The Interplanetary Dust Complex and Comets

Sykes, M. V.; Grün, E.; Reach, W. T.; Jenniskens, Peter

doi:10.2307/j.ctv1v7zdq5.42

Cited by 39 publications

(19 citation statements)

References 92 publications

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“…The predicted dust production mass from events like the one observed for P/2010 A2 is 3-4 orders of magnitude less than the required zodiacal dust production for a steady state, and therefore in agreement with recent work suggesting that comets supply the vast majority of the zodiacal cloud 22,23 . Although beyond the scope of the present letter, we note that the total production of dust from asteroids should be obtained by integrating the contribution from all impactor and parent body sizes; accounting for the more common but smaller impacts that future surveys will find and also rarer and larger impacts.…”

Section: Size Distribution Of Ejectasupporting

confidence: 89%

“…This is in agreement with a single detection by the LINEAR survey; we expect that more small collisions will be detected by nextgeneration surveys. Collisions of this size therefore contribute around 3 x 10 7 kg yr -1 of dust to the zodiacal cloud, which is negligible compared with comets and the total required to maintain a steady state 22 , in agreement with recent models 23 . based on a period of cometary activity (rather than a single event) or smaller particle sizes produce a significantly different pattern of synchrones in panel f (see supplementary Figures 2-4), that do not fit the observations.…”

supporting

confidence: 84%

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A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

Snodgrass

Tubiana

Vincent

et al. 2010

Nature

108

120

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The peculiar object P/2010 A2 was discovered in January 2010 and given a cometary designation because of the presence of a trail of material, although there was no central condensation or coma. The appearance of this object, in an asteroidal orbit (small eccentricity and inclination) in the inner main asteroid belt attracted attention as a potential new member of the recently recognized class of main-belt comets. If confirmed, this new object would expand the range in heliocentric distance over which main-belt comets are found. Here we report observations of P/2010 A2 by the Rosetta spacecraft. We conclude that the trail arose from a single event, rather than a period of cometary activity, in agreement with independent results. The trail is made up of relatively large particles of millimetre to centimetre size that remain close to the parent asteroid. The shape of the trail can be explained by an initial impact ejecting large clumps of debris that disintegrated and dispersed almost immediately. We determine that this was an asteroid collision that occurred around 10 February 2009.

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Section: Size Distribution Of Ejectasupporting

confidence: 89%

supporting

confidence: 84%

A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

Snodgrass

Tubiana

Vincent

et al. 2010

Nature

108

120

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“…4 Rate Estimate population of dust and micrometeoroids in the inner solar system is derived primarily from the collisional processing of asteroids and comets. The particles making up this population vary in mass, size, composition, and orbit and combine to form a dust complex with a complex morphology [17]. The most commonly-used model of the population is the model of Grün, et al [7], which estimates the cumulative flux of micrometeoroids in the inner solar system as a superposition of three distinct populations:…”

Section: Fourier Frequency [ Hz]mentioning

confidence: 99%

Detection and measurement of micrometeoroids with LISA Pathfinder

Thorpe

Parvini

Trigo-Rodríguez

2016

A&A

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The Solar System contains a population of dust and small particles originating from asteroids, comets, and other bodies. These particles have been studied using a number of techniques ranging from in-situ satellite detectors to analysis of lunar microcraters to ground-based observations of zodiacal light. In this paper, we describe an approach for using the LISA Pathfinder (LPF) mission as an instrument to detect and characterize the dynamics of dust particles in the vicinity of Earth-Sun L1. Launched on Dec. 3rd, 2015, LPF is a dedicated technology demonstrator mission that will validate several key technologies for a future space-based gravitational-wave observatory. The primary science instrument aboard LPF is a precision accelerometer which we show will be capable of sensing discrete momentum impulses as small as 4 × 10 −8 N s. We then estimate the rate of such impulses resulting from impacts of micrometeoroids based on standard models of the micrometeoroid environment in the inner solar system. We find that LPF may detect dozens to hundreds of individual events corresponding to impacts of particles with masses >10 −9 g during LPF's roughly six-month science operations phase in a 5 × 10 5 km by 8 × 10 5 km Lissajous orbit around L1. In addition, we estimate the ability of LPF to characterize individual impacts by measuring quantities such as total momentum transferred, direction of impact, and location of impact on the spacecraft. Information on flux and direction provided by LPF may provide insight as to the nature and origin of the individual impact and help constrain models of the interplanetary dust complex in general. Additionally, this direct in situ measurement of micrometeoroid impacts will be valuable to designers of future spacecraft targeting the environment around L1.

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“…The optical depth, τ , was derived by assuming the grains are blackbody emitters with temperature T = 300r −1/2 K, as was measured for trails with multi-band IRAS detections (Sykes et al 2005). Note this temperature is significantly warmer than that obtained by dust (grey, isothermal particles), for which the temperature at 1 AU T 1 < 278 K. As discussed by Sykes et al (2005), trail particles are more consistent with rapidly rotating, randomly oriented, zero-albedo particles maintaining a latitudinal temperature variation across their surfaces. Table 2 lists the resulting τ (median 2 × 10 −9 , range 0.3-16 ×10 −9 ).…”

Section: Measured Debris Trail Propertiesmentioning

confidence: 99%

A survey of debris trails from short-period comets

Reach

Kelley

Sykes

2007

Icarus

124

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We observed 34 comets using the 24 micron camera on the Spitzer Space Telescope. Each image contains the nucleus and covers at least 10^6 km of each comet's orbit. Debris trails due to mm-sized or larger particles were found along the orbits of 27 comets; 4 comets had small-particle dust tails and a viewing geometry that made debris trails impossible to distinguish; and only 3 had no debris trail despite favorable observing conditions. There are now 30 Jupiter-family comets with known debris trails, of which 22 are reported in this paper for the first time. The detection rate is >80%, indicating that debris trails are a generic feature of short-period comets. By comparison to orbital calculations for particles of a range of sizes ejected over 2 yr prior to observation, we find that particles comprising 4 debris trails are typically mm-sized while the remainder of the debris trails require particles larger than this. The lower-limit masses of the debris trails are typically 10^11 g, and the median mass loss rate is 2 kg/s. The mass-loss rate in trail particles is comparable to that inferred from OH production rates and larger than that inferred from visible-light scattering in comae.Comment: accepted by Icarus; figures compressed for astro-p

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The Interplanetary Dust Complex and Comets

Cited by 39 publications

References 92 publications

A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

A collision in 2009 as the origin of the debris trail of asteroid P/2010 A2

Detection and measurement of micrometeoroids with LISA Pathfinder

A survey of debris trails from short-period comets

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