On the Flux of Extrasolar Dust in Earth’s Atmosphere

Murray, Norman; Weingartner, Joseph C.; Capobianco, Christopher C.

doi:10.1086/380117

Cited by 63 publications

(46 citation statements)

References 66 publications

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“…10, top panels). This trend is clearly seen in the left panel of Figure 11; the slope of the line corresponds to approximately and is consistent with an analytical calculation by Murray et al (2004).…”

Section: Dependence On Planetary Architecture and Particle Sizesupporting

confidence: 88%

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

Moro‐Martín¹,

Malhotra²

2005

ApJ

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Main-sequence stars are commonly surrounded by debris disks, formed by cold far-IR-emitting dust that is thought to be continuously replenished by a reservoir of undetected dust-producing planetesimals. We have investigated the orbital evolution of dust particles in debris disks harboring massive planets. Small dust grains are blown out by radiation pressure, as is well known; in addition, gravitational scattering by the giant planets also creates an outflow of large grains. We describe the characteristics of this large-particle outflow in different planetary architectures and for different particle sizes. In addition, the ejection of particles is responsible for the clearing of dust inside the orbit of the planet. We study the efficiency of particle ejection and the resulting dust density contrast inside and outside the orbit of the planet as a function of the planet's mass and orbital elements and the particle size. We discuss its implications for exoplanetary debris disks and for the interpretation of in situ dust detection experiments on space probes traveling in the outer solar system. Subject headingg s: circumstellar matter -interplanetary medium -Kuiper Belt -methods: n-body simulationsplanetary systems -planetary systems: protoplanetary disks

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Section: Dependence On Planetary Architecture and Particle Sizesupporting

confidence: 88%

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

Moro‐Martín¹,

Malhotra²

2005

ApJ

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“…If we calculate the gyroradius for our fiducial grain values, we get ). (Murray et al 2004) Given the sizes of the solar system (∼100 au) and the magnetosphere (∼1000 Å R ; "⊕" refers toEarth), we would expect some deflection by the IMF, though not a complete disruption since the IMF weakens by several orders of magnitude beyond 1 au, whereas the magnetosphere should cause very little deflection of the dust grains. The numerical results below confirm this expectation, as summarized in Table 2.…”

Section: Magnetic Deflectionmentioning

confidence: 99%

RADIOACTIVE IRON RAIN: TRANSPORTING⁶⁰Fe IN SUPERNOVA DUST TO THE OCEAN FLOOR

Fry

Fields

Ellis

2016

ApJ

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Several searches have found evidence of Fe 60 deposition, presumably from a near-Earth supernova (SN), with concentrations that vary in different locations on Earth. This paper examines various influences on the path of interstellar dust carrying Fe 60 from an SN through the heliosphere, with the aim of estimating the final global distribution on the ocean floor. We study the influences of magnetic fields, angle of arrival, wind, and ocean cycling of SN material on the concentrations at different locations. We find that the passage of SN material through the mesosphere/lower thermosphere has the greatest influence on the final global distribution, with ocean cycling causing lesser alteration as the SN material sinks to the ocean floor. SN distance estimates in previous works that assumed a uniform distribution are a good approximation. Including the effects on surface distributions, we estimate a distance of -+ 46 610 pc for an -SN progenitor. This is consistent with an SN occurring within the Tuc-Hor stellar group ∼2.8 Myr ago, with SN material arriving on Earth ∼2.2 Myr ago. We note that the SN dust retains directional information to within 1• through its arrival in the inner solar system, so that SN debris deposition on inert bodies such as the Moon will be anisotropic, and thus could in principle be used to infer directional information. In particular, we predict that existing lunar samples should show measurable Fe 60 differences.

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“…A recent study of meteoroid ejection velocities from pre-main sequence stellar systems taking into account radiation pressure, Poynting-Robertson and gravitational forces suggests that in some cases small meteoroids may be produced with velocities of the order of at least several hundred km s −1 (Quirt & Hawkes 2005). Recently Murray et al (2004) have considered production mechanisms from AGB stars, young stellar objects such as T Tauri stars, and debris disks around Vega-like stars. They have also considered the survival in interstellar space of such material.…”

Section: Introductionmentioning

confidence: 99%

“…Baggaley & Neslusan (2002) have examined how a stream of particles from a single interstellar source would encounter the Earth in terms of observed velocity distributions. Murray et al (2004), however, have recently suggested that it is unlikely that radar detectable interstellar meteors are produced by β-Pictoris. Issues of the subsequent destruction of these interstellar meteoroids (see e.g.…”

Section: Introductionmentioning

confidence: 99%

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High geocentric velocity meteor ablation

Hill¹,

Rogers²,

Hawkes³

2005

A&A

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Interstellar origin meteoroids have now been detected using radar, image intensified video, large aperture radar and space dust impact techniques. Dynamical and radiation production mechanisms will eject some meteoroids from other planetary systems into orbits which will impact Earth with high geocentric velocities. In this paper we numerically model the ablation of high geocentric velocity (71 to 500 km s −1 ) meteors in order to predict the heights, light curves and trail lengths to be expected. We modeled three compositions and structures: asteroidal, cometary and porous cometary. Meteoroid masses ranging from 10 −6 to 10 −13 kg were used in the model. As expected, these high geocentric velocity meteors, when compared to other meteors, ablate higher in the atmosphere. For example a 300 km s −1 cometary structure meteor of mass 10 −9 kg will have a peak luminosity at about 190 km. They will also have significantly longer trail lengths. The same 300 km s −1 , 10 −9 kg cometary meteor would be within 2 mag of its peak brightness for a vertical displacement of 60 km if incident at a zenith angle of 45• . The peak light intensity of these high geocentric velocity meteors changes only slowly with velocity. Although the incident kinetic energy per unit time increases dramatically, this is largely offset by a decrease in the optical luminous efficiency in this velocity regime according to our luminous efficiency model. The 300 km s −1 , 10 −9 kg cometary meteor would have an absolute meteor magnitude at peak luminosity of about +8.5 mag. Our results suggest that at least those high geocentric velocity meteors larger than about 10 −8 kg should be observable with current meteor electro-optical technology although there may be observational biases against their detection. The results of this paper can be used to help optimize a search strategy for these very high geocentric velocity meteors.

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On the Flux of Extrasolar Dust in Earth’s Atmosphere

Cited by 63 publications

References 66 publications

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

RADIOACTIVE IRON RAIN: TRANSPORTING⁶⁰Fe IN SUPERNOVA DUST TO THE OCEAN FLOOR

High geocentric velocity meteor ablation

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On the Flux of Extrasolar Dust in Earth’s Atmosphere

Cited by 63 publications

References 66 publications

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

Dust Outflows and Inner Gaps Generated by Massive Planets in Debris Disks

RADIOACTIVE IRON RAIN: TRANSPORTING60Fe IN SUPERNOVA DUST TO THE OCEAN FLOOR

High geocentric velocity meteor ablation

Contact Info

Product

Resources

About

RADIOACTIVE IRON RAIN: TRANSPORTING⁶⁰Fe IN SUPERNOVA DUST TO THE OCEAN FLOOR