<p>You are correct - when we look at stars in the sky, about half of them are actually binary systems, with a range of separations. The frequency of binarity is strongly mass dependent; the 50% figure is appropriate for stars like the Sun, but it appears to be closer to 100% for high-mass O-stars and as small as 20% for the lowest mass M-dwarf stars.
There is also a change in the separation (and corresponding orbital period) distribution. The distributions of separations looks "log-normal" (like a Gaussian when you plot log separation on the x-axis). For solar type stars the peak is at around 50-100 au, but binaries become more compact (maybe 10-30 au) for low-mass stars. There is a tail of binaries with much smaller and larger separations.</p>

<p>These observational data are explained (or are in the process of being explained) as a combination of nature and nurture. The basic process of star formation results from the collapse and fragmentation of molecular clouds. If a collapsing fragment has significant angular momentum then the most energetically favourable way it can continue to collapse whilst conserving angular momentum is to sub-fragment into two pieces orbiting each other. This is thought to be the most basic binary formation process. Other processes include the formation of low mass companions through instabilities in cicumstellar disks or interactions between young stars in dense protostellar environments. Exactly how this leads to the mass dependence of the binary frequency and separation distribution is a topic of contemporary research; there is no definitive answer I can give.</p>

<p>After that I think there are two basic ways, or rather two basic locations, in which planets could form in a binary stem. Either around one or other of the stars or as circumbinary objects. The likelihood of each will depend how and when the binary formed, the binary component separation and mass ratio. </p>

<p>The planets would likely form in the same way that they do around single stars. If the binary star components are originally formed close together, there could be a circumbinary disk from which a stable planetary system formed. Both circumbinary disks and circumbinary planets have been observed.</p>

<p>Disks around individual components are truncated by tidal forces at a radius <em>roughly</em> corresponding to a third of the binary separation. Inside this radius it may be possible to form planets. Thus widely separated binaries could have planets orbiting the individual stars. </p>

CC BY-SA 3.0
2015-09-12T08:52:41.853Z
2015-09-12T08:52:41.853Z
ProfRob
<p>Alpha Centauri, which is a binary star, is likely to have planets (they may have been detected, but not everyone is convinced).  The most likely scenario for planets to form stably would be if the two stars were widely separated.  For instance, a pair consisting of a sun-like star and a small red dwarf at a distance of 50 AU apart would allow plenty of room around the sun-like star for planet formation.  In fact, if there were a 90 Jupiter-mass red dwarf orbiting our sun at a distance of 50 AU, it would have less gravitation pull on us than Jupiter does.</p>

CC BY-SA 3.0
2015-08-12T18:23:22.153Z
While this may be true for the suggested case, does this mean that all binary stars are initially 50 AU or more apart?  Wouldn't the presence of such a large ratio of binary systems suggest that the orbits of these systems are stable over long periods of time, and not migrating?
jkyrouac
CC BY-SA 3.0
2015-08-12T20:06:59.623Z
It seems the median orbital period for binary systems is 14 years, which assuming a single solar mass system would be about 6 AU [ref](http://adsabs.harvard.edu/abs/1991A%26A...248..485D).  The system HM Cancri, orbits at about 0.0005 AU about every 5 minutes, which, while a white dwarf pair, has about 1 solar mass in total. [space](http://www.popsci.com/technology/article/2010-03/fastest-binary-stars-ever-discovered-spin-310-miles-second)
jkyrouac
CC BY-SA 3.0
2015-09-12T09:05:55.987Z
@jkyrouac The first conclusion of the well-known paper you link to is that the median orbital period is **180 years**. This means the median separation ends up being around 50 au or so.
ProfRob
CC BY-SA 3.0
2015-08-12T03:33:06.850Z
2015-08-12T03:33:06.850Z
user7935
<p>It has been reported that perhaps half of nearby sun-like stars are found in multiple systems.</p>

<p>Why is this so common, and how do planets form in such a situation?</p>

<p>Kaitlin M. Kratter, “Sibling Rivalry Begins at Birth,” Nature, Vol. 518, 12 February 2015, p. 173</p>

CC BY-SA 3.0
2015-08-06T19:48:08.680Z
The short of the matter is that a collapsing cloud of dust tends to do so asymmetrically.  Smaller regions inside of it collapse together faster than everything is going to the center of the entire cloud's collapse.  In this way one (large) cloud of collapsing dust can produce many nearby stars.  For reasons I'm not qualified to expound upon our understanding of, this results in the majority of stars (Sun-like or otherwise) being in gravitationally bound systems with at least one other star.
zibadawa timmy
CC BY-SA 3.0
2015-08-06T21:21:14.523Z
To reinforce zibadawa's point, consider that even our solar system has Jupiter, which although much smaller than the Sun is still a significant secondary mass concentration in the solar system.
called2voyage
CC BY-SA 3.0
2015-08-07T00:50:13.157Z
50% of all stars are binaries. We do not know how many planets in general those host. We only have an idea about Single G stars, some single G and M (upcoming with Kepler2) and only in a certain mass and radius range. It therefore may take still several decades to answer your question.
AtmosphericPrisonEscape
CC BY-SA 3.0
2015-08-08T10:54:59.943Z
50% of all stars may be in binary (or more) systems but I think it's better to count by solarsystem, for example, if you count by star a binary is 2 and a single star system is one, if you count by system, it's 1-1.   About 2/3rds of sun like stars are in binary systems (see link).  and larger solar systems appear more likely to form into a binary (or more) system.   Most stars are M stars and most of those aren't binary.    http://www.space.com/7792-double-sunsets-common-twin-star-setups-mysterious.html    Planet formation for binary systems has been observed, but I don't think much is known.
userLTK
<exoplanet><binary-star>
Why are so many sun-like stars found in multiple systems? How do planets form in such a situation?
jkyrouac
# Why are so many sun-like stars found in multiple systems? How do planets form in such a situation?

