The Formation of Encke Meteoroids and Dust Trail

Reach, W. T.; Sykes, M. V.; Lien, D. J.; Davies, John K.

doi:10.1006/icar.2000.6478

Cited by 106 publications

(88 citation statements)

References 38 publications

(56 reference statements)

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“…The existence of a similar circumsolar ring at the orbit of Venus has also been confirmed based on the imaging data of the STEREO mission (Jones et al 2013). In addition to these small-scale structures on scales of a few to a few tens of degrees, finer-scale features associated with the orbits of periodic comets, the so-called cometary dust trails, have also been observed in the IRAS survey data Sykes & Walker 1992;Reach et al 2000).…”

Section: ±2mentioning

confidence: 62%

AKARI far-infrared maps of the zodiacal dust bands

Ootsubo¹,

Doi²,

Takita³

et al. 2016

Publications of the Astronomical Society of Japan

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Zodiacal emission is thermal emission from interplanetary dust. Its contribution to the sky brightness is non-negligible in the region near the ecliptic plane, even in the far-infrared (far-IR) wavelength regime. We analyse zodiacal emission observed by the AKARI far-IR all-sky survey, which covers 97% of the entire sky at arcminute-scale resolution in four photometric bands, with central wavelengths of 65, 90, 140, and 160 µm. AKARI detected small-scale structures in the zodiacal dust cloud, including the asteroidal dust bands and the circumsolar ring, at far-IR wavelengths. Although the smooth component of the zodiacal emission structure in the far-IR sky can be reproduced well by models based on existing far-IR observations, previous zodiacal emission models have discrepancies in the small-scale structures compared with observations. We investigate the geometry of the small-scale dust-band structures in the 1 AKARI far-IR all-sky maps and construct template maps of the asteroidal dust bands and the circumsolar ring components based on the AKARI far-IR maps. In the maps, ±1.• 4, ±2.• 1 and ±10• asteroidal dust-band structures are detected in the 65 µm and 90 µm bands. A possible ±17• band may also have been detected. No evident dust-band structures are identified in either the 140 µm or the 160 µm bands. By subtracting the dust-band templates constructed in this paper, we can achieve a similar level of flux calibration of the AKARI far-IR all-sky maps in the |β| < 40• region to that in the region for |β| > 40• .

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Section: ±2mentioning

confidence: 62%

AKARI far-infrared maps of the zodiacal dust bands

Ootsubo¹,

Doi²,

Takita³

et al. 2016

Publications of the Astronomical Society of Japan

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“…Moreno et al (2008) studied the morphology of the dust cloud in terms of the dynamics of the particles, and found that >600 μm particles, which are much less sensitive to radiation pressure than micrometersized or smaller particles, could be ejected by the outburst. Evidence of such large particles is found to be ubiquitous in in situ observations (McDonnell et al 1986;Tuzzolino et al 2003), by the remote sensing observations of dust tail (Fulle 2004;Moreno 2009;Watanabe et al 1990) and dust trail Ishiguro 2008;Sarugaku et al 2007;Reach et al 2000Reach et al , 2007Kelley et al 2008), sub-millimeter and millimeter observations (Jewitt & Matthews 1997;Altenhoff et al 1999). As a result of these studies, we found that the power index of the size distribution of almost all comets would be in the range of −4 and −3 (Fulle 2004).…”

Section: Mass Erosionmentioning

confidence: 97%

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

Ishiguro¹,

Watanabe²,

Sarugaku³

et al. 2010

ApJ

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Based on optical and infrared observations, we study the albedo and the temperature of the dust grains associated with the spectacular 2007 outburst of Jupiter-family comet 17P/Holmes. We found that the albedo at the solar phase angle ∼16 • was 0.03-0.12. While the color temperature around 3-4 μm was 360 ± 40 K, the color temperature at 12.4 μm and 24.5 μm was ∼200 K, which is consistent with that of a blackbody. We studied the equilibrium temperature of the dust grains at 2.44 AU and found that the big discrepancy in the temperature was caused by the heterogeneity in particle size, that is, hotter components consist of submicron absorbing grains whereas colder components consist of large ( 1 μm) grains. The contemporaneous optical and mid-infrared observations suggest that the albedo and the temperature could decrease within ∼ 3 days after the outburst and stabilized at typical values of the other comets. We estimated the total mass injected into the coma by the outburst on the basis of the derived albedo and the optical magnitude for the entire dust cloud, and found that at least 4 × 10 10 kg (equivalent to a few meter surface layer) was removed by the initial outburst event. The derived mass suggests that the outburst is explainable by neither the exogenetic asteroidal impact nor water ice sublimation driven by solar irradiation, but by an endogenic energy source. We conclude that the outburst was triggered by the energy sources several meters or more below the nuclear surface.

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“…Higher temperature fits to dust coma in excess of black body and sub-solar-point temperatures have been found to be consistent with the dominance of small dust grains in the coma (cf. Lisse et al 1998;Reach et al 2000), owing to super-heating and the presence of silicate emission at ∼10-12 μm. We find a weak W2 signal that is in slight excess of the dust signal that can accommodate CO or CO 2 production rates of 1 × 10 28 and 1 × 10 27 molecule s −1 , respectively (1σ upper limits; Bauer et al 2012a;Pittichová et al 2008).…”

Section: Chiron and The Active Centaursmentioning

confidence: 99%

CENTAURS AND SCATTERED DISK OBJECTS IN THE THERMAL INFRARED: ANALYSIS OFWISE/NEOWISEOBSERVATIONS

Bauer

Grav

Blauvelt

et al. 2013

ApJ

112

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The Wide-field Infrared Survey Explorer (WISE) observed 52 Centaurs and scattered disk objects (SDOs) in the thermal infrared, including 15 new discoveries. We present analyses of these observations to estimate sizes and mean optical albedos. We find mean albedos of 0.08 ± 0.04 for the entire data set. Thermal fits yield average beaming parameters of 0.9 ± 0.2 that are similar for both SDO and Centaur sub-classes. Biased cumulative size distributions yield size-frequency distribution power law indices of ∼−1.7 ± 0.3. The data also reveal a relation between albedo and color at the 3σ level. No significant relation between diameter and albedos is found.

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The Formation of Encke Meteoroids and Dust Trail

Abstract: We observed comet 2P/Encke with the Infrared Space Observatory ISOCAM on

Cited by 106 publications

References 38 publications

AKARI far-infrared maps of the zodiacal dust bands

AKARI far-infrared maps of the zodiacal dust bands

2007 Outburst of 17p/Holmes: The Albedo and the Temperature of the Dust Grains

CENTAURS AND SCATTERED DISK OBJECTS IN THE THERMAL INFRARED: ANALYSIS OFWISE/NEOWISEOBSERVATIONS

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