Radiation Pressure and the Poynting–Robertson Effect for Fluffy Dust Particles

Kimura, Hiroshi; Okamoto, Hajime; Mukai, T.

doi:10.1006/icar.2002.6849

Cited by 59 publications

(77 citation statements)

References 58 publications

(65 reference statements)

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“…At dust sizes, we did not take into account P-R drag, its role is discussed in Section 6.8. In calculating the radiation pressure force acting on dust grains, we assumed them to be compact and spherical, thus ignoring possible non-radial effects (e.g., Kimura et al 2002). Like mechanical properties, optical properties of dust may vary from one grain to another, resulting in different response to radiation pressure, different temperatures, and different thermal fluxes even for like-sized particles (Krivov et al 2006).…”

Section: Limitations Of the Modelmentioning

confidence: 99%

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Müller

Löhne

Krivov

2009

ApJ

102

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The archetypical debris disk around Vega has been observed intensively over the past 25 years. It has been argued that the resulting photometric data and images may be in contradiction with a standard, steady-state collisional scenario of the disk evolution. In particular, the emission in the mid-infrared (mid-IR) appears to be in excess of what is expected from a "Kuiper belt" at ∼100 AU, which is evident in the submillimeter images and inferred from the majority of photometric points. Here we re-address the question of whether or not the Vega disk observations are compatible with a continuous dust production through a collisional cascade. Instead of seeking a size and spatial distribution of dust that provide the best fit to observations, our approach involves physical modeling of the debris disk "from the sources." We assume that dust is maintained by a belt of parent planetesimals, and employ our collisional and radiative transfer codes to consistently model the size and radial distribution of the disk material and then thermal emission of dust. In doing so, we vary a broad set of parameters, including the stellar properties, the exact location, extension, and dynamical excitation of the planetesimal belt, chemical composition of solids, and the collisional prescription. We are able to reproduce the spectral energy distribution in the entire wavelength range from the near-IR to millimeter, as well as the mid-IR and submillimeter radial brightness profiles of the Vega disk. Thus, our results suggest that the Vega disk observations are not in contradiction with a steady-state collisional dust production, and we put important constraints on the disk parameters and physical processes that sustain it. The total disk mass in 100 km-sized bodies is estimated to be ∼10 Earth masses. Provided that collisional cascade has been operating over much of the Vega age of ∼350 Myr, the disk must have lost a few Earth masses of solids during that time. We also demonstrate that using an intermediate luminosity of the star between the pole and the equator, as derived from its fast rotation, is required to reproduce the debris disk observations. Finally, we show that including cratering collisions into the model is mandatory.

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Section: Limitations Of the Modelmentioning

confidence: 99%

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Müller

Löhne

Krivov

2009

ApJ

102

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“…Papers by Klačka and Kocifaj (1994), Kocifaj et al (2000) and Kimura et al (2002) are based on the paper by Klačka (1994a), which hypothesized that quantities corresponding to components of space vector Q ′ ≡ (Q ′ 1 , Q ′ 2 , Q ′ 3 ) behave as scalars under Lorentz transformation. Our derivation proves correctness of the hypothesis.…”

Section: Equation Of Motionmentioning

confidence: 99%

“…Klačka (2000a) presented relativistically covariant form of equation of motion. Later on, Kimura et al (2002) became aware that relativistic form of equation of motion is required to be sure that the offered equation of motion is correct. Thus, the authors presented relativistic derivation of the equation of motion, also.…”

Section: Introductionmentioning

confidence: 99%

Electromagnetic Radiation and Motion of a Particle

Klačka

2004

Celestial Mechanics and Dynamical Astronomy

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Abstract. We consider the motion of uncharged dust grains of arbitrary shape including the effects of electromagnetic radiation and thermal emission. The resulting relativistically covariant equation of motion is expressed in terms of standard optical parameters.Explicit expressions for secular changes of osculating orbital elements are derived in detail for the special case of the Poynting-Robertson effect. Two subcases are considered: (i) central acceleration due to gravity and the radial component of radiation pressure independent of the particle velocity, (ii) central acceleration given by gravity and the radiation force as the disturbing force. The latter case yields results which may be compared with secular orbital evolution in terms of orbital elements for an arbitrarily shaped dust particle. The effects of solar wind are also presented.

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“…Furthermore, it is shown that the values of β for a fluffy aggregate computed based on Mie theory and Maxwell-Garnett effective medium theory well agree with those derived by the DDA. Kimura et al (2002) have extended the analysis for the dynamical effect of solar radiation on the fluffy dust grains based on the DDA method. Although many trials to study the dynamics of nonspherical grains in the interplanetary space have been done previously as mentioned above, no quantitative examinations of the coupling between the heliocentric Kepler motion and the rotation of the grain have appeared.…”

Section: The Equation Of Motionmentioning

confidence: 99%

“…A discovery of the asteroid dust bands by the Infrared Astronomical Satellite (IRAS) associated with the Koronis and Themis families (Low et al, 1984) has proved that the collisional debris from the asteroids becomes scattered through the interplanetary space. Further satellite observations by the Diffuse Infrared Background Experiment (DIRBE) instrument on the Cosmic Background Explorer (COBE) (Spiesman et al, 1995), as well as the ground-based observations in the visible (Ishiguro et al, 1998), have confirmed the presence of the dust bands.…”

Section: Introductionmentioning

confidence: 99%

Orbital variation of the rotating non-spherical dust grains due to change of the solar radiation forces by shape effect

Saklayen

Mukai

2014

Earth Planet Sp

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We present the values of a ratio β of the solar radiation pressure force to the solar gravity on the finite circular cylindrical grains, as functions of an aspect ratio of the cylinder and an incident angle of the solar radiation. By using the resulting formula of β( ), the trajectory of the Kepler orbit for the rotating silicate cylinder is computed associated with a spin motion under the assumption that the spin axis is along the shortest axis of the cylinder and points to the direction perpendicular to the solar radiation. We found for the silicate cylinder grain with a mass equivalent to a sphere with a radius of 0.15 μm, and the aspect ratio of 2.0 that a heliocentric distance of the grain varies periodically with a time, having an amplitude of the fluctuation in the heliocentric distance of about 0.02 AU, where the spin velocity is 0.25 rotation/day and the initial orbit has a semi-major axis 3.0 AU and an eccentricity 0. In addition, during such a fluctuation of the heliocentric distance, the instantaneous eccentricity of the orbit also varies simultaneously from 0 to 1.6 with the rotation of the grain. This implies that the in-situ measurements of orbital elements of impact grains on the dust detector may record those instantaneous orbital elements related to the phase of the grain's rotation.

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Radiation Pressure and the Poynting–Robertson Effect for Fluffy Dust Particles

Cited by 59 publications

References 58 publications

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Electromagnetic Radiation and Motion of a Particle

Orbital variation of the rotating non-spherical dust grains due to change of the solar radiation forces by shape effect

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