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

Ishiguro, Masateru; Kim, Yoonyoung; Kim, Junhan; Usui, Fumihiko; Vaubaillon, Jérémie; Ishihara, Daisuke; Hanayama, H.; Sarugaku, Yuki; Hasegawa, Susumu; Kasuga, Toshihiro; Warjurkar, Dhanraj S.; Ham, Ji Beom; Pyo, Jeonghyun; Kuroda, D.; Ootsubo, Takafumi; Sakamoto, Makoto; Narusawa, Shin Ya; Takahashi, Jun; Akisawa, Hiroki; Watanabe, Jun

doi:10.1088/0004-637x/778/1/19

Cited by 12 publications

(16 citation statements)

References 62 publications

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“…For example, the analysis of size and age of the particles in the dust trail of main belt object P/2012 F5 (Gibbs) in Stevenson et al (2012) was confirmed by Moreno et al (2012). The analysis of short-period comet 17P/Holmes in Stevenson et al (2014) is consistent with results obtained by several other groups including Reach et al (2010) and Ishiguro et al (2013). The analysis of the dust trail of 67P/Churyumov-Gerasimenko in Bauer et al (2012) is consistent with the large particles that have been found by the Rosetta mission (Rotundi et al 2015), providing further "ground truth" to our modeling techniques.…”

Section: Effect Of Initial Particle Velocity and Justification For Tsupporting

confidence: 88%

The Perihelion Emission of Comet C/2010 L5 (WISE)

Kramer

Bauer

Fernández

et al. 2017

ApJ

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The only Halley-type comet discovered by the Wide-Field Infrared Survey Explorer (WISE), C/2010 L5 (WISE), was imaged three times by WISE, and it showed a significant dust tail during the second and third visits (2010 June and July, respectively). We present here an analysis of the data collected by WISE, putting estimates on the comet's size, dust production rate, gas production (CO+CO 2 ) rate, and active fraction. We also present a detailed description of a novel tail-fitting technique that allows the commonly used syndyne-synchrone models to be used analytically, thereby giving more robust results. We find that C/2010 L5ʼs dust tail was likely formed by strong emission, likely in the form of an outburst, occurring when the comet was within a few days of perihelion. Analyses of the June and July data independently agree on this result. The two separate epochs of dust tail analysis independently suggest a strong emission event close to perihelion. The average size of the dust particles in the dust tail increased between the epochs, suggesting that the dust was primarily released in a short period of time, and the smaller dust particles were quickly swept away by solar radiation pressure, leaving the larger particles behind. The difference in CO 2 and dust production rates measured in 2010 June and July is not consistent with "normal" steady-state gas production from a comet at these heliocentric distances, suggesting that much of the detected CO 2 and dust was produced in an episodic event. Together, these conclusions suggest that C/2010 L5 experienced a significant outburst event when the comet was close to perihelion.

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Section: Effect Of Initial Particle Velocity and Justification For Tsupporting

confidence: 88%

The Perihelion Emission of Comet C/2010 L5 (WISE)

Kramer

Bauer

Fernández

et al. 2017

ApJ

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“…Another outburst, in 2007, was well observed, revealing a spherical envelope, a detached blob, and a central coma (see, e.g., Watanabe et al 2009;Reach et al 2010). Total ejecta mass was estimated to be (1 ∼ 610) × 10 10 kg (Altenhoff et al 2009;Reach et al 2010;Ishiguro et al 2010;Li et al 2011;Boissier et al 2012;Ishiguro et al 2013). The expansion speed on the plane of the sky of the dust envelope particles was 554 ± 5 m s −1 (Lin et al 2009;Montalto et al 2008).…”

Section: Comparison With Other Cometsmentioning

confidence: 96%

“…We applied a three-dimensional analysis to match the observed images, following the model in Ishiguro et al (2007), Hanayama et al (2012), and Ishiguro et al (2013). We adopted a power-law function for the terminal speed of ejected dust particles:…”

