Last Train to Oxford (Someone Called Derrida)

Last Train to Oxford - a thought thriller. A dramatised adaptation of John Schad’s documentary novel by Fred Dalmasso & John Schad Someone called Jacques Derrida, the philosopher, someone called him on the phone, someone who was dead. A mystery, he thought, a mystery that begins in 1968 when Derrida visits Oxford and there he dies, several times. Murder, he thought. So too thought my father, an Oxonian, in his final nightmare years. And so we investigate, not just the Oxford of the 1960s but the Oxford of the 1930s and a public school in the middle of the Second World War. In the end, the question is: 'Can one die of another's death? Or can one live?

Quo vadis, paradox? Centripetal and centrifugal forces in theory development

Organizations increasingly face contradictory goals, multiple stakeholder expectations, and pluralistic missions that surface and intensify competing demands. Paradox theory offers a lens to understand and engage these tensions. Yet as research adopting a paradox lens continues to grow, scholars warn that its success could advance a dominant logic, which will ultimately hinder conceptual development and result in its downfall. We suggest that scholars can avoid this denigration by embracing theory development’s driving forces—centripetal forces that define and buffer a conceptual core and centrifugal forces aimed at challenging the core and extending its boundaries. Although these forces’ directions diverge, we depict these dual forces as paradoxical—contradictory and fundamentally interdependent. That is, we explore paradoxical forces of theory development to understand the development of paradox theory. We offer means to use, balance, and leverage these insights to help surface the black boxes in paradox research

Probing the Solar Atmosphere Using Oscillations of Infrared CO Spectral Lines

Oscillations were observed across the whole solar disk using the Doppler shift and line depth of spectral lines from the CO molecule near 4666~nm with the National Solar Observatory's McMath/Pierce solar telescope. Power, coherence, and phase spectra were examined, and diagnostic diagrams reveal power ridges at the solar global mode frequencies to show that these oscillations are solar p-modes. The phase was used to determine the height of formation of the CO lines by comparison with the IR continuum intensity phase shifts as measured in Kopp et al., 1992; we find the CO line formation height varies from 425 < z < 560 km as we move from disk center towards the solar limb 1.0 > mu > 0.5. The velocity power spectra show that while the sum of the background and p-mode power increases with height in the solar atmosphere as seen in previous work, the power in the p-modes only (background subtracted) decreases with height, consistent with evanescent waves. The CO line depth weakens in regions of stronger magnetic fields, as does the p-mode oscillation power. Across most of the solar surface the phase shift is larger than the expected value of 90 degrees for an adiabatic atmosphere. We fit the phase spectra at different disk positions with a simple atmospheric model to determine that the acoustic cutoff frequency is about 4.5 mHz with only small variations, but that the thermal relaxation frequency drops significantly from 2.7 to 0 mHz at these heights in the solar atmosphere