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<i>EPOXI</i> : COMET 103P/HARTLEY 2 OBSERVATIONS FROM A WORLDWIDE CAMPAIGN
Meech, K. J.,A’Hearn, M. F.,Adams, J. A.,Bacci, P.,Bai, J.,Barrera, L.,Battelino, M.,Bauer, J. M.,Becklin, E.,Bhatt, B.,Biver, N.,Bockelé,e-Morvan, D.,Bodewits, D.,Bö,hnhardt, H.,Boissier, J IOP Publishing 2011 ASTROPHYSICAL JOURNAL LETTERS - Vol.734 No.1
<P>Earth- and space-based observations provide synergistic information for space mission encounters by providing data over longer timescales, at different wavelengths and using techniques that are impossible with an in situ flyby. We report here such observations in support of the EPOXI spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and dark, and exhibited a very rapidly changing rotation period. Prior to the onset of activity, the period was similar to 16.4 hr. Starting in 2010 August the period changed from 16.6 hr to near 19 hr in December. With respect to dust composition, most volatiles and carbon and nitrogen isotope ratios, the comet is similar to other Jupiter-family comets. What is unusual is the dominance of CO2-driven activity near perihelion, which likely persists out to aphelion. Near perihelion the comet nucleus was surrounded by a large halo of water-ice grains that contributed significantly to the total water production.</P>
FRAGMENTATION KINEMATICS IN COMET 332P/IKEYA-MURAKAMI
Jewitt, David,Mutchler, Max,Weaver, Harold,Hui, