms of dynamics (slower stellar winds, but higher Keplerian velocities) and ambient magnetic fields (2 to 3 orders of magnitude larger than the interplanetary medium surrounding the Earth). The characterisation of the host star's wind is also crucial for the study of how the wind interacts with exoplanets. For example, we compute the exoplanetary radio emission that is released in the wind-exoplanet interaction. For the hot-Jupiters studied here, we find radio fluxes ranging from 0.02 to 0.13 mJy. These fluxes could become orders of magnitude higher when stellar eruptions impact exoplanets, increasing the potential of detecting exoplanetary radio emission.

Seismic Rays

2017 ◽  
Author(s):  
John A. Adam
Keyword(s):  
Inverse Problem ◽  
Seismic Tomography ◽  
Seismic Waves ◽  
Seismic Station ◽  
Three Dimensional ◽  
Arrival Times ◽  
The Earth ◽  
Straight Lines ◽  
Ray Path ◽  
Uniform Composition

This chapter focuses on the underlying mathematics of seismic rays. Seismic waves caused by earthquakes and explosions are used in seismic tomography to create computer-generated, three-dimensional images of Earth's interior. If the Earth had a uniform composition and density, seismic rays would travel in straight lines. However, it is broadly layered, causing seismic rays to be refracted and reflected across boundaries. In order to calculate the speed along the wave's ray path, the time it takes for a seismic wave to arrive at a seismic station from an earthquake needs to be determined. Arrival times of different seismic waves allow scientists to define slower or faster regions deep in the Earth. The chapter first presents the relevant equations for seismic rays before discussing how rays are propagated in a spherical Earth. The Wiechert-Herglotz inverse problem is considered, along with the properties of X in a horizontally stratified Earth.

Three-dimensional models of the zodiacal dust cloud

Icarus ◽  
1989 ◽  
Vol 82 (2) ◽  
pp. 369-378 ◽  
Author(s):  
R.H. Giese ◽  
B. Kneiβel
Keyword(s):  
Dust Cloud ◽  
Three Dimensional ◽  
Zodiacal Dust ◽  
Dimensional Models ◽  
Three Dimensional Models
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