Widdekind Posted August 8, 2011 Share Posted August 8, 2011 (edited) At a given pressure, inside stars, for a given inward gravity, electrons, being less massive, experience less inward pull, despite their similar thermal energies, and higher velocities. I read in a book, that this means stars shed a few electrons, until their slight positive charge affords electrons a balancing EM attraction. The following equations attempt to mathematically model said effect. First, from the Virial Theorem [math]<U> = -2 <K>[/math], applied separately to the electronic, and ionic, components, of the stellar plasma, w.h.t. [math]-\frac{G M m_e}{R} - \frac{Q e}{4 \pi \epsilon_0 \, R} = -2 \left( \frac{3}{2} k_B T_e \right)[/math] [math]-\frac{G M <A> m_p}{R} + \frac{Q <Z> e}{4 \pi \epsilon_0 \, R} = -2 \left( \frac{3}{2} k_B T_i \right)[/math] Now, assuming thermalization of electrons & ions, s.t. [math]T_e \approx T_i[/math], we can equate these expressions, s.t.: [math]-\frac{G M m_e}{R} - \frac{Q e}{4 \pi \epsilon_0 \, R^2} = -\frac{G M <A> m_p}{R} + \frac{Q <Z> e}{4 \pi \epsilon_0 \, R}[/math] which, after algebraic manipulations, yields (in Coulombs): [math]Q = \left( \frac{4 \pi \epsilon_0}{e} \right) \left( G M m_p \right) \frac{<A>}{<Z>+1} \approx 300 \left( \frac{M}{2 M_{\odot}} \right) \frac{<A>}{<Z>+1}[/math] since NS are [math]\approx 2 M_{\odot}[/math], characteristically (Kirshner. Extravagent Universe, p.36). For a pure H plasma, [math]A = Z = 1[/math], so that the 'plasma fraction' is ~1/2; whereas for a pure (and fully ionized) Fe plasma, characteristic of massive pre-collapse star cores (at [math]T \approx 300 keV[/math]) w.h.t. [math]<A> \approx 2 <Z>[/math], so that the 'plasma fraction' is ~2. Even in such a case, that's only 0.6 m-mol of electrons, out of an entire NS worth of mass. Now, a spinning charged sphere generates a magnetic moment, and dipole-like magnetic field, of characteristic surface-strength [math]B \approx \frac{\mu_0}{4 \pi} \frac{m}{R^3}[/math], where the magnetic moment [math]m \approx \frac{Q}{2 M} L = \frac{1}{5} Q R^2 \omega[/math]. Thus, w.h.t. (in Tesla): [math]B \approx \frac{1}{5} \frac{\mu_0}{4 \pi} \frac{Q \omega}{R} \approx 8 \times 10^{-6} \left( \frac{M}{2 M_{\odot}} \right) \left( \frac{R}{7 km} \right)^{-1} \left( \frac{\omega}{716 Hz} \right)[/math] even using the most rapidly rotating pulsar observed to date. Thus, even a 1ms pulsar, would not be expected, according to these equations, to generate a surface magnetic field, in excess of 0.1G, through this method. Edited August 8, 2011 by Widdekind Link to comment Share on other sites More sharing options...
Recommended Posts
Create an account or sign in to comment
You need to be a member in order to leave a comment
Create an account
Sign up for a new account in our community. It's easy!
Register a new accountSign in
Already have an account? Sign in here.
Sign In Now