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[[Image:Solar Magnetic Field Lines.jpg|thumb|The magnetic field lines rotate together with the Sun as a solid object. Ionized material carried along the field lines will at some point <math> r_c </math> escape the magnetic field lines and thus take away the Sun's angular momentum]]
'''Magnetic braking''' is a theory explaining the loss of solar [[angular momentum]] due to material getting captured by the [[solar magnetic field]] and thrown out at great distance from the surface of the Sun.


==The problem==
The currently accepted theory of the [[solar systems|solar system's]] evolution states that the Solar System originates from a contracting gas cloud. As the cloud contracts, the [[angular momentum]] <math> L</math> must be [[angular momentum#Conservation of angular momentum|conserved]]. Any small net rotation of the cloud will cause the spin to increase as the cloud collapses, forcing the material into a rotating disk. At the dense center of this disk a [[protostar]] forms, which gains heat from the [[gravitational energy]] of the collapse. As the collapse continues, the rotation rate can increase to the point where the accreting protostar can break up due to [[centrifugal force]] at the equator.


Thus the rotation rate must be braked during the first 100,000 years of the star's life to avoid this scenario. One possible explanation for the braking is the interaction of the protostar's magnetic field with the stellar wind. In the case of our own Sun, when the planets' angular momenta are compared to the Sun's own, the Sun has less than 1% of its supposed angular momentum. In other words, the Sun has slowed down its spin while the planets have not.
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==The idea behind magnetic braking==
Ionized material captured by the magnetic field lines will rotate with the Sun as if it were a solid body. As material escapes from the Sun due to the [[Solar wind]], the highly ionized material will be captured by the field lines and rotate with the same angular velocity as the Sun, even though it is carried far away from the Sun's surface, until it eventually escapes. This effect of carrying mass far from the centre of the Sun and throwing it away robs the Sun of its spin.<ref>{{cite journal |authors=Ferreira, J.; Pelletier, G.; Appl, S. |title=Reconnection X-winds: spin-down of low-mass protostars |journal=Monthly Notices of the Royal Astronomical Society |year=2000 |volume=312 |issue=2 |pages=387–397 |bibcode=2000MNRAS.312..387F |doi=10.1046/j.1365-8711.2000.03215.x }}</ref><ref>{{cite news |first=Terry |last=Devitt |title=What Puts The Brakes On Madly Spinning Stars? |publisher=University of Wisconsin-Madison |date=January 31, 2001 |url=http://www.news.wisc.edu/5732 |accessdate=2007-06-27 }}</ref> The same effect is used in slowing the spin of a [[Yo-yo de-spin|rotating satellite]]; here two wires spool out weights to a distance slowing the satellites spin, then the wires are cut, letting the weights escape into space and permanently robbing the spacecraft of its [[angular momentum]].
 
==Theory behind magnetic braking==
{{unreferenced section|date=April 2013}}
{{original research section|date=April 2013}}
As ionized material follows the Sun's magnetic field lines, due to the effect of the field lines being frozen in the [[plasma (physics)|plasma]], the charged particles feel a force <math> \mathbf{F} </math> of the magnitude:
:<math> \mathbf{F}=q \mathbf{v} \times \mathbf{B} </math>
where <math>q</math> is the charge, <math>\mathbf{v}</math> is the velocity and <math>\mathbf{B}</math> is the magnetic field vector. This bending action forces the particles to "[[corkscrew]]" around the magnetic field lines while held in place by a "magnetic pressure"<math> P_B </math>, or "energy density", while rotating together with the Sun as a solid body:
 
:<math>P_B=\frac{B^2}{2 \mu_0} </math>
 
Since magnetic field strength decreases with the cube of the distance there will be a place where the kinetic gas pressure <math> P_g </math> of the ionized gas is great enough to break away from the field lines:
 
:<math> P_g=n m v^2 </math>
where n is the number of particles, m is the mass of the individual particle and v is the radial velocity away form the Sun, or the speed of the solar wind.
 
The magnetic field strength as a function of radius can be approximated as:
:<math> B(r)=\frac{D_\odot}{r^3}  </math>
 
The critical distance where the material will break away from the field lines can then be calculated as the distance where the kinetic pressure and the magnetic pressure are equal, i.e.
:<math> P_B=P_g \Rightarrow</math>
 
:<math> \frac{B(rc)^2}{2\mu_0}=n m v^2\Rightarrow</math>
 
:<math> \frac{D_{\odot}^2}{2\mu_0 r_c^6}=n m v^2</math>
 
If the solar mass loss is omni-directional then the mass loss <math>n m= \frac{dM/dt}{4\pi r^2 v}</math>; plugging this into the above equation and isolating the critical radius it follows that
:<math>r_c=\left(\frac{2\pi D_\odot ^2}{\mu_0 v \dot{M}}\right)^{1 \over 4}</math>
 
===Present day value===
Currently it is estimated that:
* The mass loss of the Sun is about <math>\dot{M}=dM/dt=2 \cdot 10^9 kg/s</math>
* The solar wind speed is  <math>v=5\cdot10^5m/s</math>
* The dipole field is <math>D_{\odot}=8 \cdot 10^{22} T m^3</math>
 
This leads to a critical radius <math>r_c =3.4 R_\odot</math>. This means that the ionized plasma will rotate together with the Sun as a solid body until it reaches a distance of nearly 3.4 the radius of the Sun; from there the material will break off and stop affecting the Sun.
 
The amount of solar mass needed to be thrown out along the field lines to make the Sun completely stop rotating can then be calculated using the specific angular momentum:
:<math>\frac{j_\odot}{j_c}=\left(\frac{R_\odot}{r_c}\right)^2 \approx 10%</math>
About 1/10 of the solar mass should thus have be lost by now due to this effect, but if the present mass loss rate was stable throughout the Sun's "life" only about 0.01% of the Sun's original mass would have been lost. This indicates that either the Sun's mass loss must have been higher in the past or that the Sun's magnetic field has been much stronger.
 
==References==
{{reflist}}
 
==See also==
* [[Stellar magnetic field]]
* [[Stellar rotation]]
 
[[Category:Conservation laws]]
[[Category:Concepts in physics]]
[[Category:Physical quantities]]
[[Category:Rotation]]
[[Category:Rotational symmetry]]

Latest revision as of 18:22, 24 March 2014


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