Abstract: We derive an exact expression for the radiation pressure of a quasimonochromatic plane wave incident from the free space onto the flat surface of a semi-infinite dielectric medium. In order to account for the total optical momentum (incident plus reflected) that is transferred to the dielectric, the mechanical momentum acquired by the medium must be added to the rate of flow of the el...

The effective recombination coefficient, αeff , is refined for optically thin cases. Radiation pressure in Lyman-α and HeII Lyman-α is calculated in terms of the number density and the mean free path. Pressure equilibrium between Lyman-α clouds and an adiabatically expanding inter-galactic medium is assumed, niTi = ncTc. Numerical models of isothermal and adiabatic expanding Lyman-α forest clou...

We analyze two nonlinear optofluidic processes where nonlinearity is induced by the interplay between optical field and liquid interface. Specifically, guided optical waves generate radiation pressure on the liquid interface, which can in turn distort the liquid interface and modify the properties of the optical field. In the first example, we discuss the feasibility of nonlinear optofluidic so...

I consider the physics of gravitational instabilities in the presence of dynamically important radiation pressure and gray radiative diffusion, governed by a constant opacity κ. For any non-zero radiation diffusion rate on an optically-thick scale k−1, the medium is unstable unless the classical gas-only isothermal Jeans criterion is satisfied. If the radiation acoustic sound crossing timescale...

We consider the structure of marginally Toomre-stable starburst disks under the assumption that radiation pressure on dust grains provides the dominant vertical support against gravity. This assumption is particularly appropriate when the disk is optically thick to its own infrared radiation, as in the central regions of Ultraluminous Infrared Galaxies (ULIRGs). We argue that because the disk r...

We show that the radiation pressure of an intense optical field impinging on a perfectly reflecting vibrating mirror is able to entangle in a robust way the first two optical sideband modes. Under appropriate conditions, the generated entangled state is of EPR type [A. Einstein, et al., Phys. Rev. 47, 777 (1935)]. PACS numbers: 42.50.Vk, 03.65.Ud, 03.67.-a

It is shown that radiation pressure can be profitably used to entangle macroscopic oscillators like movable mirrors, using present technology. We prove a new sufficient criterion for entanglement and show that the achievable entanglement is robust against thermal noise. Its signature can be revealed using common optomechanical readout apparatus.

The ratioβ of the radiation pressure force to the gravitational attraction is calculated for circumstellar grains. Eleven stars of various spectral type are considered and their spectral flux compiled from available data sometimes supplemented by appropriate models. The materials composing the grains are a silicate (obsidian), organic materials (ice tholin, poly-HCN), graphite and glassy carbon...

Stars with masses of ∼ 20 M⊙ have short Kelvin times that enable them to reach the main sequence while still accreting from their natal clouds. The resulting nuclear burning produces a huge luminosity and a correspondingly large radiation pressure force on dust grains in the accreting gas. This effect may limit the upper mass of stars that can form by accretion. Indeed, simulations and analytic...

Can entanglement and the quantum behavior in physical systems survive at arbitrary high temperatures? In this Letter we show that this is the case for a electromagnetic field mode in an optical cavity with a movable mirror in a thermal state. We also identify two different dynamical regimes of generation of entanglement separated by a critical coupling strength.