Magnetic field

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In physics, a magnetic field (commonly denoted by H) describes a magnetic field (a vector) at every point in space; it is a vector field. In non-relativistic physics, the space in question is the three-dimensional Euclidean space ${\displaystyle \mathbb {E} ^{3}}$—the infinite world that we live in.

In general H is seen as an auxiliary field useful when a magnetizable medium is present. The magnetic flux density B is usually seen as the fundamental magnetic field, see the article about B for more details about magnetism.

The SI unit of magnetic field strength is ampere⋅turn/meter; a unit that is based on the magnetic field of a solenoid. In the Gaussian system of units |H| has the unit oersted, with one oersted being equivalent to (1000/4π)⋅A⋅turn/m.

Relation between H and B[edit]

The magnetic field H is closely related to the magnetic induction B (also a vector field). It is the vector B that enters the expression for magnetic force on moving charges (Lorentz force). Historically, the theory of magnetism developed from Coulomb's law, where H played a pivotal role and B was an auxiliary field, which explains its historic name "magnetic induction". At present the roles have swapped and some authors give B the name magnetic field (and do not give a name to H other than "auxiliary field").

In the general case, H is introduced in terms of B as:

${\displaystyle {\begin{aligned}\mathbf {H} &={\frac {1}{\mu _{0}}}\mathbf {B} -\mathbf {M} \qquad &{\hbox{in SI units}}\\\mathbf {H} &=\mathbf {B} -4\pi \mathbf {M} \qquad \;\;&{\hbox{in Gaussian units}},\\\end{aligned}}}$

with M(r, t) the magnetization of the medium.

For the most common case of linear materials, M is linear in H,^[1] and in SI units,

${\displaystyle \mathbf {B} =\mu _{0}(\mathbf {1} +{\boldsymbol {\chi }})\mathbf {H} ,}$

where 1 is the 3×3 unit matrix, χ the magnetic susceptibility tensor of the magnetizable medium, and μ₀ the magnetic permeability of the vacuum (also known as magnetic constant). In Gaussian units the relation is

${\displaystyle \mathbf {B} =(\mathbf {1} +4\pi {\boldsymbol {\chi }})\mathbf {H} ,}$

Many non-ferromagnetic materials are linear and isotropic; in the isotropic case the susceptibility tensor is equal to χ_m1, and H can easily be solved (in SI units)

${\displaystyle \mathbf {H} ={\frac {\mathbf {B} }{\mu _{0}(1+\chi _{m})}}\equiv {\frac {\mathbf {B} }{\mu _{0}\mu _{r}}},}$

with the relative magnetic permeability μ_r = 1 + χ_m.

For example, at standard temperature and pressure (STP) air, a mixture of paramagnetic oxygen and diamagnetic nitrogen, is paramagnetic (i.e., has positive χ_m), the χ_m of air is 4⋅10⁻⁷. Argon at STP is diamagnetic with χ_m = −1⋅10⁻⁸. For most ferromagnetic materials χ_m depends on H, with a non-linear relation between H and B and is large (depending on the material) from, say, 50 to 10000 and strongly varying as a function of H.

The magnetic flux density B is a solenoidal (divergence-free, transverse) vector field because of one of Maxwell's equations

${\displaystyle {\boldsymbol {\nabla }}\cdot \mathbf {B} =0\ ,}$

This equation denies the existence of magnetic monopoles (magnetic charges) and hence also of magnetic currents.

The magnetic field H is not necessarily solenoidal, however, because it satisfies:

${\displaystyle {\boldsymbol {\nabla }}\cdot \mathbf {H} =-{\boldsymbol {\nabla }}\cdot \mathbf {M} \ ,}$

which need not be zero, although it will be zero in some common cases, for example, when B = μH. The H-field also exhibits discontinuity conditions at interfaces between media that may cause it to be non-solenoidal.

Example[edit]

(CC) Image: John R. Brews
B-field lines near a sphere uniformly magnetized in the horizontal direction

To illustrate the roles of B and H a classic example is a sphere with uniform magnetization in an applied external uniform external magnetic flux density B.^[2] The figure shows the lines of the B-field when no external field is present; because B is solenoidal, field lines are closed. Outside the sphere, as shown below, the field is that of a magnetic dipole. To this dipole field, at the end of this example, a uniform external field is added oriented along the magnetization direction.

