Thermal radiation from dust grains in Edgeworth-Kuiper Belt

Yamamoto, Sakae; Mukai, T.

doi:10.1186/bf03352145

Cited by 9 publications

(5 citation statements)

References 17 publications

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“…This result confirms earlier conclusion (see, e.g. Yamamoto & Mukai 1998;Krivov et al 2008) that the blackbody assumption is probably too crude and should not be used in modeling the thermal emission of debris disks.…”

Section: Calculated Fluxsupporting

confidence: 81%

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The Edgeworth-Kuiper debris disk

Vitense¹,

Krivov²,

Löhne³

2010

A&A

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The Edgeworth-Kuiper belt (EKB) and its presumed dusty debris is a natural reference for extrsolar debris disks. We re-analyze the current database of known transneptunian objects (TNOs) and employ a new algorithm to eliminate the inclination and the distance selection effects in the known TNO populations to derive expected parameters of the "true" EKB. Its estimated mass is M EKB = 0.12 M ⊕ , which is by a factor of ∼15 larger than the mass of the EKB objects detected so far. About a half of the total EKB mass is in classical and resonant objects and another half is in scattered ones. Treating the debiased populations of EKB objects as dust parent bodies, we then "generate" their dust disk with our collisional code. Apart from accurate handling of destructive and cratering collisions and direct radiation pressure, we include the Poynting-Robertson (P-R) drag. The latter is known to be unimportant for debris disks around other stars detected so far, but cannot be ignored for the EKB dust disk because of its much lower optical depth. We find the radial profile of the normal optical depth to peak at the inner edge of the classical belt, ≈40 AU. Outside the classical EKB, it approximately follows τ ∝ r −2 which is roughly intermediate between the slope predicted analytically for collision-dominated (r −1.5 ) and transport-dominated (r −2.5 ) disks. The size distribution of dust is less affected by the P-R effect. The cross section-dominating grain size still lies just above the blowout size (∼1 . . . 2 µm), as it would if the P-R effect was ignored. However, if the EKB were by one order of magnitude less massive, its dust disk would have distinctly different properties. The optical depth profile would fall off as τ ∝ r −3 , and the cross section-dominating grain size would shift from ∼1 . . . 2 µm to ∼100 µm. These properties are seen if dust is assumed to be generated only by known TNOs without applying the debiasing algorithm. An upper limit of the in-plane optical depth of the EKB dust set by our model is τ = 2 × 10 −5 outside 30 AU. If the solar system were observed from outside, the thermal emission flux from the EKB dust would be about two orders of magnitude lower than for solar-type stars with the brightest known infrared excesses observed from the same distance. Herschel and other new-generation facilities should reveal extrasolar debris disks nearly as tenuous as the EKB disk. We estimate that the Herschel/PACS instrument should be able to detect disks at a ∼1 . . . 2M EKB level.

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Section: Calculated Fluxsupporting

confidence: 81%

“…The latter is defined as a mixture consisting of a water ice matrix (with constants from Warren 1984) contaminated with 10% volume fraction of astronomical silicate (Laor & Draine 1993). This is similar to what, for instance, Yamamoto & Mukai (1998) adopted in their calculation of thermal emission of the EKB dust.…”

Section: Parameters and Materialsmentioning

confidence: 67%

The Edgeworth-Kuiper debris disk

Vitense¹,

Krivov²,

Löhne³

2010

A&A

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“…The figure shows the dominant process for dust around the sun and Eridani whose mass loss rate is given by Wood et al (2002Wood et al ( , 2005. The total mass of dust in the Kuiper belt is estimated by Backman et al (1995) and by Yamamoto & Mukai (1998), who include production of dust particles by interstellar dust impacts on Kuiper belt objects. When the sun was young at its t = 0.7 Gyr age, both the mass loss rate and the total dust mass were higher than the current values as expected from the mass loss history of solar-like stars (Ṁ ∝ t −2.33 ) given by Wood et al (2005) and the collisional evolution (Ṁ d ∝ t −1 ) or PR drag evolution (Ṁ d ∝ t −2 ) of dust given by Dominik & Decin (2003).…”

Section: Discussionmentioning

confidence: 99%

Momentum transfer to fluffy dust aggregates from stellar winds

Minato

Koehler

Kimura

et al. 2006

A&A

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Aims. Dust-plasma interaction may play a dominant role in the dynamics of dust particles around young main-sequence stars. Circumstellar dust is expected to be an aggregate consisting of small grains. The momentum transfer cross section (MTCS) for an aggregate is a key quantity for determining the lifetimes of circumstellar dust disks. Methods. We formulate the MTCS of fluffy dust aggregates and propose an algorithm for computing the MTCS. We compare the magnitude of the plasma and photon Poynting-Roberson effects (PR effects). Results. We find an empirical formula that approximates numerical results well for the MTCSs. A comparison of the magnitudes of the PR effects shows that the lifetime of debris dust around young main-sequence stars is shorter by orders of magnitude than the lifetime estimated by considering the photon PR effect alone. Brief discussion is given on the plasma PR effect for dust debris disks around young main-sequence stars.

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“…Fulle 1992;Sekanina 1996;Kelley et al 2013;Epifani et al 2016). Dust production from Edgeworth-Kuiper Belt objects has also been long hypothesized, with mutual collisions (Stern 1995(Stern , 1996, bombardment by interstellar dust grains (Yamamoto and Mukai 1998), and bombardment by interplanetary dust grains (Poppe 2015) all theorized as possible production mechanisms. The relative balance between these hypothesized production mechanisms at EKBs is currently unclear and it is possible that all three contribute substantially.…”

Section: Outer Interplanetary Dust and Meteoroid Cloudmentioning

confidence: 99%

Interplanetary Dust, Meteoroids, Meteors and Meteorites

et al. 2019

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Interplanetary dust particles and meteoroids mostly originate from comets and asteroids. Understanding their distribution in the Solar system, their dynamical behavior and their properties, sheds light on the current state and the dynamical behavior of the Solar system. Dust particles can endanger Earth-orbiting satellites and deep-space probes, and a good understanding of the spatial density and velocity distribution of dust and meteoroids in the Solar system is important for designing proper spacecraft shielding. The study of inter-Cosmic Dust from the Laboratory to the Stars Edited by

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Thermal radiation from dust grains in Edgeworth-Kuiper Belt

Cited by 9 publications

References 17 publications

The Edgeworth-Kuiper debris disk

The Edgeworth-Kuiper debris disk

Momentum transfer to fluffy dust aggregates from stellar winds

Interplanetary Dust, Meteoroids, Meteors and Meteorites

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