Contributions in Merlin

We investigate how corporate venture capitalists (CVCs) can rapidly attain central positions in venture capital syndication networks. Using data of CVC investments by U.S. corporations between 1996 and 2005, we complement prior research, which suggests that centrally positioned VCs predominantly invest together with other centrally positioned VCs. While we find clear support for the social network theory arguments that prior central positions in syndication networks significantly explain future network positions of CVCs, we also find a negative interaction effect between past centrality and corporate resources. This finding implies that resources of CVCs can substitute for their lack of prior centrality and allow them to gain rapidly central positions in rigid VC syndication networks.

In this article, we propose a model which interprets the crossed-hand deficit of temporal order judgment (TOJ) from the dynamical systems perspective. The TOJ paradigm is important to understanding how the body image is dynamically sustained in our daily life. Our aim is to show one possible example of how the TOJ deficit could be consistently expressed in the dynamical systems framework. According to the study reported by Yamamoto and Kitazawa, using the genetic algorithm, we reconstruct the crossed-hand effect with a recurrent neural network, and show that it was caused by slow relaxation dynamics near the critical point in our model agent. Moreover, by using the same agent, we demonstrate the occurrence of the deficit in response to three successive stimuli which may help reveal the mechanism of TOJ deficit in the real human case.

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This article presents a conceptual model of entrepreneurial opportunity production from a constructivist perspective. The model assumes that opportunity production proceeds through several stages, including conceptualization of an opportunity idea by an entrepreneur, objectification of that idea, and enactment of the opportunity into a new venture. However, not all opportunity ideas survive this full process. Between the conceptualization stage and the objectification stage, some ideas are abandoned due to inadequate objectification. Also, between the objectification stage and the enactment stage, some objectified opportunities are abandoned due to insufficient resource support. We identify variables that influence the likelihood that opportunity ideas will be objectified and other variables that influence the likelihood that objectified opportunities will be enacted, and these variables are incorporated into empirically testable propositions. In the discussion section, we describe several boundary conditions for our theory, contrast the theory with objectivist (discovery) theory, and derive implications for future research.

We present a gravitational wave (GW) analysis of an extensive series of three-dimensional magnetohydrodynamical core-collapse simulations. Our 25 models are based on a 15 progenitor stemming from (i) stellar evolution calculations; (ii) a spherically symmetric effective general relativistic potential, either the Lattimer-Swesty (with three possible compressibilities) or the Shen equation of state for hot, dense matter; and (iii) a neutrino parametrisation scheme that is accurate until about 5 ms postbounce. For three representative models, we also included long-term neutrino physics by means of a leakage scheme, which is based on partial implementation of the isotropic diffusion source approximation (IDSA). We systematically investigated the effects of the equation of state, the initial rotation rate, and both the toroidal and the poloidal magnetic fields on the GW signature. We stress the importance of including of postbounce neutrino physics, since it quantitatively alters the GW signature. Slowly rotating models, or those that do not rotate at all, show GW emission caused by prompt and proto-neutron star (PNS) convection. Moreover, the signal stemming from prompt convection allows for the distinction between the two different nuclear equations of state indirectly by different properties of the fluid instabilities. For simulations with moderate or even fast rotation rates, we only find the axisymmetric type I wave signature at core bounce. In line with recent results, we could confirm that the maximum GW amplitude scales roughly linearly with the ratio of rotational to gravitational energy at core bounce below a threshold value of about 10%. We point out that models set up with an initial central angular velocity of 2π rad s-1 or faster show nonaxisymmetric narrow-band GW radiation during the postbounce phase. This emission process is caused by a low T/|W| dynamical instability. Apart from these two points, we show that it is generally very difficult to discern the effects of the individual features of the input physics in a GW signal from a rotating core-collapse supernova that can be attributed unambiguously to a specific model. Weak magnetic fields do not notably influence the dynamical evolution of the core and thus the GW emission. However, for strong initial poloidal magnetic fields (≳1012 G), the combined action of flux-freezing and field winding leads to conditions where the ratio of magnetic field pressure to matter pressure reaches about unity which leads to the onset of a jet-like supernova explosion. The collimated bipolar out-stream of matter is then reflected in the emission of a type IV GW signal. In contradiction to axisymmetric simulations, we find evidence that nonaxisymmetric fluid modes can counteract or even suppress jet formation for models with strong initial toroidal magnetic fields. The results of models with continued neutrino emission show that including of the deleptonisation during the postbounce phase is an indispensable issue for the quantitative prediction of GWs from core-collapse supernovae, because it can alter the GW amplitude up to a factor of 10 compared to a pure hydrodynamical treatment. Our collapse simulations indicate that corresponding events in our Galaxy would be detectable either by LIGO, if the source is rotating, or at least by the advanced LIGO detector, if it is not or only slowly rotating.

Using a unique dataset containing separate information on the base and bonus pay of over a million workers, we provide novel evidence on the determinants and earnings effects of performance pay. Several observables—in particular age, education, tenure, and job complexity—have a large impact on both the likelihood and the magnitude of performance pay. Performance pay workers earn a sizable wage premium compared to salary workers, and the earnings premium is larger for men than for women. The wage functions differ markedly between salary and performance pay workers. In particular, the earnings premia associated with age, job complexity, and managerial position are much larger for performance pay workers than for salary workers. The difference in these earnings premia can in part be explained by the fact that heterogeneity among workers increases with age, job complexity, and managerial position. It accounts for about half of the earnings differential between salary and performance pay workers. A separate analysis of the base pay and bonus components of performance pay workers’ earnings reveals that workers who receive higher base pay also get larger bonuses, and that observables predict base pay much better than bonuses.

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