Section: Dust Dynamical Modelmentioning

confidence: 99%

Outbursting Comet P/2010 V1 (Ikeya-Murakami): A Miniature Comet Holmes

Ishiguro

Jewitt

Hanayama

et al. 2014

ApJ

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The short-period comet P/2010 V1 (Ikeya-Murakami, hereafter "V1") was discovered visually by two amateur astronomers. The appearance of the comet was peculiar, consisting of an envelope, a spherical coma near the nucleus and a tail extending in the anti-solar direction. We investigated the brightness and the morphological development of the comet by taking optical images with ground-based telescopes. Our observations show that V1 experienced a large-scale explosion between UT 2010 October 31 and November 3. The color of the comet was consistent with the Sun (g − R C = 0.61 ± 0.20, R C − I C = 0.20 ± 0.20, and B − R C = 0.93 ± 0.25), suggesting that dust particles were responsible for the brightening. We used a dynamical model to understand the peculiar morphology, and found that the envelope consisted of small grains (0.3-1 μm) expanding at a maximum speed of 500 ± 40 m s −1 , while the tail and coma were composed of a wider range of dust particle sizes (0.4-570 μm) and expansion speeds 7-390 m s −1 . The total mass of ejecta is ∼5 × 10 8 kg and kinetic energy ∼5 × 10 12 J. These values are much smaller than in the historic outburst of 17P/Holmes in 2007, but the energy per unit mass (1 × 10 4 J kg −1 ) is comparable. The energy per unit mass is about 10% of the energy released during the crystallization of amorphous water ice suggesting that crystallization of buried amorphous ice can supply the mass and energy of the outburst ejecta.

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“…To derive the ejection speed, mass, and kinetic energy of the dust cloud in a comprehensive manner, we conducted a model simulation to reproduce the observed morphologies of dust ejecta from the second outburst by following the scheme in Ishiguro et al (2013). The morphologies of dust clouds are generally determined by the ejection speeds and the effects of solar radiation pressure, which can be approximately given by a function of grain size.…”

Section: Ejecta Dynamical Modelmentioning

confidence: 99%

2014–2015 Multiple Outbursts of 15p/Finlay

Ishiguro

Kuroda

Hanayama

et al. 2016

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-3 -Multiple outbursts of a Jupiter-family comet, 15P/Finlay, occurred from late 2014 to early 2015. We conducted an observation of the comet after the first outburst and subsequently witnessed another outburst on 2015 January 15.6-15.7. The gas, consisting mostly of C 2 and CN, and dust particles expanded at speeds of 1,110 ± 180 m s −1 and 570 ± 40 m s −1 at a heliocentric distance of 1.0 AU. We estimated the maximum ratio of solar radiation pressure with respect to the solar gravity β max = 1.6 ± 0.2, which is consistent with porous dust particles composed of silicates and organics. We found that 10 8 -10 9 kg of dust particles (assumed to be 0.3 µm-1 mm) were ejected through each outburst. Although the total mass is three orders of magnitude smaller than that of the 17P/Holmes event observed in 2007, the kinetic energy per unit mass (10 4 J kg −1 ) is equivalent to the estimated values of 17P/Holmes and 332P/2010 V1 (Ikeya-Murakami), suggesting that the outbursts were caused by a similar physical mechanism. From a survey of cometary outbursts on the basis of voluntary reports, we conjecture that 15P/Finlay-class outbursts occur >1.5 times annually and inject dust particles from Jupiter-family comets and Encke-type comets into interplanetary space at a rate of ∼10 kg s −1 or more.

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

Cited by 12 publications

References 62 publications

The Perihelion Emission of Comet C/2010 L5 (WISE)

The Perihelion Emission of Comet C/2010 L5 (WISE)

Outbursting Comet P/2010 V1 (Ikeya-Murakami): A Miniature Comet Holmes

2014–2015 Multiple Outbursts of 15p/Finlay

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