User talk:Sentientstarstuff/sandbox

Daniel's Review

Galaxies which encounter one another from certain directions may interact: collide, merge, rip each other apart, or transfer some member objects( give an example of a member object transfer).

In these situations, it can be difficult to tell where one galaxy ends and where another begins. "Collisions" between galaxies do not necessarily involve collisions between objects from one galaxy and objects from the other, since galaxies are mostly composed of empty space. Rather, gravitational forces from nearby clouds[4] of matter are capable of distorting one another, or bringing a clump of mass from one galaxy over into another. 

Despite also being satellites of host galaxies, globular clusters should not be mistaken for satellite galaxies. Apart from satellite galaxies being more extended and diffuse compared to globular clusters, the primary distinguishing feature between these two objects is that satellite galaxies are enshrouded in massive dark-matter halos.[5 ( Might also point out that GC's have a very different origin of formation.

Furthermore, in this model dwarfs galaxies are considered to be the fundamental building blocks that give rise to more massive galaxies, and the satellites that are observed around these galaxies are the dwarfs that have yet to be consumed by their host. ( you might want to go into details about hierarchal formation in the context of the role satellites play, (and maybe use the milky way merging with its satellites as an example. )

Make this next section less technical and more descriptive. I really enjoy the section describing the role satellites play in galaxy formation, perhaps express all this in layman's terms.

A crude yet useful method to determine how dark matter halos progressively gain mass through mergers of less massive halos can be explained using the excursion set formalism, also known as the extended Press-Schechter formalism (EPS. This is used to determine the average number of progenitors at time within the mass interval that have merged to produce a halo at time . This is accomplished by considering a spherical region of mass with a corresponding mass variance that is defined to ensure that a collapsed object is formed at . Then earlier content follows.

(i.e. mass-overdensity space) perhaps explain what mass over-density space is in layman's terms and why its useful for this calculation Stars are interacting in all directions and thus trace out trajectories that are described well by Markovian random walks. — Preceding unsigned comment added by Dfmckeown (talk • contribs) 22:02, 7 June 2018 (UTC)