Youtor
Achernar SpaceSim
>> YOUR LINK HERE: ___ http://youtube.com/watch?v=CWShFUx_bKQ
This is a simulation of Achernar, the brightest example of a Be-type star in our sky. Be type stars are rapidly spinning B-type stars which can form a disk around themselves due to their rapid rotation, as showcased in this simulation. • The colors correspond to temperatures, roughly equating to their blackbody temperature's color. Reds are cool, blues are hot, dark blue is the hottest temperatures present. In-simulation, this takes place over a bit more than 4 months, while the simulation ran in real life in less than 2 days, if I remember correctly (I have been very busy since I ran the simulation so i don't remember exactly) • This simulation was inspired by an idea I had for a what-if simulation to give the Sun a rapid spin, I found that it formed a disk and wondered if there actually were stars where that could happen. I wasn't expecting to find anything but was pleasantly surprised to find the info about Be stars and decided to make a full simulation based on one, Achernar seemed like a good one to model. I tried to model it as accurately as possible in SpaceSim, so given what the software models this should be at least close to the real case. • Here is a paper on Be stars, in case you're curious: • https://arxiv.org/abs/1310.3962 • The thumbnail is art I did of this star based on what I read of the paper above, and info about Achernar specifically. This art can be found on my ArtStation here: • https://www.artstation.com/artwork/bl... • In the beginning, the rapid rotation of the star immediately pulls material outward, which is then less supported by the material underneath it, so it falls back down, and does so with enough force to compress into the material below. This causes it to rebound back out, forming a bounce motion to the star as a whole, from which the star then stabilizes. This should not be taken as a real physical process but rather as the simulation finding the stable equilibrium point. After this, the material near the equator slowly begins to pinch out into a disk. • 0:00 Simulation finding equilibrium. • 0:20 Equilibrium oblate spheroid shape is reached. • 1:00 Material slowly lifting off the equator slows down, stretching the temperature difference patterns on the star's surface. • 1:30 Particles begin to break off the star and form the decretion disk. • 8:30 The disk begins to separate from the star, particles with enough velocity staying in the disk while ones without fall to the surface. • I recommend watching at 2x playback speed.
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