(Asked by: username_0 on 2015-08-06)

It has been reported that perhaps half of nearby sun-like stars are found in multiple systems.

Why is this so common, and how do planets form in such a situation?

Kaitlin M. Kratter, “Sibling Rivalry Begins at Birth,” Nature, Vol. 518, 12 February 2015, p. 173

**Tags:** exoplanet, binary-star

> **Comments:**
> **username_1**: The short of the matter is that a collapsing cloud of dust tends to do so asymmetrically.  Smaller regions inside of it collapse together faster than everything is going to the center of the entire cloud's collapse.  In this way one (large) cloud of collapsing dust can produce many nearby stars.  For reasons I'm not qualified to expound upon our understanding of, this results in the majority of stars (Sun-like or otherwise) being in gravitationally bound systems with at least one other star.  
> **username_2**: To reinforce username_1's point, consider that even our solar system has Jupiter, which although much smaller than the Sun is still a significant secondary mass concentration in the solar system.  
> **username_3**: 50% of all stars are binaries. We do not know how many planets in general those host. We only have an idea about Single G stars, some single G and M (upcoming with Kepler2) and only in a certain mass and radius range. It therefore may take still several decades to answer your question.  
> **username_4**: 50% of all stars may be in binary (or more) systems but I think it's better to count by solarsystem, for example, if you count by star a binary is 2 and a single star system is one, if you count by system, it's 1-1.   About 2/3rds of sun like stars are in binary systems (see link).  and larger solar systems appear more likely to form into a binary (or more) system.   Most stars are M stars and most of those aren't binary.    http://www.space.com/7792-double-sunsets-common-twin-star-setups-mysterious.html    Planet formation for binary systems has been observed, but I don't think much is known.  

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## 2 answers

### Answer by username_5 on 2015-09-12. Score: 2

You are correct - when we look at stars in the sky, about half of them are actually binary systems, with a range of separations. The frequency of binarity is strongly mass dependent; the 50% figure is appropriate for stars like the Sun, but it appears to be closer to 100% for high-mass O-stars and as small as 20% for the lowest mass M-dwarf stars.
There is also a change in the separation (and corresponding orbital period) distribution. The distributions of separations looks "log-normal" (like a Gaussian when you plot log separation on the x-axis). For solar type stars the peak is at around 50-100 au, but binaries become more compact (maybe 10-30 au) for low-mass stars. There is a tail of binaries with much smaller and larger separations.

These observational data are explained (or are in the process of being explained) as a combination of nature and nurture. The basic process of star formation results from the collapse and fragmentation of molecular clouds. If a collapsing fragment has significant angular momentum then the most energetically favourable way it can continue to collapse whilst conserving angular momentum is to sub-fragment into two pieces orbiting each other. This is thought to be the most basic binary formation process. Other processes include the formation of low mass companions through instabilities in cicumstellar disks or interactions between young stars in dense protostellar environments. Exactly how this leads to the mass dependence of the binary frequency and separation distribution is a topic of contemporary research; there is no definitive answer I can give.

After that I think there are two basic ways, or rather two basic locations, in which planets could form in a binary stem. Either around one or other of the stars or as circumbinary objects. The likelihood of each will depend how and when the binary formed, the binary component separation and mass ratio.

The planets would likely form in the same way that they do around single stars. If the binary star components are originally formed close together, there could be a circumbinary disk from which a stable planetary system formed. Both circumbinary disks and circumbinary planets have been observed.

Disks around individual components are truncated by tidal forces at a radius *roughly* corresponding to a third of the binary separation. Inside this radius it may be possible to form planets. Thus widely separated binaries could have planets orbiting the individual stars.


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### Answer by username_6 on 2015-08-12. Score: 0

Alpha Centauri, which is a binary star, is likely to have planets (they may have been detected, but not everyone is convinced). The most likely scenario for planets to form stably would be if the two stars were widely separated. For instance, a pair consisting of a sun-like star and a small red dwarf at a distance of 50 AU apart would allow plenty of room around the sun-like star for planet formation. In fact, if there were a 90 Jupiter-mass red dwarf orbiting our sun at a distance of 50 AU, it would have less gravitation pull on us than Jupiter does.

> **Comments:**
> **username_0**: While this may be true for the suggested case, does this mean that all binary stars are initially 50 AU or more apart?  Wouldn't the presence of such a large ratio of binary systems suggest that the orbits of these systems are stable over long periods of time, and not migrating?  
> **username_0**: It seems the median orbital period for binary systems is 14 years, which assuming a single solar mass system would be about 6 AU [ref](http://adsabs.harvard.edu/abs/1991A%26A...248..485D).  The system HM Cancri, orbits at about 0.0005 AU about every 5 minutes, which, while a white dwarf pair, has about 1 solar mass in total. [space](http://www.popsci.com/technology/article/2010-03/fastest-binary-stars-ever-discovered-spin-310-miles-second)  
> **username_5**: @username_0 The first conclusion of the well-known paper you link to is that the median orbital period is **180 years**. This means the median separation ends up being around 50 au or so.  

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