1
Q
When are non-linear (magneto-)hydrodynamics simulations applicable?
A
Star formation Cosmological simulations of galaxies and cosmological structure Accretion Disks Exoplanetary atmospheres Stellar structure
2
Q
When are N-body simulations applicable?
A
Dark Matter Stellar clusters • In the absence of gas • Coupled to hydrodynamic simulations Planetary dynamics
3
Q
What is the principle behind smoothed particle hydrodynamics?
A
A smoothing kernel that weights closer neighbors more heavily
4
Q
How is the Courant number defined?
A
C=c_s*delta t/delta x
RRY041
flashcards
Decks in class (21)
# Cards
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1. Introduction47
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Lecture 2 - Collisional processes14
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Lecture 4 - More Radiative Processes30
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Lecture 3 - Radiative Processes10
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Lecture 5 - Free-Free emission and absorption and radio waves9
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Lecture 6 - Collisional Excitation15
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Lecture 7 - Radio Lines, Radiative Trapping, Excitation by Recombination, Optical Pumping17
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Lecture 8 - Ionisation and Recombination11
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Lecture 9 - Interstellar dust16
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Astrochemistry26
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Lecture 11 - grain temperature, charge and dynamics8
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Lecture 12 - Heating and Cooling of HII regions2
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Lecture 13 - Heating & Cooling of HI Gas8
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Lecture 14 - Molecular clouds14
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Lecture 15 - Observations of Molecular Clouds2
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Lecture 16 - Molecular Clouds and CO7
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Lecture 17 - Gas Dynamics3
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Lecture 18 - Simulations4
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Lecture 21 - The Interstellar Medium and Star Formation9
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Lecture 19 - Shock Waves4
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Lecture 20 - Supernovae & the “3-Phase” Model of the ISM7
