php require("/home/jeffery/public_html/astro/planetary_systems/planetary_system_formation_videos.html");?>
Planetary system formation videos
(i.e., Planetary system formation
videos):
- Planetary System Formation Simulation (200 AU View) | 0:44:
Professional computer simulation
using
smoothed-partice hydrodynamics (SPH)
of Planet formation in
protoplanetary disk
with planetary migration.
Planetary migration
happens because of
gravitational interactions among
the protoplanets,
planetesimals,
grains of condensed matter,
and gas
which is mainly
hydrogen
and helium, of course.
The is also some viscosity
and magnetic field effects.
It is all very complicated and
supercomputer
computer simulations
are needed for understanding which is still only partial.
Good for classroom.
- Trans-Neptunian binaries formation
by the streaming instability (2019) | 0:30:
A critical step in
planet formation
in a protoplanetary disk
is the accretion of planetesimals,
bodies 1--1,000 km in size scale, from smaller disk constituents.
This process is poorly understood, partly because we lack good observational constraints
on the complex physical processes that contribute to
planetesimal formation.
In the outer Solar System,
the best place to look for clues is the
Kuiper belt, where
icy
planetesimals
survive to this day. Here we report evidence that
Kuiper belt planetesimals formed by
the streaming instability,
a process in which fluid dynamically
concentrated clumps of pebbles
gravitationally collapse
into 100-kilometre-class bodies.
Gravitational collapse
has previously been suggested to explain the ubiquity of
binary systems with
equal-sized companions
in the Kuiper belt. We analyse new
fluid dynamical
computer simulation
of the streaming instability
to determine the model expectations for the spatial orientation of
binary system orbits.
The predicted broad inclination distribution with approximately 80%
of prograde
binary system orbits
matches the observations of
trans-Neptunian object
binaries.
The formation models that imply predominantly
retrograde
binary system orbits
can be ruled out. Given its applicability over a wide range of
protoplanetary disk conditions,
it is expected that the streaming instability
also seeded planetesimal formation
elsewhere in the Solar System
and throughout the observable universe.
Good for classroom.
- Planet-Disk Interaction and Orbital Migration. Movie 1. Low Mass Planet | 0:33: Good short presentation of
planetary migration by
one simple mechanism with narration.
Protoplanetary disks
can have spiral density waves
which are distantly related to the
spiral density waves in
spiral galaxies.
Very good for classroom.
- Planetary migration - FARGO3D | 2:28:
Good with
graph to show decrease
in mean orbital radius
with planetary migration.
No narration.
Jump to 40 second mark.
Show a bit to the classroom.
- Planetary Formation Process | 1:00:
Good and shows
molecular cloud and
then planet formation.
Authoritative imagery since the credit is Gemini Observatory/STScI.
Appropriate music.
Short enough for classroom.
- Formation of a planetary system | 0:20:
Seems good.
You see a planet forming in the swirl of
protoplanetary disk.
- Hubble Source |
Stellar Disk and Planet Formation | 0:30:
Seems good.
There is bipolar outflow due
to magnetic fields too---but it seems only
a monopolar one.
You time-leap and a
planet that emerged form the swirl of
protoplanetary disk.
It has an umbra.
Short enough for the classroom.
- Sport videos:
php require("/home/jeffery/public_html/astro/sport/sport_videos.html");?>
Local file: local link: planetary_system_formation_videos.html.
File: Planetary systems file:
planetary_system_formation_videos.html.