Photophoresis of a spherical particle in a rarefied gas

Beresnev, S. A.; Chernyak, V. G.; Fomyagin, G. A.

doi:10.1063/1.858540

Cited by 81 publications

(72 citation statements)

References 22 publications

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“…Photophoresis is a potentially powerful effect acting on particles in a gas that are exposed to radiation (Rohatschek 1985;Beresnev et al 1993). It is a force acting on a particle which is illuminated and absorbs light.…”

Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

“…A rigorous treatment of photophoresis on spherical particles of radius a for all gas pressures, i.e., in the free molecular flow regime and the continuum regime, has been given by Beresnev et al (1993). Assuming the accommodation coefficients (how gas molecules on the surface of a particle adapt to energy and momentum) to be 1 and a complete absorption of the light at the illuminated side of the particle, the photophoretic force is given as (Beresnev et al 1993) (1) where I is the light flux, m g is the average mass of the gas molecules (3.914 × 10 −27 kg), T is the gas temperature, k the Boltzmann constant, and ψ 1 and ψ 2 are functions of the Knudsen number (Equation 3).…”

Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

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Outward transport of CAIs during FU‐Orionis events

Wurm¹,

Haack

2009

Meteorit & Planetary Scien

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available online at http://meteoritics.org Abstract-Evidence from meteorites shows that the first solids to form in the solar system, calciumaluminum-rich inclusions (CAIs), were transported outward from the Sun by several AU in the early solar system. We introduce a new concept of levitation and outward transport of CAIs at the surface of protoplanetary disks. Thermal radiation from the disk and the Sun can cause particles to levitate above the disk and drift outward through a process known as photophoresis. During normal conditions this process only works for dust-sized particles but during high luminosity events like FU-Orionis Outward transport of CAIs during FU-Orionis events

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Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

Outward transport of CAIs during FU‐Orionis events

Wurm¹,

Haack

2009

Meteorit & Planetary Scien

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“…From this a net momentum on the particle results. A detailed theory for thermophoresis and photophoresis exist for spherical particles [6][7][8][9]. Many parameters within this theory are not easily accessible for calculations, i.e.…”

Section: Introductionmentioning

confidence: 99%

Ice particles trapped by temperature gradients at mbar pressure

Kelling

Wurm

Dürmann

2011

Review of Scientific Instruments

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In laboratory experiments we observe that ice particles (≤ 100 µm) entrained in a low pressure atmosphere (∼ 1 mbar) get trapped by temperature gradients between three reservoirs at different tempertature. Confining elements are a peltier element at 250 K (bottom), a liquid nitrogen reservoir at 77 K (top) and the surrounding vacuum chamber at 293 K. Particle levitation and trapping is modeled by an interplay of thermophoresis, photophoresis and gravity. A number of ice particles are trapped simultaneously in close spatial distance to each other at least up to minutes and are accessible for further experiments.

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“…In the contrary case, the gas flow is in the continuum regime. In these conditions, the photophoretic force F ph on a spherical particle, valid for both flow regimes, can be expressed as follows (Beresnev et al 1993):…”

Section: The Photophoretic Forcementioning

confidence: 99%

“…(9), one obtains the mean free path. We note in passing that Beresnev et al (1993) used a normalising factor of 1/2 in Eq. (9) instead of the 1/3 that applies for three-dimensional gases, and this may slightly modify the numerical constants in Eq.…”

Section: Balistic Transportmentioning

confidence: 99%

Photophoretic transport of hot minerals in the solar nebula

Moudens¹,

Mousis²,

Petit³

et al. 2011

A&A

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Context. Hot temperature minerals have been detected in a large number of comets and were also identified in the samples of Comet Wild 2 that were returned by the Stardust mission. Meanwhile, observations of the distribution of hot minerals in young stellar systems suggest that these materials were produced in the inner part of the primordial nebula and have been transported outward in the formation zone of comets. Aims. We investigate the possibility that photophoresis provides a viable mechanism to transport high-temperature materials from the inner solar system to the regions in which the comets were forming. Methods. We use a grid of time-dependent disk models of the solar nebula to quantify the distance range at which hot minerals can be transported from the inner part of the disk toward its outer regions as a function of their size (10 −5 to 10 −1 m) and density (500 and 1000 kg m −3 ). These models will also yield information on the disk properties (radius of the inner gap, initial mass, and lifetime of the disk). The particles considered here are in the form of aggregates that presumably were assembled from hot mineral individual grains ranging down to submicron sizes and formed by condensation within the hottest portion of the solar nebula. Our particle-transport model includes the photophoresis, radiation pressure, and gas drag. Results. Depending on the postulated disk parameters and the density of particles, 10 −2 to 10 −1 m aggregates can reach heliocentric distances up to ∼35 AU in the primordial nebula over very short timescales (no more than a few hundred thousand years). 10 −3 m particles follow the same trajectory as the larger ones but their maximum migration distance does not exceed ∼26 AU and is reached at later epochs in the disks. On the other hand, 10 −5 to 10 −4 m aggregates are continuously pushed outward during the evolution of the solar nebula. Depending on the adopted disk parameters, these particles can reach the outer edge of the nebula well before its dissipation. Conclusions. Our simulations suggest that irrespective of the employed solar nebula model, photophoresis is a mechanism that can explain the presence of hot temperature minerals in the formation region of comets. Comets probably had the time to trap the dust transported from the inner solar system either in their interior during accretion or in the form of shells surrounding their surface if they ended their growth before the particles reached their formation location.

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Photophoresis of a spherical particle in a rarefied gas

Cited by 81 publications

References 22 publications

Outward transport of CAIs during FU‐Orionis events

Outward transport of CAIs during FU‐Orionis events

Ice particles trapped by temperature gradients at mbar pressure

Photophoretic transport of hot minerals in the solar nebula

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