scholarly journals Micromechanical Resonator Driven by Radiation Pressure Force

2017 ◽  
Vol 7 (1) ◽  
Author(s):  
Joseph A. Boales ◽  
Farrukh Mateen ◽  
Pritiraj Mohanty
Keyword(s):  
Radiation Pressure ◽  
Pressure Force ◽  
Radiation Pressure Force

scholarly journals Laser-induced vibration of a thin soap film

Lab on a Chip ◽  
2014 ◽  
Vol 14 (18) ◽  
pp. 3525-3529 ◽  
Author(s):  
Olivier Emile ◽  
Janine Emile
Keyword(s):  
Radiation Pressure ◽  
Optical Radiation ◽  
Soap Film ◽  
Pressure Force ◽  
Radiation Pressure Force

We report on the vibration of a thin soap film based on the optical radiation pressure force.

scholarly journals Observations of X-Ray Radiation Pressure Force Using High-Speed Diffracted X-Ray Tracking

2011 ◽  
Vol 100 (3) ◽  
pp. 312a
Author(s):  
Yuji C. Sasaki ◽  
Yasuhito Suzuki ◽  
Hiroshi Sekiguchi ◽  
Noboru Ohta ◽  
Tatsuhito Mastuo ◽  
...  
Keyword(s):  
Radiation Pressure ◽  
High Speed ◽  
Pressure Force ◽  
X Ray ◽  
Radiation Pressure Force

scholarly journals Long Dust Trails of Short Period Comets

1991 ◽  
Vol 126 ◽  
pp. 229-234
Author(s):  
H.U. Keller ◽  
K. Richter
Keyword(s):  
Radiation Pressure ◽  
Dust Cloud ◽  
Dust Particles ◽  
Pressure Force ◽  
Meteor Streams ◽  
Short Period ◽  
Orbital Periods ◽  
Comet Halley ◽  
Observational Techniques ◽  
Radiation Pressure Force

Comets constitute an important source for the zodiacal dust cloud. Mainly large particles are contributed because the smaller particles are emitted into hyperbolic orbits relative to the sun. Radiation pressure force reduces the effective solar gravitational attraction. Information about large cometary particles can be derived from a variety of sources requiring quite different observational techniques. Many distinct meteor streams are connected to orbits of short period comets. These streams contain large dust particles that are very little influenced by radiation pressure force. In some cases such as the η Aquarids and Orionids connected to comet Halley the total mass and the age of the meteors have been derived (Hughes, 1987; Hajduk, 1987). The mass of the streams is 5 to 10 times larger than the present mass of the nucleus and their lifetime corresponds to 2000 to 3000 orbital periods. Visible meteors are typically 10−2g and more of centimetre size.

Radiation pressure force acting on cometary aggregates

2007 ◽  
Vol 40 (2) ◽  
pp. 266-271 ◽  
Author(s):  
M. Köhler ◽  
T. Minato ◽  
H. Kimura ◽  
I. Mann
Keyword(s):  
Radiation Pressure ◽  
Pressure Force ◽  
Radiation Pressure Force

scholarly journals Dust trajectory simulations around the Sun, Vega, and Fomalhaut

2019 ◽  
Vol 626 ◽  
pp. A107 ◽  
Author(s):  
Johann Stamm ◽  
Andrzej Czechowski ◽  
Ingrid Mann ◽  
Carsten Baumann ◽  
Margaretha Myrvang
Keyword(s):  
Magnetic Field ◽  
Radiation Pressure ◽  
Gravitational Force ◽  
Charged Particles ◽  
Charged Dust ◽  
The Sun ◽  
Pressure Force ◽  
Electromagnetic Forces ◽  
Model Calculations ◽  
Radiation Pressure Force

Context. Vega and Fomalhaut display a thermal emission brightness that could possibly arise from hot dust near the stars, an inner extension of their planetary debris disks. An idea has been suggested that nanometer-sized dust particles are kept in the vicinity of the stars by electromagnetic forces. This resembles the trapping that model calculations show in the corotating magnetic field in the inner heliosphere within approximately 0.2 AU from the Sun. Aims. The aim of this work is to study whether the trapping of dust due to electromagnetic forces acting on charged dust near the Sun can occur around Vega and Fomalhaut and what are the conditions for trapping. Methods. We studied the dust trajectories with numerical calculations of the full equation of motion, as well as by using the guiding center approximation. We assumed a constant dust charge and a Parker-type magnetic field, which we estimated for the two stars. Results. We find no bound trajectories of charged particles around Vega or Fomalhaut as long as the radiation pressure force exceeds the gravitational force, that is, for particles smaller than 1 μm. A trapping zone could exist inside of 0.02 AU for Vega and 0.025 AU for Fomalhaut, but only for those particles with radiation pressure force smaller than gravitational force. In comparison to the Sun, the trapping conditions would occur closer to the stars because their faster rotation leads to a more closely wound-up magnetic field spiral. We also show that plasma corotation can be consistent with trapping. Our model calculations show that the charged particles are accelerated to stellar wind velocity very quickly, pass 1 AU after approximately three days, and are further ejected outward where they pass the debris disks at high velocity. We find this for particles with a surface charge-to-mass ratio larger than 10−6 elementary charges per proton mass for both negatively and positively charged dust and independent of the strength of the radiation pressure force. Based on charging assumptions, this would correspond to dust of sizes 100 nm and smaller.

scholarly journals Prediction of radiation pressure force exerted on moving particles by the two-level skeletonization

2014 ◽  
Vol 22 (8) ◽  
pp. 10032 ◽  
Author(s):  
Xiao-Min Pan ◽  
Ming-Jiang Gou ◽  
Xin-Qing Sheng
Keyword(s):  
Radiation Pressure ◽  
Pressure Force ◽  
Radiation Pressure Force
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