almogyalin - Network

Some stars lose mass as stellar wind, and when that star is orbiting a companion, the binary motion excites spiral density waves in the wind...

Some stars lose mass as stellar wind, and when that star is orbiting a companion, the binary motion excites spiral density waves in the wind nebula

Demonstration of the spiral pattern that forms in an accretion disc around an align, spinning black hole due to the Bardeen Petterson...

Demonstration of the spiral pattern that forms in an accretion disc around an align, spinning black hole due to the Bardeen Petterson effect

https://theoretical-physics-digest.fandom.com/wiki/Bardeen_Petterson_Effect

Hydrodynamic simulation of an air burst. The lower portion of the domain (y<-5) is filled with a high density medium so that the shock...

Hydrodynamic simulation of an air burst. The lower portion of the domain (y<-5) is filled with a high density medium so that the shock reflects from it. The things that form at the point where the shock front intersects the boundary between the media are called Mach branches

Rayleigh Taylor instability

Rayleigh Taylor instability

Passage of dense impactor through a tenuous medium

Passage of dense impactor through a tenuous medium

Animation of Lloyd's method for regularising a Voronoi tessellation

Animation of Lloyd's method for regularising a Voronoi tessellation

Simulation of a deflagration to detonation transition close to the surface of a white dwarf

Simulation of a deflagration to detonation transition close to the surface of a white dwarf

Turbulence excited by supernova explosions

Turbulence excited by supernova explosions

Laminar flow around an obstacle

Laminar flow around an obstacle

Propagation of a supernova explosion in a clumpy interstellar medium

Propagation of a supernova explosion in a clumpy interstellar medium

Development of hydrodynamic instabilities during implosion. Perturbations have six-fold symmetry due to the use of a hexagonal grid

Development of hydrodynamic instabilities during implosion. Perturbations have six-fold symmetry due to the use of a hexagonal grid

Presentation of the derivation of the Eddington luminosity using manim

Presentation of the derivation of the Eddington luminosity using manim

Simulation of a surface explosion - an impact event sans impactor

Simulation of a surface explosion - an impact event sans impactor

Kelvin Helmholtz instability. Top portion moves to the left, while bottom moves to the right. Colour represent initial velocity

Kelvin Helmholtz instability. Top portion moves to the left, while bottom moves to the right. Colour represent initial velocity

Formation of a high mach number bow shock around a perfectly rigid spherical obstacle

Formation of a high mach number bow shock around a perfectly rigid spherical obstacle

Hydrodynamic simulations of high velocity collisions of strengthless objects

Hydrodynamic simulations of high velocity collisions of strengthless objects

Mutual gravitational interaction of three planets of equal masses. Orbits are represented by circular lines, while the arrows at the centre...

Mutual gravitational interaction of three planets of equal masses. Orbits are represented by circular lines, while the arrows at the centre represent the eccentricity vector. In the left all planets are moving prograde, while to the right the middle planet is moving retrograde, and stabilises the system.

In this visualisation I continuously inject particles (colour indicates initial position, where lighter = higher), which move in a Brownlian...

In this visualisation I continuously inject particles (colour indicates initial position, where lighter = higher), which move in a Brownlian way in the vertical direction, while simultaneously experiencing a downward drift velocity, which increase as one moves to the right.