Dark red debris from three short-period comets: 2P/Encke, 22P/Kopff, and 65P/Gunn

Ishiguro, Masateru; Sarugaku, Yuki; Ueno, Munetaka; Miura, N.; Usui, Fumihiko; Chun, Moo-Young; Kwon, Suk Minn

doi:10.1016/j.icarus.2007.01.003

Cited by 69 publications

(88 citation statements)

References 58 publications

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“…To find the faint dust cloud structure, star-subtracted composite images were produced in a method described in Ishiguro et al (2007) and Ishiguro (2008). We first made images to align the stars to detect faint stars and galaxies.…”

Section: Data Reductionmentioning

confidence: 99%

“…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%

“…It is likely that the dust particles ejected soon after the outburst were responsible for the dust tail. Synchrone-syndyne analysis, however, tends to lead to a misleading value of dust sizes (Ishiguro et al 2007;Fulle 2004). A three-dimensional analysis, which allows nonzero ejection velocities to be considered, is appropriate to estimate the particle sizes and mass-loss rate.…”

Section: Dust Tail Morphologymentioning

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%

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

Ishiguro¹,

Kim²,

Kim³

et al. 2013

ApJ

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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.

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Section: Data Reductionmentioning

confidence: 99%

Section: Radial Profilesmentioning

confidence: 99%

Section: Dust Tail Morphologymentioning

confidence: 99%

Section: Dust Tail Morphologymentioning

confidence: 99%

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

Ishiguro¹,

Kim²,

Kim³

et al. 2013

ApJ

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“…Detailed analysis of single targets, both by ground and space (HST, SPITZER) telescopes, has been performed on comets when at large heliocentric distances, to be sure to observe the bare nucleus (the apparent lack of activity in obtained CCD images has been often -but not always -proven with the comparison of the surface brightness profile of the comet with the Point Spread Function of background stars). Recent papers and surveys on cometary trails (Ishiguro et al 2007;Reach et al 2007) have provided indirect data on distant activity. An analysis of single cometary nuclei has been performed by several authors (see references in Table 1).…”

Section: Observational Data Used To Compile the Inventorymentioning

confidence: 99%

A survey on the distant activity of short period comets

Epifani¹,

Palumbo²,

Colangeli³

2009

A&A

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Aims. The aim of this paper is to build up an inventory of observations of short period comets (SPCs) far from the Sun, and perform an analysis of general properties of the family, investigating the link between distant activity and present and historical orbital parameters. Methods. We gathered all the data available in the literature (as per June 2009) on SPCs ground-based and space observations at heliocentric distance r h > 3 AU. We analyzed the occurrence of distant activity with respect to: position on orbital branch, present orbital parameters (in particular the perihelion distance q), and their recent variations.Results. There is no sharp cut-off at any heliocentric distance, beyond which the cometary activity fades and only bare nuclei are observed. SPCs are more likely to be active post-perihelion than pre-perihelion: among a dataset of 90 comets (for which a heliocentric distance of analysis has been unequivocally established), 59% of the comets observed post-perihelion were detected as active targets, while only 22% of the comets observed pre-perihelion were active. There is a weak trend of comets with increasing perihelion distance to be more likely active at large heliocentric distance: among comets with q < 1.5 AU, only 5 out of 18 comets (28%) have been reported as active at large heliocentric distance, while among those with q > 3 AU, 14 out of 16 comets (88%) have been classified as active. A much less clear trend has been observed for distant cometary activity with semi-major axis a. No apparent appreciable link of a recent (or secular) increase of the perihelion temperature ΔT (due to a rapid decrease in the perihelion distance) with the present degree of distant activity has been observed.

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Meteoroids and Meteors — Observations and Connection to Parent Bodies

Abe¹

2008

Small Bodies in Planetary Systems

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Dark red debris from three short-period comets: 2P/Encke, 22P/Kopff, and 65P/Gunn

Cited by 69 publications

References 58 publications

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

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

A survey on the distant activity of short period comets

Meteoroids and Meteors — Observations and Connection to Parent Bodies

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