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Revival of the magnetar PSR J1622-4950: observations with MeerKAT, Parkes, XMM-Newton, Swift, Chandra, and NuSTAR

New radio (MeerKAT and Parkes) and X-ray (XMM-Newton, Swift, Chandra, and NuSTAR) observations of PSR J1622-4950 indicate that the magnetar, in a quiescent state since at least early 2015, reactivated between 2017 March 19 and April 5. The radio flux density, while variable, is approximately 100x larger than during its dormant state. The X-ray flux one month after reactivation was at least 800x larger than during quiescence, and has been decaying exponentially on a 111+/-19 day timescale. This high-flux state, together with a radio-derived rotational ephemeris, enabled for the first time the detection of X-ray pulsations for this magnetar. At 5%, the 0.3-6 keV pulsed fraction is comparable to the smallest observed for magnetars. The overall pulsar geometry inferred from polarized radio emission appears to be broadly consistent with that determined 6-8 years earlier. However, rotating vector model fits suggest that we are now seeing radio emission from a different location in the magnetosphere than previously. This indicates a novel way in which radio emission from magnetars can differ from that of ordinary pulsars. The torque on the neutron star is varying rapidly and unsteadily, as is common for magnetars following outburst, having changed by a factor of 7 within six months of reactivation.Comment: Published in ApJ (2018 April 5); 13 pages, 4 figure

A multiconfigurational approach to the electronic structure of electro-generated species of the Re2(μ- Ph2PCH2PPh2)(S2CNEt2)4 complex

The nature of Re-Re bonding in Re2(µ-Ph2PCH2PPh2)(S2CNEt2)4 complex, including its neutral (10) and two oxidized (1+ and 12+) species, was explored utilizing state-of-the-art quantum chemical methodologies within density functional theory (DFT) and complete active space self-consistent field (CASSCF). Our results show that the ground state electron configuration of the 10 is σ^2 π^4 δ^2 δ^(*2) with an effective bond order (EBO) of 2.73 computed with CASSCF. The oxidation discloses an electron removal from a metal-based orbital, giving 1+ and 12+ with an EBO of 2.71 and 2.64, respectively. The relative similarity in EBO values among neutral and oxidized species suggests that the oxidation processes have almost no effect on the Re-Re bond strength even though electrons removal from metal-based orbitals because the electrons that occupied the δ components of Re-Re bonds in 1+ and 12+ localized on the two Re ions, thus, they were excluded from EBO estimation

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