RXTE Observations of LMC X-1 and LMC X-3

Of all known persistent stellar-mass black hole candidates, only LMC X-1 and LMC X-3 consistently show spectra that are dominated by a soft, thermal component. We present results from long (170ksec) Rossi X-ray Timing Explorer (RXTE) observations of LMC X-1 and LMC X-3 made in 1996 December. The spectra can be described by a multicolor disk blackbody plus an additional high-energy power-law. Even though the spectra are very soft (Gamma is about 2.5), RXTE detected a significant signal from LMC X-3 up to energies of 50keV, the hardest energy at which the object was ever detected. Focusing on LMC X-3, we present results from the first year of an ongoing monitoring campaign with RXTE which started in 1997 January. We show that the appearance of the object changes considerably over its ~200d long cycle. This variability can either be explained by periodic changes in the mass transfer rate or by a precessing accretion disk analogous to Her X-1.Comment: 4 pages, 5 figures, also available at http://aitzu3.ait.physik.uni-tuebingen.de/publications/preprints1998.html to be published in "Highlights of X-Ray Astronomy, a symposium in honour of Joachim Truemper" (B. Aschenbach et al., eds.), MPE Repor

Spectral variations of the X-ray binary pulsar LMC X-4 during its long period intensity variation and a comparison with Her X-1

We present spectral variations of the binary X-ray pulsar LMC X-4 using the RXTE/PCA observations at different phases of its 30.5 day long super-orbital period. Only out of eclipse data were used for this study. During the high state of the super-orbital period of LMC X-4, the spectrum is well described by a high energy cut-off power-law with a photon index in the range of 0.7-1.0 and an iron emission line. In the low state, the spectrum is found to be flatter with power-law photon index in the range 0.5-0.7. A direct correlation is detected between the continuum flux in 7-25 keV energy band and the iron emission line flux. The equivalent width of the iron emission line is found to be highly variable during low intensity state, whereas it remains almost constant during the high intensity state of the super-orbital period. It is observed that the spectral variations in LMC X-4 are similar to those of Her X-1 (using RXTE/PCA data). These results suggest that the geometry of the region where the iron line is produced and its visibility with respect to the phase of the super-orbital period is similar in LMC X-4 and Her X-1. A remarkable difference between these two systems is a highly variable absorption column density with phase of the super-orbital period that is observed in Her X-1 but not in LMC X-4.Comment: 7 pages, 5 figures, Accepted for publication in Astronomy and Astrophysic

Timing and spectral studies of LMC X-4 in high and low states with Beppo-SAX: Detection of pulsations in the soft spectral component

We report here detailed timing and spectral analysis of two Beppo-SAX observations of the binary X-ray pulsar LMC X-4 carried out during the low and high states of its 30.5 days long super-orbital period. Timing analysis clearly shows 13.5 s X-ray pulsations in the high state of the super-orbital period which allows us to measure the mid-eclipse time during this observation. Combining this with two other mid-eclipse times derived earlier with the ASCA, we derived a new estimate of the orbital period derivative. Pulse-phase averaged spectroscopy in the high and low states shows that the energy spectrum in the 0.1 - 10 keV band comprises of a hard power-law, a soft excess, and a strong iron emission line. The continuum flux is found to decrease by a factor of ~ 60 in the low state while the decrease in the iron line flux is only by a factor of ~ 12, suggesting a different site for the production of the line emission. In the low state, we have not found any significant increase in the absorption column density. The X-ray emission is found to come from a very large region, comparable to the size of the companion star. Pulse phase resolved spectroscopy in the high state shows a pulsating nature of the soft spectral component with some phase offset compared to the hard X-rays, as is known in some other binary X-ray pulsars.Comment: 13 pages, 10 figures, Accepted for publication in The Astrophysical Journa

Discovery of Recurring Soft to Hard State Transitions in LMC X-3

We present the analysis of an RXTE monitoring campaign of the canonical soft state black hole candidates LMC X-1 and LMC X-3. In contrast to LMC X-1, which does not exhibit any periodic spectral changes, we find that LMC X-3 exhibits stron spectral variability on time scales of days to weeks. For typical RXTE ASM count rates, the luminosity variations of LMC X-3 are due to changes of the phenomenological disk blackbody temperature. During episodes of especially low luminosity (ASM count rates < 0.6 counts/sec), kT strongly decreases and the power law significantly hardens to a photon index of ~1.8. These changes are consistent with state changes of LMC X-3 from the soft state to the canonical hard state of galactic black hole candidates. We argue that the long term variability of LMC X-3 might be due to a wind-driven limit cycle such as discussed by Shields et al. (1986)Comment: MNRAS, in press, added discussion on LMC X-1 correlations, cosmetic updates to table

A Transition to the Soft State in GRS 1758-258

Near the end of 2001 February, the black-hole candidate (BHC) GRS 1758-258 made an abrupt transition from a standard hard (low) state to a soft state. Unlike Cyg X-1 and other BHCs, whose luminosity increases during this transition, GRS 1758-258 was dimmer after the transition. We present observations with the Proportional Counter Array on the Rossi X-ray Timing Explorer and interpret the phenomenon in the context of a ``dynamical'' soft state model. Using this model we predicted that mass transfer from the companion had ceased, and that the luminosity should decay on a timescale of a few weeks. The most recent data support this prediction, being consistent with a decay time of 34 dy. The current state is consistent with the ``off'' state of GRS 1758-258 reported by GRANAT/Sigma in 1991-1992.Comment: 13 pages, 5 figures, accepted for publication in The Astrophysical Journal Letters Accepted version has only minor changes, plus extra data showing more of the deca

Switching Distributions for Perpendicular Spin-Torque Devices within the Macrospin Approximation

We model "soft" error rates for writing (WSER) and for reading (RSER) for perpendicular spin-torque memory devices by solving the Fokker-Planck equation for the probability distribution of the angle that the free layer magnetization makes with the normal to the plane of the film. We obtain: (1) an exact, closed form, analytical expression for the zero-temperature switching time as a function of initial angle; (2) an approximate analytical expression for the exponential decay of the WSER as a function of the time the current is applied; (3) comparison of the approximate analytical expression for the WSER to numerical solutions of the Fokker-Planck equation; (4) an approximate analytical expression for the linear increase in RSER with current applied for reading; (5) comparison of the approximate analytical formula for the RSER to the numerical solution of the Fokker-Planck equation; and (6) confirmation of the accuracy of the Fokker-Planck solutions by comparison with results of direct simulation using the single-macrospin Landau-Lifshitz-Gilbert (LLG) equations with a random fluctuating field in the short-time regime for which the latter is practical