We study statistical properties of stochastic variations in pulse arrival times, timing noise, in radio pulsars using a new analysis method applied in the time domain. The method proceeds in two steps. First, we subtract low‐frequency wander using a high‐pass filter. Secondly, we calculate the discrete correlation function of the filtered data. As a complementary method for measuring correlations, we introduce a statistic that measures the dispersion of the data with respect to the data translated in time. The analysis methods presented here are robust and of general usefulness for studying arrival time variations over time‐scales approaching the average sampling interval. We apply these methods to timing data for 32 pulsars. In two radio pulsars, PSRs B1133+16 and B1933+16, we find that fluctuations in arrival times are correlated over time‐scales of 10–20 d with the distinct signature of a relaxation process. Though this relaxation response could be magnetospheric in origin, we argue that damping between the neutron star crust and interior liquid is a more likely explanation. Under this interpretation, our results provide the first evidence independent from pulsar spin glitches of differential rotation in neutron stars. PSR B0950+08 shows evidence for quasi‐periodic oscillations that could be related to mode switching.
We investigate a thermoresistive instability in the outer crusts of magnetars wherein a perturbation in temperature increases ohmic heating. We show that magnetars of characteristic age τage∼ 104 yr are unstable over time‐scales as short as days if strong current sheets are present in the outer crust. This instability could play an important role in the thermal and magnetic field evolution of magnetars, and may be related to bursting activity in magnetars.
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Form Approved OMB No. 0704-0188The public reporting burden for this collection of information is estimated to average 1 hour per response, including the time for reviewing instructions, searching existing data sources, gathering and maintaining the data needed, and completing and reviewing the collection of information. Send comments regarding this burden estimate or any other aspect of this collection of information, including suggestions for reducing the burden, We describe a technique to determine the temperature of a Resident Space Object (RSO) from multiple infrared (IR) bands. The characteristic temperature of an object is the temperature of the Planck function that has the closest least squares fit to the observed irradiance in at least three infrared bands. The characteristic temperature and the effective solid angle are free parameters in a formulation that requires simultaneous minimization, across all bands, of chi-square expressions using modeled irradiances and the measured irradiances and their errors. Solutions are determined from a multi-dimensional Levenberg-Marquardt fitting algorithm. The advantage of this approach is that it provides a single, best-fit solution to the RSO modeled as a gray body radiator. In contrast, a 2-band (color) temperature approach using three or more bands produces different solutions for different band combinations with no objective way of determining which solution is best.
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