A theory of dust comets. I. Model and equations

Finson, Michael L.; Probstein, Ronald F.

doi:10.1086/149762

Cited by 146 publications

(83 citation statements)

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“…Since this comet is known to have undergone a number of explosions (Southworth 1963(Southworth , 1964, such an approximation is clearly unsatisfactory, although it is difficult to es timate the extent of damage done by the forced production law. We notice though that the function f(3) derived by Hiroshi and Liu Cai-pin resem bles that found by Finson and Probstein (1968b) except for a slight shift in the position of the primary maximum toward a larger $.…”

Section: A Monte Carlo Version Of the Finson-probstein Methodssupporting

confidence: 61%

“…The practical applications of the Finson-Probstein method to Comets 1957 III (Finson and Probstein 1968b) and 1970 II (Sekanina and Miller 1973) indicated that in both cases the function f(3) had the following general characteristics:…”

Section: Particle Size Related Distribution Functionmentioning

confidence: 99%

“…At an assumed constant Finson and Probstein (1968b) assumed z = 1. (k)Corrected for particle-evaporation effects but somewhat uncertain.…”

mentioning

confidence: 99%

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Physical Characteristics of Cometary Dust from Dynamical Studies: A Review

Sekanina

1980

Symp. - Int. Astron. Union

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In this review attention is focused on those areas of the dynamical investigation of cometary dust in which significant progress has been achieved since the previous review papers (Sekanina 1976a, 1977). Much of the progress stems from work based on the model of dust comets formulated by Finson and Probstein (1968a). Their introduction of a new technique for dust-tail studies has made it possible for the first time to gain insight into such properties of cometary dust as the size distribution function of particles shortly after emission from the comet nucleus, the distribution of particle ejection velocities, and the production of dust versus time. Since the Finson-Probstein approach is of a combined dynamical/photometric type, information on particle sizes and masses is provided indirectly, through parametric functions determined from the observed distribution of light intensity in the tail. The basic limitation is that particle radius a cannot be separated from particle density ρ, as their product is related to a directly observed quantity β, the acceleration exerted on the particle by solar radiation pressure. Expressed in units of solar attraction, β for a spherical particle is given by where c0 = 0.585 × 10−4 g/cm2 and Qpr is the integrated scattering efficiency of the particle for radiation pressure, which varies significantly with a for particles whose dimensions are smaller than the effective wavelength of solar radiation.

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Section: A Monte Carlo Version Of the Finson-probstein Methodssupporting

confidence: 61%

Section: Particle Size Related Distribution Functionmentioning

confidence: 99%

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Physical Characteristics of Cometary Dust from Dynamical Studies: A Review

Sekanina

1980

Symp. - Int. Astron. Union

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“…We start the dynamical analysis with the zero ejection velocity approximation and calculate the syndynes and synchrones of the dust particles using the equations given by Finson and Probstein (1968a). After being released from the nucleus, particles move in the gravitational field of the Sun (gravitational force F g ) reduced by the force of radiation pressure F r .…”

Section: Syndynes-synchrones Analysismentioning

confidence: 99%

A dynamical model with a new inversion technique applied to observations of Comet C/2000 WM1 (LINEAR)☆

Bonev

Jockers

Karpov

2008

Icarus

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“…2). By observing the extent and morphology of the dust coma and using dust-dynamical models (Finson and Probstein 1968) we can determine the relative velocity distribution, size distribution and production rates of the dust as a function of distance. These models evaluate the motion of a suite of particles after leaving the nucleus under the influence of solar radiation pressure and gravity.…”

Section: Finson-probstein Dust Modelingmentioning

confidence: 99%

The Deep Impact Earth-Based Campaign

et al. 2005

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Prior to the selection of the comet 9P/Tempel 1 as the Deep Impact mission target, the comet was not well-observed. From 1999 through the present there has been an intensive world-wide observing campaign designed to obtain mission critical information about the target nucleus, including the nucleus size, albedo, rotation rate, rotation state, phase function, and the development of the dust and gas coma. The specific observing schemes used to obtain this information and the resources needed are presented here. The Deep Impact mission is unique in that part of the mission observations will rely on an Earth-based (ground and orbital) suite of complementary observations of the comet just prior to impact and in the weeks following. While the impact should result in new cometary activity, the actual physical outcome is uncertain, and the Earth-based observations must allow for a wide range of post-impact phenomena. A world-wide coordinated effort for these observations is described.

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A theory of dust comets. I. Model and equations

Cited by 146 publications

References 0 publications

Physical Characteristics of Cometary Dust from Dynamical Studies: A Review

Physical Characteristics of Cometary Dust from Dynamical Studies: A Review

A dynamical model with a new inversion technique applied to observations of Comet C/2000 WM1 (LINEAR)☆

The Deep Impact Earth-Based Campaign

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