<p>There are two main theories for the formation of binary stars - one accepted, and one mainly deprecated.</p>

<ol>
<li><strong><a href="http://www.phys.lsu.edu/astro/nap98/bf.final.html" rel="noreferrer">The fission hypothesis.</a></strong> The fission hypothesis states that the binary system forms after the collapse of the original gas cloud into a protostar. Angular momentum is conserved, so as the extremely large cloud slowly contracts, it spins faster. After enough time, the protostar could form a dumbbell shape, one part of which eventually breaks off. There are now two blobs, and thus two protostars, which will evolve into a binary star system.</li>
<li><strong><a href="http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1988ComAp..12..169B&amp;defaultprint=YES&amp;filetype=.pdf" rel="noreferrer">The fragmentation hypothesis.</a></strong> The fragmentation hypothesis states that the gas cloud <em>fragments</em> earlier on, due to some instability or cooling/heating effects. Each of the two fragments then evolves separately, forming a binary star system.</li>
</ol>

<p>The fission hypothesis is no longer favored. It cannot explain the existence of systems with certain mass ratios or separations. The fragmentation hypothesis, however, can, and <em>is</em> accepted. It is also possible for a binary system to form through the capture of one star by another, but that requires a third body, and probably cannot explain the high fraction of binary systems in the galaxy.</p>

<p>Basically, then, the main theory to date is that the protostellar nebula breaks up, and then both fragments collapse independently.</p>

CC BY-SA 3.0
2017-04-04T09:53:56.160Z
Just as a point of interest:
Capture of one star by another through N-body interactions cannot explain the number of binaries as stated but if you are only looking at creating binaries it is interesting to note that this mechanism is exceptionally important in explaining observations of globular clusters where binaries are continuously created in the core. References: 

[1]Hurley, J. and Shara, M. (2012). A direct n-body model of core-collapse and core oscillations.

[2]Joshi et al. (2000). Monte carlo simulations of globular cluster evolution. I. methods and test calculations.
AspicioAstra
CC BY-SA 3.0
2017-03-17T19:05:26.737Z
2017-03-17T19:05:26.737Z
HDE 226868
<p>That's a really good question. I'll explain as best as I can, there are about a number of ways this can happen.</p>

<ol>
<li>Fragmentation, as the protostar forms, the disk may fragment under its own gravity, or like the method listed below, it may rotate enough until some of the mass breaks off so another star may form.</li>
<li>Accretion, another object in the system may "steal" matter from the forming star, and when it's mass reaches a high enough point, a second star may start to form.</li>
<li>Breaking up, if the star rotates fast enough, it may split apart into two separate stars. But like HDE 226868 said, it is no longer favored.</li>
<li>Normal formation, when the stars are forming, both may acquire enough mass without any of these effects to form a binary system.</li>
<li>Capture, a nearby star may capture another so that they orbit each other.</li>
</ol>

<p>Keep in mind that there are probably more ways for binary stars to form. Also, a collision isn't very likely to form these systems.</p>

CC BY-SA 3.0
2017-03-17T21:14:27.243Z
2017-03-17T21:14:27.243Z
StellarExile
<p>I don't know how common it is for a system to have two stars (or perhaps even more) but how do they arise? Is that due to the stellar accretion disc, or the composition of the stellar nebula? 
Or are most of them created by a collision of stars?</p>

CC BY-SA 3.0
2017-03-17T19:08:23.677Z
Just out of interest, check out [this question on the frequency of stellar multiplicities](http://astronomy.stackexchange.com/questions/18604/multiple-star-system-percentages/18608#18608). The general consensus seems to be that $\sim20-30\%$ of all stellar systems are binary systems.
zephyr
CC BY-SA 3.0
2017-03-18T01:20:46.613Z
With a *lot* of 1s and 0s. (Sorry, couldn't resist).
magma
<star><star-formation><binary-star>
How are binary star systems created?
Marijn 
# How are binary star systems created?

(Asked by: username_0 on 2017-03-17)

I don't know how common it is for a system to have two stars (or perhaps even more) but how do they arise? Is that due to the stellar accretion disc, or the composition of the stellar nebula?
Or are most of them created by a collision of stars?

**Tags:** star, star-formation, binary-star

> **Comments:**
> **username_1**: Just out of interest, check out [this question on the frequency of stellar multiplicities](http://astronomy.stackexchange.com/questions/18604/multiple-star-system-percentages/18608#18608). The general consensus seems to be that $\sim20-30\%$ of all stellar systems are binary systems.  
> **username_2**: With a *lot* of 1s and 0s. (Sorry, couldn't resist).  

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## 2 answers

### Answer by username_3 on 2017-03-17. Score: 13

There are two main theories for the formation of binary stars - one accepted, and one mainly deprecated.

1. **[The fission hypothesis.](http://www.phys.lsu.edu/astro/nap98/bf.final.html)** The fission hypothesis states that the binary system forms after the collapse of the original gas cloud into a protostar. Angular momentum is conserved, so as the extremely large cloud slowly contracts, it spins faster. After enough time, the protostar could form a dumbbell shape, one part of which eventually breaks off. There are now two blobs, and thus two protostars, which will evolve into a binary star system.
2. **[The fragmentation hypothesis.](http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1988ComAp..12..169B&defaultprint=YES&filetype=.pdf)** The fragmentation hypothesis states that the gas cloud *fragments* earlier on, due to some instability or cooling/heating effects. Each of the two fragments then evolves separately, forming a binary star system.

The fission hypothesis is no longer favored. It cannot explain the existence of systems with certain mass ratios or separations. The fragmentation hypothesis, however, can, and *is* accepted. It is also possible for a binary system to form through the capture of one star by another, but that requires a third body, and probably cannot explain the high fraction of binary systems in the galaxy.

Basically, then, the main theory to date is that the protostellar nebula breaks up, and then both fragments collapse independently.

> **Comments:**
> **username_4**: Just as a point of interest: Capture of one star by another through N-body interactions cannot explain the number of binaries as stated but if you are only looking at creating binaries it is interesting to note that this mechanism is exceptionally important in explaining observations of globular clusters where binaries are continuously created in the core. References:   [1]Hurley, J. and Shara, M. (2012). A direct n-body model of core-collapse and core oscillations.  [2]Joshi et al. (2000). Monte carlo simulations of globular cluster evolution. I. methods and test calculations.  

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### Answer by username_5 on 2017-03-17. Score: 4

That's a really good question. I'll explain as best as I can, there are about a number of ways this can happen.

1. Fragmentation, as the protostar forms, the disk may fragment under its own gravity, or like the method listed below, it may rotate enough until some of the mass breaks off so another star may form.
2. Accretion, another object in the system may "steal" matter from the forming star, and when it's mass reaches a high enough point, a second star may start to form.
3. Breaking up, if the star rotates fast enough, it may split apart into two separate stars. But like HDE username_3 said, it is no longer favored.
4. Normal formation, when the stars are forming, both may acquire enough mass without any of these effects to form a binary system.
5. Capture, a nearby star may capture another so that they orbit each other.

Keep in mind that there are probably more ways for binary stars to form. Also, a collision isn't very likely to form these systems.


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