A circumsolar ring of asteroidal dust in resonant lock with the Earth

Dermott, S. F.; Jayaraman, S.; Xu, Y. L.; Gustafson, B. Å. S.; Liou, J.‐C.

doi:10.1038/369719a0

Cited by 256 publications

(212 citation statements)

References 23 publications

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“…These resonant structures have been predicted by theoretical studies (Roques et al 1994;Liou & Zook 1999;Ozernoy et al 2000), and observed in few cases around nearby main-sequence stars (e.g., Wilner et al 2002;Greaves et al 2005;Kalas et al 2005;Schneider et al 2009). The most well-studied example of an asymmetric disc is the solar zodiacal cloud, which exhibits several structures interpreted as the dynamical signature of planets (Dermott et al 1985(Dermott et al , 1994Reach et al 1995). This trend suggests that exozodiacal clouds may be full of rings, clumps, and other asymmetries induced by the presence of embedded planets.…”

Section: Impact Of the Exozodiacal Cloud Morphologymentioning

confidence: 99%

Nulling interferometry: impact of exozodiacal clouds on the performance of future life-finding space missions

Defrère¹,

Absil²,

Hartog

et al. 2010

A&A

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Context. Earth-sized planets around nearby stars are being detected for the first time by ground-based radial velocity and space-based transit surveys. This milestone is opening the path toward the definition of instruments able to directly detect the light from these planets, with the identification of bio-signatures as one of the main objectives. In that respect, both the European Space Agency (ESA) and the National Aeronautics and Space Administration (NASA) have identified nulling interferometry as one of the most promising techniques. The ability to study distant planets will however depend on the amount of exozodiacal dust in the habitable zone of the target stars. Aims. We assess the impact of exozodiacal clouds on the performance of an infrared nulling interferometer in the Emma X-array configuration. The first part of the study is dedicated to the effect of the disc brightness on the number of targets that can be surveyed and studied by spectroscopy during the mission lifetime. In the second part, we address the impact of asymmetric structures in the discs such as clumps and offset which can potentially mimic the planetary signal. Methods. We use the DarwinSIM software which was designed and validated to study the performance of space-based nulling interferometers. The software has been adapted to handle images of exozodiacal discs and to compute the corresponding demodulated signal. Results. For the nominal mission architecture with 2-m aperture telescopes, centrally symmetric exozodiacal dust discs about 100 times denser than the solar zodiacal cloud can be tolerated in order to survey at least 150 targets during the mission lifetime. Considering modeled resonant structures created by an Earth-like planet orbiting at 1 AU around a Sun-like star, we show that this tolerable dust density goes down to about 15 times the solar zodiacal density for face-on systems and decreases with the disc inclination. Conclusions. Whereas the disc brightness only affects the integration time, the presence of clumps or offset is more problematic and can hamper the planet detection. Based on the worst-case scenario for debris disc structures, the upper limit on the tolerable exozodiacal dust density is approximately 15 times the density of the solar zodiacal cloud. This gives the typical sensitivity that we will need to reach on exozodiacal discs in order to prepare the scientific programme of future Earth-like planet characterisation missions.

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Section: Impact Of the Exozodiacal Cloud Morphologymentioning

confidence: 99%

Nulling interferometry: impact of exozodiacal clouds on the performance of future life-finding space missions

Defrère¹,

Absil²,

Hartog

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…Radial and azimuthal structure can be induced in circumstellar disks by the gravitational perturbation due to planets or other substellar companions in or in the vicinity of disks (see Dermott et al 1994, Liou & Zook 1999, Wyatt et al 1999, and Ozernoy et al 2000 for gas-free disks, and, e.g., Lubow et al 1999 for gas disks). Detection of such structure is one of the main diagnostic tools in many of the future imaging projects at various wavelengths.…”

Section: Origin Of Structure In Disks : Dust Migration Vsmentioning

confidence: 99%

Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks

Takeuchi

Artymowicz

2001

ApJ

207

239

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We analyze the dynamics of gas-dust coupling in the presence of stellar radiation pressure in circumstellar disks, which are in a transitional stage between the gas-dominated, optically thick, primordial nebulae, and the dust-dominated, optically thin Vega-type disks. Dust grains undergo radial migration, either leaving the disk owing to a strong radiation pressure or seeking a stable equilibrium orbit in corotation with gas. In our models of A-type stars surrounded by a total gas mass from a fraction to dozens of Earth masses, the outward migration speed of dust is comparable with the gas sound speed. Equilibrium orbits are circular, with exception of those signiÐcantly a †ected by radiation pressure, which can be strongly elliptic with apocenters extending beyond the bulk of the gas disk. The migration of dust gives rise to radial fractionation of dust and creates a variety of possible observed disk morphologies, which we compute by considering the equilibrium between the dust production and the dust-dust collisions removing particles from their equilibrium orbits. Large grains (typically km) are distributed Z200 throughout most of the gas disk. Smaller grains (in the range of 10È200 km) concentrate in a prominent ring structure in the outer region of the gas disk (presumably at radius D100 AU), where gas density is rapidly declining with radius. The width and density, as well as density contrast of the dust ring with respect to the inner dust disk, depend on the distribution of gas and the mechanical strength of the particles. Our results open the prospect for deducing the distribution of gas in circumstellar disks by observing their dust. We have qualitatively compared our models with two observed transitional disks around HR 4796A and HD 141569A. Dust migration can result in observation of a ring or a bimodal radial dust distribution, possibly very similar to the ones produced by gap-opening planets embedded in the disk, or shepherding it from inside or outside. We conclude that a convincing planet detection via dust imaging should include speciÐc nonaxisymmetric structure (spiral waves, streamers, resonant arcs) following from the dynamical simulations of perturbed disks.

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“…A circumsolar dust ring close to Earth's orbit was observed by satellites IRAS (Dermott et al 1994) and COBE (Reach et al 1995). The dust particles in this ring can comprise particles moving close to the equilibrium points of the CR3BP with radiation.…”

Section: Equilibrium Points With Velocity Termsmentioning

confidence: 99%

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

Pástor¹

2014

Monthly Notices of the Royal Astronomical Society

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For a body with negligible mass moving in the gravitational field of a star and one planet in a circular orbit (the circular restricted three-body problem) five equilibrium points exist and are known as the Lagrangian points. The positions of the Lagrangian points are not valid for dust particles because in the derivation of the Lagrangian points is assumed that no other forces beside the gravitation act on the body with negligible mass. Here we determined positions of the equilibrium points for the dust particles in the circular restricted three-body problem with radiation. The equilibrium points are located on curves connecting the Lagrangian points in the circular restricted threebody problem. The equilibrium points for Jupiter are distributed in large interval of heliocentric distances due to its large mass. The equilibrium points for the Earth explain a cloud of dust particles trailing the Earth observed with the Spitzer Space Telescope. The dust particles moving in the equilibrium points are distributed in interplanetary space according to their properties.

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A circumsolar ring of asteroidal dust in resonant lock with the Earth

Cited by 256 publications

References 23 publications

Nulling interferometry: impact of exozodiacal clouds on the performance of future life-finding space missions

Nulling interferometry: impact of exozodiacal clouds on the performance of future life-finding space missions

Dust Migration and Morphology in Optically Thin Circumstellar Gas Disks

Positions of equilibrium points for dust particles in the circular restricted three-body problem with radiation

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