<i>EPOXI</i>: COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN

Meech, К. J.; A’Hearn, Michael F.; Adams, Jennifer A.; Bacci, P.; Bai, J. M.; Barrera, L.; Battelino, Milan; Bauer, J. M.; Becklin, E. E.; Bhatt, B. C.; Biver, Nicolás; Bockelée‐Morvan, Dominique; Bodewits, Dennis; Böhnhardt, H.; Boissier, J.; Bonev, B. P.; Borghini, W.; Brucato, J. R.; Bryssinck, E.; Buie, M. W.; Cánovas, H.; Castellano, D.; Charnley, Steven B.; Chen, W. P.; Chiang, P. S.; Choi, Young Jun; Christian, D. J.; Chuang, Y. L.; Cochran, A. L.; Colom, P.; Combi, M. R.; Coulson, I. M.; Crovisier, J.; Russo, N. Dello; Dennerl, K.; Dewahl, K.; DiSanti, M. A.; Facchini, M.; Farnham, T. L.; Fernández, Y. R.; Florén, Hans-Gustav; Frisk, U.; Fujiyoshi, Takuya; Furusho, Reiko; Fuse, Tetsuharu; Galli, G.; García-Hernández, D. A.; Gersch, Alan; Getu, Z.; Gibb, E. L.; Gillon, M.; Guido, E.; Guillermo, R. A.; Hadamcik, Edith; Hainaut, Olivier; Hammel, H. B.; Harker, David; Harmon, J. K.; Harris, Walter M.; Hartogh, P.; Hashimoto, M.; Häusler, B.; Herter, T.; Hjalmarson, Å.; Holland, S. T.; Honda, M.; Hosseini, Sona; Howell, E. S.; Howes, N.; Hsieh, Henry H.; Hsiao, H. Y.; Hutsemékers, Damien; Immler, S.; Jackson, William M.; Jeffers, S. V.; Jehin, Emmanuël; Jones, T. J.; Ovelar, M. de Juan; Kaluna, H. M.; Karlsson, Torgny; Kawakita, Hideyo; Keane, J. V.; Keller, L. D.; Kelley, Michael S. P.; Kinoshita, Daisuke; Kiselev, N. N.; Kleyna, Jan; Knight, Matthew M.; Kobayashi, Hitomi; Kobulnicky, Henry A.; Kolokolova, L.; Kreiny, M.; Kuan, Yi‐Jehng; Küppers, M.; Lacruz, J.; Landsman, W. B.; Lara, L. M.; Lecacheux, A.; Levasseur-Regourd, Anny Chantal; Li, B.; Licandro, J.; Ligustri, R.; Lin, Z.-Y.; Lippi, M.; Lis, D. C.; Lisse, C. M.; Lovell, A. J.; Lowry, S. C.; Lu, H.; Lundin, Stefan; Magee-Sauer, K.; Magain, Pierre; Manfroid, Jean; Epifani, E. Mazzotta; McKay, Adam; Melita, M. D.; Mikuz, H.; Milam, Stefanie N.; Milani, Giannantonio; Min, M.; Moreno, R.; Mueller, B. E. A.; Mumma, M. J.; Nicolini, M.; Nolan, M. C.; Nordh, H. L.; Nowajewski, Priscilla; Team, Odin; Ootsubo, Takafumi; Paganini, L.; Perrella, C.; Pittichová, J.; Prosperi, E.; Radeva, Y. L.; Reach, W. T.; Remijan, Anthony J.; Rengel, Miriam; Riesen, T.; Rodenhuis, M.; Rodríguez, D.; Russell, R. W.; Sahu, D. K.; Samarasinha, Nalin H.; Caso, Albert Sánchez; Sandqvist, Aa.; Sarid, Gal; Sato, Masaki; Schleicher, D. G.; Schwieterman, Edward W.; Sen, A. K.; Shenoy, D.; Shi, Jianchun; Shinnaka, Yoshiharu; Skvarč, J.; Snodgrass, C.; Sitko, Michael L.; Sonnett, S.; Sosseini, S.; Sostero, G.; Sugita, Seiji; Swinyard, B. M.; Szutowicz, S.; Takato, Naruhisa; Tanga, P.; Taylor, Patrick A.; Tozzi, G. P.; Trabatti, R.; Trigo-Rodríguez, J. M.; Tubiana, C.; Val-Borro, M. de; Vacca, William D.; Vandenbussche, B.; Vaubaillion, J.; Velichko, F. P.; Velichko, Sergey; Vervack, R. J.; Vidal-Nunez, M. J.; Villanueva, G. L.; Vinante, C.; Vincent, J.-B.; Wang, M.; Wasserman, L. H.; Watanabe, J.; Weaver, Harold A.; Weissman, P. R.; Wolk, S. J.; Wooden, D. H.; Woodward, C. E.; Yamaguchi, Mitsuru; Yamashita, Takuji; Yanamandra-Fischer, P. A.; Yang, Bin; Yao, J. S.; Yeomans, D. K.; Zenn, T.; Zhao, H. B.; Ziffer, Julie

doi:10.1088/2041-8205/734/1/l1

Cited by 101 publications

(62 citation statements)

