Dynamics of pebbles in the vicinity of a growing planetary embryo: hydro-dynamical simulations

Understanding the growth of the cores of giant planets is a difficult problem. Recently, Lambrechts and Johansen (2012; LJ12) proposed a new model in which the cores grow by the accretion of pebble-size objects, as the latter drift towards the star due to gas drag. Here, we investigate the dynamics of pebble-size objects in the vicinity of planetary embryos of 1 and 5 Earth masses and the resulting accretion rates. We use hydrodynamical simulations, in which the embryo influences the dynamics of the gas and the pebbles suffer gas drag according to the local gas density and velocities. The pebble dynamics in the vicinity of the planetary embryo is non-trivial, and it changes significantly with the pebble size. Nevertheless, the accretion rate of the embryo that we measure is within an order of magnitude of the rate estimated in LJ12 and tends to their value with increasing pebble-size. We conclude that the model by LJ12 has the potential to explain the rapid growth of giant planet cores. The actual accretion rates however, depend on the surface density of pebble size objects in the disk, which is unknown to date.Comment: In press in Astronomy and Astrophysic

On the Destruction of Musical Instruments

In this article, I aim to provide an account of the peculiar reasons that motivate our negative reaction whenever we see musical instruments being mistreated and destroyed. Stephen Davies has suggested that this happens because we seem to treat musical instruments as we treat human beings, at least in some relevant respects. I argue in favour of a different explanation, one that is based on the nature of music as an art form. The main idea behind my account is that musical instruments are not mere tools for the production of art; rather, they are involved in an essential way in artistic appreciation of music. This fact not only grounds our negative reaction to their mistreatment and destruction but also has a normative force that is lacked by the account proposed by Davies

Collisional Cascades in Planetesimal Disks I. Stellar Flybys

We use a new multiannulus planetesimal accretion code to investigate the evolution of a planetesimal disk following a moderately close encounter with a passing star. The calculations include fragmentation, gas and Poynting-Robertson drag, and velocity evolution from dynamical friction and viscous stirring. We assume that the stellar encounter increases planetesimal velocities to the shattering velocity, initiating a collisional cascade in the disk. During the early stages of our calculations, erosive collisions damp particle velocities and produce substantial amounts of dust. For a wide range of initial conditions and input parameters, the time evolution of the dust luminosity follows a simple relation, L_d/L_{\star} = L_0 / [alpha + (t/t_d)^{beta}]. The maximum dust luminosity L_0 and the damping time t_d depend on the disk mass, with L_0 proportional to M_d and t_d proportional to M_d^{-1}. For disks with dust masses of 1% to 100% of the `minimum mass solar nebula' (1--100 earth masses at 30--150 AU), our calculations yield t_d approx 1--10 Myr, alpha approx 1--2, beta = 1, and dust luminosities similar to the range observed in known `debris disk' systems, L_0 approx 10^{-3} to 10^{-5}. Less massive disks produce smaller dust luminosities and damp on longer timescales. Because encounters with field stars are rare, these results imply that moderately close stellar flybys cannot explain collisional cascades in debris disk systems with stellar ages of 100 Myr or longer.Comment: 33 pages of text, 12 figures, and an animation. The paper will appear in the March 2002 issue of the Astronmomical Journal. The animation and a copy of the paper with full resolution figures are at S. Kenyon's planet formation website: http://cfa-www.harvard.edu/~kenyon/p

Spartan Daily, October 27, 1964

Volume 52, Issue 25https://scholarworks.sjsu.edu/spartandaily/4635/thumbnail.jp

Dust in stationary and flowing plasmas

This thesis contains work of a computational and theoretical nature. The floating potential of dust grains immersed in plasma is investigated via particle-in-cell simulation for a range of parameters. In particular, work is focused on the charging of grains large with respect to the electron Debye length. Numerical fits are given for the floating potential of large grains in stationary and flowing plasma. A modified version of the well known orbit-motion-limited (OML) theory is developed for large dust grains. The modified OML theory is shown to be in good agreement with simulation. This modified theory is then adapted for use with flowing plasmas. In the case of flowing plasma, for low ion temperatures and flow speeds upwards of Mach 1, interesting and unexpected effects are seen in the potential and density distribution around dust grains, these are investigated and discussed. Finally, the application of this work is outlined with particular focus on dust grains in a tokamak plasma environment

The fluid mechanics of bubbly drinks

Bubbly drinks are surprisingly attractive. There is something about the nature of the these beverages that make them preferable among other choices. In this article we explore the physics involved in this particular kind of two-phase, mass-transfer-driven flows.Comment: Extended version of Zenit R and Rodr\'iguez-Rodr\'iguez J. The fluid mechanics of bubbly drinks. Physics Today, Vol. 71(11) pp. 44-50, November 201