Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8108fig1.eps}\end{figure}$ Figure 1: Braking index as a function of characteristic spindown time. We plot here $\pm \log\vert n\vert$ ( $\pm$ according to whether n>0 or n<0) vs. $\log\tau$ , where $\tau\equiv -\Omega/2\dot{\Omega}$ in years. Note that |n|>1 everywhere. At large $\tau >10^5$ , the diagram may be fit by the simple linear relation $\pm \log\vert n\vert\sim \pm (\log\tau-3)$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8108fig2.eps}\end{figure}$ Figure 2: $P-\dot{P}$ diagram for the $\sim$ 400 pulsars with measured braking index values shown in Figure 1. Here, P, $\dot{P}$ are the pulsar period and period derivative respectively. The distribution is that of a standard sparse $P-\dot{P}$ diagram without any obvious observational bias.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{8108fig3.eps}\end{figure}$ Figure 3: Fit of the distribution shown in Fig. 1 assuming a 100% cyclic evolution of the pulsar spindown torque (Eqs. (4) and (5)). $\tau_{\rm cycle}\sim 10~000$ (in years). The fit is acceptable, even for young pulsars ( $\tau \leq 10^5$ ) where some of the dispersion in the measurements of n is due to neutron star glitches.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8108fig4.eps}\end{figure}$ Figure 4: On the left, we plot the magnetic field structure in the case of no magnetospheric reconnection (CKF). Distances are normalized to the light cylinder distance $r_{\rm L}$ . On the right, we plot the corresponding electric current distribution $I=I(\Psi )$ along the field lines that cross the light cylinder. The magnetic flux is normalized to the canonical value $\Psi _o\equiv \pi B_* r^3/r_{\rm L}$ . The electric current is normalized to the canonical value $I_o\equiv \Omega \Psi _o/(4\pi )$ . For comparison, we plot also (dashed line) the electric current distribution of a relativistic magnetic split monopole with the same amount of magnetic flux crossing the light cylinder (Michel 1991).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8108fig5.eps}\end{figure}$ Figure 5: Same as Fig. 4 with some amount of equatorial magnetospheric reconnection that corresponds to $\epsilon = 0.4$ (Eq. (10)).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8108fig6.eps}\end{figure}$ Figure 6: Same as Fig. 4 with maximum equatorial magnetospheric reconnection that corresponds to $\epsilon = 1$ .
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{8108fig7.eps}\end{figure}$ Figure 7: The spindown torque parameter f (Eq. (1)) as a function of the dissipation parameter $\epsilon$ . In the absence of reconnection ( $\epsilon = 0$ ), f=0.6 (CKF).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8108fig1.eps}\end{figure}$	Figure 1: Braking index as a function of characteristic spindown time. We plot here $\pm \log\vert n\vert$ ( $\pm$ according to whether n>0 or n<0) vs. $\log\tau$ , where $\tau\equiv -\Omega/2\dot{\Omega}$ in years. Note that \|n\|>1 everywhere. At large $\tau >10^5$ , the diagram may be fit by the simple linear relation $\pm \log\vert n\vert\sim \pm (\log\tau-3)$ .
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8108fig2.eps}\end{figure}$	Figure 2: $P-\dot{P}$ diagram for the $\sim$ 400 pulsars with measured braking index values shown in Figure 1. Here, P, $\dot{P}$ are the pulsar period and period derivative respectively. The distribution is that of a standard sparse $P-\dot{P}$ diagram without any obvious observational bias.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{8108fig3.eps}\end{figure}$	Figure 3: Fit of the distribution shown in Fig. 1 assuming a 100% cyclic evolution of the pulsar spindown torque (Eqs. (4) and (5)). $\tau_{\rm cycle}\sim 10~000$ (in years). The fit is acceptable, even for young pulsars ( $\tau \leq 10^5$ ) where some of the dispersion in the measurements of n is due to neutron star glitches.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8108fig5.eps}\end{figure}$	Figure 5: Same as Fig. 4 with some amount of equatorial magnetospheric reconnection that corresponds to $\epsilon = 0.4$ (Eq. (10)).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8108fig6.eps}\end{figure}$	Figure 6: Same as Fig. 4 with maximum equatorial magnetospheric reconnection that corresponds to $\epsilon = 1$ .
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$\begin{figure} \par\includegraphics[width=6cm,clip]{8108fig7.eps}\end{figure}$	Figure 7: The spindown torque parameter f (Eq. (1)) as a function of the dissipation parameter $\epsilon$ . In the absence of reconnection ( $\epsilon = 0$ ), f=0.6 (CKF).
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