Detection of a Long-Extended Dust Trail Associated with Short-Period Comet 4P/Faye in 2006 Return

Sarugaku, Yuki; Ishiguro, Masateru; Pyo, Jeonghyun; Miura, N.; Nakada, Y.; Usui, Fumihiko; Ueno, Munetaka

doi:10.1093/pasj/59.4.l25

Cited by 12 publications

(10 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

Self Cite

View full text Add to dashboard Cite

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.

show abstract

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

Self Cite

View full text Add to dashboard Cite

show abstract

“…Although there are many factors to determine the expansion dust speed, it can be approximated by a simple power-law function of the size and the heliocentric distance, that is, v ej = K/ √ r h a d , where a d denotes the radius of dust particles in micron. K is a constant, typically in the range of 100 < K < 1000 m s −1 based on theoretical studies (Whipple 1951;Ip & Mendis 1974), past observations of normal comet activities (Lisse et al 1998;Ishiguro et al 2007;Sarugaku et al 2007;Snodgrass et al 2008;Ishiguro 2008), and cometary outbursts including the 17P/Holmes event in 2007 (Sekanina 2008;Montalto et al 2008;Moreno et al 2008;Hsieh et al 2010;Sarugaku et al 2010;Reach et al 2010;Stevenson & Jewitt 2012). From the equation for the expanding speed, dust particles could escape from a region of 1 ′′ aperture in 1.4-22 hours for a d = 1 µm and 6-94 days for a d = 1 cm particles.…”

Section: Radial Profilesmentioning

confidence: 99%

“…A three-dimensional analysis, which allows nonzero ejection velocities to be considered, is appropriate to estimate the particle sizes and mass-loss rate. Here we applied a three-dimensional analysis to match the observed images, following the model in Ishiguro et al (2007), Sarugaku et al (2007), Ishiguro (2008), and Hanayama et al (2012).…”

Section: Dust Tail Morphologymentioning

confidence: 99%

Comet 17p/Holmes: Contrast in Activity Between Before and After the 2007 Outburst

Ishiguro¹,

Kim²,

Kim³

et al. 2013

ApJ

Self Cite

View full text Add to dashboard Cite

A Jupiter-family comet, 17P/Holmes, underwent outbursts in 1892 and 2007. In particular, the 2007 outburst is known as the greatest outburst over the past century. However, little is known about the activity before the outburst because it was unpredicted. In addition, the time evolution of the nuclear physical status has not been systematically studied. Here we study the activity of 17P/Holmes before and after the 2007 outburst through optical and mid-infrared observations. We found that the nucleus highly depleted its near-surface icy component before but became activated after the -3 -2007 outburst. Assuming a conventional 1-µm-sized grain model, we derived a surface fractional active area of 0.58% ± 0.14% before the outburst whereas it was enlarged by a factor of ∼50 after the 2007 outburst. We also found that large (≥1 mm) particles could be dominant in the dust tail observed around aphelion. Based on the size of the particles, the dust production rate was 170 kg s −1 at the heliocentric distance r h = 4.1 AU, suggesting that the nucleus still held active status around the aphelion passage. The nucleus color was similar to that of the dust particles and average for a Jupiter-family comet but different from most Kuiper Belt objects, implying that the color may be inherent to icy bodies in the solar system. On the basis of these results, we concluded that more than 76 m surface materials were blown off by the 2007 outburst.

show abstract

“…The sky background was contaminated by elongated stars and galaxies because the observations were carried out in comet-tracking mode. We removed these stellar objects using the masking algorism developed for the data reduction of cometary dust trails (Sarugaku et al 2007;Ishiguro et al 2007;Ishiguro 2008), outlined as follows. We first made images to align the stars, because this is an effective way of detecting faint stars and galaxies.…”

Section: Data Reductionmentioning

confidence: 99%

“…No obvious dust trail was found in the Subaru optical image, even though it was clear in the Spitzer infrared image. In this study, we re-analyzed the Subaru/Suprime-Cam images using the masking method developed for the detection of faint cometary dust clouds (Ishiguro et al 2007;Sarugaku et al 2007;Ishiguro 2008) and constructed a comet image without contaminants (e.g., stars and galaxies). This technique enabled us to detect mini-comets brighter that 26.5 mag and diffuse light sources associated with the comet brighter than 30.0 mag arcsec -2 .…”

mentioning

confidence: 99%

2006 Fragmentation of Comet 73P/Schwassmann-Wachmann 3B observed with Subaru/Suprime-Cam

Ishiguro¹,

Usui²,

Sarugaku³

et al. 2009

Icarus

Self Cite

View full text Add to dashboard Cite

a b s t r a c tThe fragmentation of the split Comet 73P/Schwassmann-Wachmann 3 B was observed with the primefocus camera Suprime-Cam attached to the Subaru 8.2-m telescope. The fragmentation revealed dozens of miniature comets [Fuse, T., Yamamoto, N., Kinoshita, D., Furusawa, H., Watanabe, J., 2007. Publ. Astron. Soc. Jpn. 59 (2), 381-386]. We analyzed the Subaru/Suprime-Cam images, detecting no fewer than 154 mini-comets, mostly extending to the southwest. Three were close to the projected orbit of fragment B. We applied synchrone-syndyne analysis, modified for rocket effect analysis, to the mini-fragment spatial distribution. We found that most of these mini-comets were ejected from fragment B by an outburst occurring around 1 April 2006, and three fragments on the leading side of nucleus B could have been released sunward on the previous return. Several fragments might have been released by successive outbursts around 24 April and 2 May 2006. The ratio of the rocket force to solar gravity was 7-23 times larger than that exerted on fragment B. No significant color variation was found. The mean color index, V-R = 0.50 ± 0.07, was slightly redder than that of the Sun and similar to that of the largest fragment, C, which suggests that these mini-fragments were detected mainly through sunlight reflected by dust particles and materials on the nuclei. We examined the surface brightness profiles of all detected fragments and estimated the sizes of 154 fragments. We found that the radius of these mini-fragments was in the 5-to 108-m range (equivalent size of Tunguska impactor). The power-law index of the differential size distribution was q = À3.34 ± 0.05. Based on this size distribution, we found that about 1-10% of the mass of fragment B was lost in the April 2006 outbursts. Modeling the cometary fragment dynamics [Desvoivres, E.] revealed that it is likely that mini-fragments smaller than $10-20 m could be depleted in water ice and become inactive, implying that decameter-sized comet fragments could survive against melting and remain as near-Earth objects. We attempted to detect the dust trail, which was clearly found in infrared wavelengths by Spitzer. No brightness enhancement brighter than 30.0 mag arcsec À2 (3r) was detected in the orbit of fragment B.

show abstract

Detection of a Long-Extended Dust Trail Associated with Short-Period Comet 4P/Faye in 2006 Return

Cited by 12 publications

References 7 publications

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

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

Comet 17p/Holmes: Contrast in Activity Between Before and After the 2007 Outburst

2006 Fragmentation of Comet 73P/Schwassmann-Wachmann 3B observed with Subaru/Suprime-Cam

Contact Info

Product

Resources

About