Main content
Course: Unlisted resources area > Unit 1
Lesson 1: Unlisted videos- A message from Sal on school closures and distance learning with Khan Academy
- Video tour: Teaching programming in the classroom
- Video tour: Khan Academy AP®︎ Computer Science Principles
- Adding two 16-bit binary numbers
- Editing a webpage in an online editor
- Editing webpages in a desktop editor
- Editing a webpage from a command line editor
- Using inspect element for HTML
- Using inspect element for CSS styles
- A Tour of Programming on Khan Academy
- John Resig: Building jQuery
- Genesis effect
- Online Python Tutor (1-minute demo)
- Tetrilingo
- LXJS 2013 - Bill Mills and Angelina Fabbro - JavaScript for Science
- AP CSP example: Traffic simulation
- Scientific simulations: IllustrisTNG Single Galaxy Formation
- Memoized Fibonacci visualization
- Memoized factorial visualization
- Bottom-up Fibonacci visualization
- Recursive Fibonacci Calls (Diagrammed)
- Memoized Recursive Fibonacci Calls (Diagrammed)
- A message from Sal on school closures and Khan Academy remote learning.
© 2024 Khan AcademyTerms of usePrivacy PolicyCookie Notice
Scientific simulations: IllustrisTNG Single Galaxy Formation
This video is an example of a powerful scientific simulation that helps cosmologists understand the mechanisms of galaxy formation and test out different theories about physics and cosmology.
Credit: TNG Simulations (http://www.tng-project.org/media/)
Description from TNG project:
"Formation of a single galaxy, tracked through time from high redshift until the present day. This relatively "average" TNG50 galaxy will be just slightly less massive than our own Milky Way at z=0. We include a large-scale view (lower left), and zoomed in views of the central gas and stellar structures (lower right), while the main panel shows projected gas density. At z=1.5 we pause and rotate around the system, showing in order: gas metallicity, gas velocity field, and H-alpha luminosity, before continuing. What is a small dwarf at high redshift (108.3 solar masses in stars at z=4) transitions, at late times, into a large stable disk with a quasi-steady star formation rate of a few solar masses per year."