References 37 publications

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“…Images of comet Tempel were obtained before and after Deep Impact collision as a part of an international campaign (Meech et al, 2005). Internationally coordinated multisite observational programme to characterize the nuclei of comets is continuing in order to support future space missions (Meech et al, 2011a;Meech et al, 2011b;Belton et al, 2011). Similarly, HCT also participated in the internationally coordinated follow-up observations of the main belt comet P/2006 VW 139 (Hsieh et al, 2012) and C/2012 S1 (ISON) (Meech et al, 2013).…”

Section: Solar System Objectsmentioning

confidence: 99%

Indian Astronomical Observatory, Leh-Hanle

Prabhu¹

2014

Proceedings of the Indian National Science Academy

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Section: Solar System Objectsmentioning

confidence: 99%

Indian Astronomical Observatory, Leh-Hanle

Prabhu¹

2014

Proceedings of the Indian National Science Academy

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“…When the comet reached 1.4 AU (pre-perihelion) CO 2 driven activity dominated, to the point at which water ice can be driven off the surface, as if it were dust. The CO 2 driven activity would persist beyond the comet's aphelion (Meech et al, 2011).…”

Section: Parametermentioning

confidence: 99%

The persistent activity of Jupiter-family comets at 3–7AU

Kelley

Fernández

Licandro

et al. 2013

Icarus

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a b s t r a c tWe present an analysis of comet activity based on the Spitzer Space Telescope component of the Survey of the Ensemble Physical Properties of Cometary Nuclei. We show that the survey is well suited to measuring the activity of Jupiter-family comets at 3-7 AU from the Sun. Dust was detected in 33 of 89 targets (37 ± 6%), and we conclude that 21 comets (24 ± 5%) have morphologies that suggest ongoing or recent cometary activity. Our dust detections are sensitivity limited, therefore our measured activity rate is necessarily a lower limit. All comets with small perihelion distances (q < 1.8 AU) are inactive in our survey, and the active comets in our sample are strongly biased to post-perihelion epochs. We introduce the quantity fq, intended to be a thermal emission counterpart to the often reported Afq, and find that the comets with large perihelion distances likely have greater dust production rates than other comets in our survey at 3-7 AU from the Sun, indicating a bias in the discovered Jupiter-family comet population. By examining the orbital history of our survey sample, we suggest that comets perturbed to smaller perihelion distances in the past 150 yr are more likely to be active, but more study on this effect is needed.

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“…Numerous observers (Jehin et al 2010;A'Hearn et al 2011;Meech et al 2011;Samarasinha et al 2011) showed that the apparent period near 17 hr in late August/early September slowed by an unusually large amount in only a few months. This change cannot always have been linear since the apparent period was nearly unchanged from mid-2009 ) until 2010 August (Knight et al 2010); this is unsurprising since period changes would be expected to be small or nonexistant due to lack of torques when activity was weak at large heliocentric distances.…”

Section: Introductionmentioning

confidence: 99%

A Further Investigation of Apparent Periodicities and the Rotational State of Comet 103p/Hartley 2 From Combined Coma Morphology and Light Curve Data Sets

Knight

Mueller

Samarasinha

et al. 2015

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We present an analysis of Kitt Peak National Observatory and Lowell Observatory observations of comet 103P/ Hartley 2 obtained from 2010 August through December. The results are then compared with contemporaneous observations made by the EPOXI spacecraft. Each ground-based data set has previously been investigated individually; the combined data set has complementary coverage that reduces the time between observing runs and allows us to determine additional apparent periods at intermediate times. We compare CN coma morphology between ground-based data sets, making nine new measurements of apparent periods. The first five are consistent with the roughly linearly increasing apparent period during the apparition found by previous authors. The final four suggest that the change in apparent period slowed or stopped by late November. We also measure an inner coma light curve in both CN and R-band ground-based images, finding a single-peaked light curve which repeats in phase with the coma morphology. The apparent period from the light curve had significantly larger uncertainties than from the coma morphology, but varied over the apparition in a similar manner. Our ground-based light curve aligns with the published EPOXI light curve, indicating that the light curve represents changing activity rather than viewing geometry of structures in the coma. The EPOXI light curve can best be phased by a triple-peaked period near 54-55 hr that increases from October to November. This phasing reveals that the spacing between maxima is not constant, and that the overall light curve shape evolves from one triple-peaked cycle to the next. These behaviors suggest that much of the scatter in apparent periods derived from ground-based data sets acquired at similar epochs are likely due to limited sampling of the data.

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EPOXI: COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN

Cited by 101 publications

References 37 publications

Indian Astronomical Observatory, Leh-Hanle

Indian Astronomical Observatory, Leh-Hanle

The persistent activity of Jupiter-family comets at 3–7AU

A Further Investigation of Apparent Periodicities and the Rotational State of Comet 103p/Hartley 2 From Combined Coma Morphology and Light Curve Data Sets

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