Interacting galaxy
Galaxies with interacting gravitational fields From Wikipedia, the free encyclopedia
Galaxies with interacting gravitational fields From Wikipedia, the free encyclopedia
Interacting galaxies (colliding galaxies) are galaxies whose gravitational fields result in a disturbance of one another. An example of a minor interaction is a satellite galaxy disturbing the primary galaxy's spiral arms. An example of a major interaction is a galactic collision, which may lead to a galaxy merger.
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A giant galaxy interacting with its satellites is common. A satellite's gravity could attract one of the primary's spiral arms. Alternatively, the secondary satellite can dive into the primary galaxy, as in the Sagittarius Dwarf Elliptical Galaxy diving into the Milky Way. That can possibly trigger a small amount of star formation. Such orphaned clusters of stars were sometimes referred to as "blue blobs" before they were recognized as stars.[1]
Colliding galaxies are common during galaxy evolution.[3] The extremely tenuous distribution of matter in galaxies means these are not collisions in the traditional sense of the word, but rather gravitational interactions.
Colliding may lead to merging if two galaxies collide and do not have enough momentum to continue traveling after the collision. As with other galaxy collisions, the merging of two galaxies may create a starburst region of new stars.[4] In that case, they fall back into each other and eventually merge into one galaxy after many passes through each other. If one of the colliding galaxies is much larger than the other, it will remain largely intact after the merger. The larger galaxy will look much the same, while the smaller galaxy will be stripped apart and become part of the larger galaxy. When galaxies pass through each other, unlike during mergers, they largely retain their material and shape after the pass.
Galactic collisions are now frequently simulated on computers, which use realistic physics principles, including the simulation of gravitational forces, gas dissipation phenomena, star formation, and feedback. Dynamical friction slows the relative motion of galaxy pairs, which may possibly merge at some point, according to the initial relative energy of the orbits. A library of simulated galaxy collisions can be found at the Paris Observatory website GALMER.[5]
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Galactic cannibalism is a common phenomenon.[16] It refers to the process in which a large galaxy, through tidal gravitational interactions with a companion, merges with that companion. The most common result of the gravitational merger between two or more galaxies is a larger irregular galaxy, but elliptical galaxies may also result.
It has been suggested that galactic cannibalism is currently occurring between the Milky Way and the Large and Small Magellanic Clouds. Streams of gravitationally-attracted hydrogen arcing from these dwarf galaxies to the Milky Way is taken as evidence for the theory.
Galaxy harassment is a type of interaction between a low-luminosity galaxy and a brighter one that takes place within rich galaxy clusters, such as Virgo and Coma, where galaxies are moving at high relative speeds and suffering frequent encounters with other systems of the cluster due to the high galactic density.
According to computer simulations, the interactions convert the affected galaxy disks into disturbed barred spiral galaxies and produces starbursts followed by, if more encounters occur, loss of angular momentum and heating of their gas. The result would be the conversion of (late type) low-luminosity spiral galaxies into dwarf spheroidals and dwarf ellipticals.[17]
Evidence for the hypothesis had been claimed by studying early-type dwarf galaxies in the Virgo Cluster and finding structures, such as disks and spiral arms, which suggest they are former disc systems transformed by the above-mentioned interactions.[18] The existence of similar structures in isolated early-type dwarf galaxies, such as LEDA 2108986, has undermined this hypothesis.[19][20]
| Name | Type | Distance (million ly) |
Magnitude | Notes |
|---|---|---|---|---|
| Milky Way Galaxy, LMC and SMC | SBc/SB(s)m/SB(s)m pec | 0 | Satellites interacting with their primary | |
| Whirlpool Galaxy (M51) | SAc (SB0-a) | 37 | +8.4 | Satellite interacting with its primary |
| NGC 1097 | SB(s)bc (E6) | 45 | +9.5 | Satellite interacting with its primary |
| Butterfly Galaxies NGC 4567/8 | SA(rs)bc / SA(rs)bc | 60 | +10.9 | Early phase of interaction |
| NGC 2207 and IC 2163 | SAc/SAbc | 114 | +11 | Galaxies going through the first phase in galactic collision |
| Mice Galaxies (NGC 4676A and NGC 4676B) | S0/SB(s)ab | 300 | +13.5 | Galaxies going through the second phase in galactic collision |
| Antennae Galaxies (NGC 4038/9) | SAc/SBm | 45 | +10.3 | Galaxies going through the third phase in galactic collision |
| NGC 520 | S | 100 | +11.3 | Galaxies going through the third phase in galactic collision |
| NGC 2936 | Irr | 352 | +12.9 | ? |
Astronomers have estimated the Milky Way Galaxy will collide with the Andromeda Galaxy in about 4.5 billion years. Some think the two spiral galaxies will eventually merge to become an elliptical galaxy[21][22] or perhaps a large disc galaxy.[23]
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