To begin, the fields introduced by the magnetized sphere alone are found. Because no conduction or displacement currents are present, the magnetic field H satisfies:

${\displaystyle \mathrm {curl} \ \mathbf {H} =0\ ,}$

which allows the introduction of a potential Φ:^[3]

${\displaystyle \mathbf {H} =-\ \mathrm {grad} \ \Phi \ .}$

Taking the divergence, and using the zero divergence of B:

${\displaystyle \nabla ^{2}\Phi =\mathrm {div} \mathbf {M} \ ,}$

which is Poisson's equation. For constant M, div M = 0. However, the solutions inside and outside the sphere must satisfy the boundary conditions on the sphere's surface that the normal component of B is continuous:

${\displaystyle \mathbf {{\hat {u}}_{12}\cdot } \left(\mathbf {B_{1}-B_{2}} \right)=\mathbf {{\hat {u}}_{12}\cdot } \mu _{0}\left(\mathbf {H_{1}+M_{1}-H_{2}-M_{2}} \right)=0\ ,}$

while the normal component of H may be discontinuous if there exist surface "magnetic" charges, σ₁ and σ₂, that is:

${\displaystyle \mathbf {{\hat {u}}_{12}\cdot } \left(\mathbf {H_{1}-H_{2}} \right)=\sigma _{1}+\sigma _{2}\ ,}$

where unit vector û₁₂ points into region 2 from region 1. Taking region 1 inside the sphere where M₁ = M and region 2 outside where M₂=0 and σ₂ = 0,

${\displaystyle \mathbf {{\hat {u}}_{12}\cdot } \mu _{0}\left(\mathbf {H_{1}+M-H_{2}} \right)=0\ ,}$

or:

${\displaystyle \mathbf {{\hat {u}}_{12}\cdot } \left(\mathbf {H_{1}-H_{2}} \right)=-\mathbf {{\hat {u}}_{12}\cdot M} \ =\sigma _{1}.}$

The solution to Poisson's equation with this surface charge is (see Poisson's equation):

${\displaystyle {\begin{aligned}\Phi (\mathbf {r} )&=\iint _{S}{\frac {\sigma _{1}(\mathbf {r'} )}{4\pi |\mathbf {r} -\mathbf {r'} |}}d{S'}\\&=\int _{-\pi }^{\pi }\sin \theta 'd\theta '\int _{0}^{\pi }d\phi '{\frac {M\cos \theta '}{4\pi |\mathbf {r} -\mathbf {r'} |}}\\&={\frac {M}{3}}R^{2}\cos \theta {\frac {r_{<}}{r_{>}^{2}}}\ ,\end{aligned}}}$

with R the radius of the sphere and r_< referring to the minimum of r and R, r_> to the maximum of r and R. The magnetic field is given inside the sphere by the gradient as:

${\displaystyle \mathbf {H} =-{\frac {M}{3}}\mathbf {{\hat {u}}_{z}} \ ,\ \mathbf {B} =\mu _{0}{\frac {2M}{3}}\mathbf {{\hat {u}}_{z}} }$

with û_z a unit vector in the horizontal direction of magnetization. Evidently, the magnetic field H points oppositely to the magnetic flux B inside the sphere. Outside the sphere the field is that of a magnetic dipole:

${\displaystyle \mathbf {H} ={\frac {MR^{3}}{3r^{3}}}\left({\hat {\mathbf {r} }}\ 2\cos \theta +{\hat {\boldsymbol {\theta }}}\sin \theta \right)\ ,\ \mathbf {B} =\mu _{0}\mathbf {H} \ .}$

In particular, along the horizontal z-axis, θ = 0, and the magnetic field outside the sphere along its axis is:

${\displaystyle \mathbf {H} ={\frac {2M}{3}}\mathbf {{\hat {u}}_{z}} \ ,\ \mathbf {B} =\mu _{0}{\frac {2M}{3}}\mathbf {{\hat {u}}_{z}} \ ,}$

showing the continuity of the normal component of B.

If an external magnetic field is imposed, H_a = H_aû_z it can be added to the zero field solution above. Then, inside the sphere the magnetic field H is H_a − M/3. The geometric factor 1/3, which depends upon the shape of the object being a sphere, is called the "demagnetizing factor".

Notes[edit]