The Effects of University Patenting and Licensing on Downstream R&D Investment and Social Welfare

A central argument behind the Bayh-Dole Act presumed that firms had no incentives to invest in downstream R&D aimed at developing university inventions committed to the public domain. The empirical evidence on university patenting and licensing is partly at odds with the premises of this argument. Non-exclusive licensing of university patents has been common and lucrative, and in the area of biomedical technologies university patents and licensing restrictions may be a hindrance to downstream R&D, rather than a stimulus. The paper presents a model of R&D competition based on a university invention where appropriability conditions are defined by the patentability of downstream innovations and imitation opportunities. A comparison of equilibria under “open access” to university inventions and under “university patenting” shows that only under restrictive conditions the latter regime results in increased R&D investment and social welfare. In general, university licensing royalties are therefore a poor gauge of social welfare gains from university patenting. Copyright Springer Science+Business Media, LLC 2006university patents, R&D competition, Bayh-Dole Act, downstream innovation, O310, O340,

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta