Wicked Problems, Foolish Decisions: Promoting Sustainability through Urban Governance in a Complex World Symposium: Governing Wicked Problems

Why do wicked problems often give birth to bad policy choices? Put another way, why do people—in the face of complex social challenges—make misdiagnoses, ineffective decisions, or no decisions at all? Typical answers point to a plethora of suspects: impatience, myopia, political stalemate, narrow-mindedness, fear and risk aversion, hubris, greed, rational self-interest, ignorance, reliance on emotionally appealing but misleading anecdotal stories, misuse of evidence, and misunderstanding of uncertainty. Amid these divergent explanations, two classes emerge: one lies in the shortcomings and mistakes of the problem solvers, and the other lies in the nature of the problem itself. One stance is to fault the ostensible problem solvers: people are not always rational, fair, patient, thoughtful, or deliberative, but instead are myopic, selfish, greedy, power hungry, or out for revenge (among other motivations). The second stance is to point to the nature of the problem. This is the focus of this Article. In particular, we examine how the dynamics of wicked problems undermine traditional problem-solving efforts. This is not to absolve the problem solvers of responsibility for poor policy choices. It is the responsibility of policymakers to diagnose the distinctive challenges and needs of wicked problems and act accordingly. As urban planning scholars, we focus on entrenched urban problems. This focus is not accidental. Horst Rittel (an architect) and Melvin Webber (a planning theorist and transportation planner) developed the idea of “wicked problems” at the University of California, Berkeley’s College of Environmental Design in the early 1970s—an era when the optimism of solving complex social issues through technical, scientific solutions was colliding hard with the failure of such efforts to conclusively resolve urban poverty, inequality, deindustrialization, racism, white flight, and the violence of the “Urban Crisis.” In this Article, we build on previous research to demonstrate how complexity thinking can engage urban challenges at three levels: (1) describing “complexity” as a symptom of urban systems; (2) analyzing the dynamics of complex urban systems; and ultimately (3) intervening through appropriate planning strategies that account for complexity. We employ this thinking to engage the politics of sustainability at the same three levels, illustrating this at two geographic scales: the neighborhood (specifically, the challenge of ecogentrification) and the megaregion (and the resulting regional externalities and trade-offs). These scales involve actors, conflicts, and specializations within planning. Yet both represent new, hybrid patterns of urbanization that produce intractable problems of environmental unsustainability and social-spatial inequality—two core planning priorities that too often collide. Both situations also generate novel social policy challenges that conventional planning, thinking, and governance tools are ill-equipped to address. These challenges instead call for interdepartmental or intergovernmental cooperation

Orbiting clouds of material at the Keplerian co-rotation radius of rapidly rotating low mass WTTs in Upper Sco

Using K2 data, we have identified 23 very low mass members of the ρ Oph and Upper Scorpius star-forming region as having periodic photometric variability not easily explained by well-established physical mechanisms such as star spots, eclipsing binaries, or pulsation. All of these unusual stars are mid-to-late M dwarfs without evidence of active accretion, and with photometric periods generally <1 day. Often the unusual light curve signature takes the form of narrow flux dips; when we also have rotation periods from star spots, the two periods agree, suggesting that the flux dips are due to material orbiting the star at the Keplerian co-rotation radius. We sometimes see “state-changes” in the phased light curve morphologies where ∼25% of the waveform changes shape on timescales less than a day; often, the “state-change” takes place immediately after a strong flare. For the group of stars with these sudden light curve morphology shifts, we attribute their flux dips as most probably arising from eclipses of warm coronal gas clouds, analagous to the sling-shot prominences postulated to explain transient Hα absorption features in AB Doradus itself and other rapidly rotating late type stars. For another group of stars with somewhat longer periods, we find the short duration flux dips to be highly variable on both short and long timescales, with generally asymmetric flux dip profiles. We believe that these flux dips are due to particulate clouds possibly associated with a close-in planet or resulting from a recent collisional event.PostprintPeer reviewe

Magnetic activity and hot Jupiters of young Suns : the weak-line T Tauri stars V819 Tau and V830 Tau

SGG acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]. SHPA acknowledges financial support from CNPq, CAPES and Fapemig. AAV acknowledges support from the Swiss National Science Foundation (SNSF) via the allocation of an Ambizione Followship. Date of Acceptance: 06/08/2015We report results of a spectropolarimetric and photometric monitoring of the weak-line T Tauri stars (wTTSs) V819 Tau and V830 Tau within the MaTYSSE (Magnetic Topologies of Young Stars and the Survival of close-ingiant Exoplanets) programme, involving the ESPaDOnS spectropolarimeter at the Canada-France-Hawaii Telescope. At ≃3 Myr, both stars dissipated their discs recently and are interesting objects for probing star and planet formation. Profile distortions and Zeeman signatures are detected in the unpolarized and circularly polarized lines, whose rotational modulation we modelled using tomographic imaging, yielding brightness and magnetic maps for both stars. We find that the large-scale magnetic fields of V819 Tau and V830 Tau are mostly poloidal and can be approximated at large radii by 350-400 G dipoles tilted at≃30° to the rotation axis. They are significantly weaker than the field of GQ Lup, an accreting classical T Tauri star (cTTS) with similar mass and age which can be used to compare the magnetic properties of wTTSs and cTTSs. The reconstructed brightness maps of both stars include cool spots and warm plages. Surface differential rotation is small, typically ≃4.4 times smaller than on the Sun, in agreement with previous results on wTTSs. Using our Doppler images to model the activity jitter and filter it out from the radial velocity(RV) curves, we obtain RV residuals with dispersions of 0.033 and 0.104km s-1 for V819 Tau and V830 Tau, respectively. RV residuals suggest that a hot Jupiter may be orbiting V830 Tau, though additional data are needed to confirm this preliminary result. We find no evidence for close-in giant planet around V819 Tau.Publisher PDFPeer reviewe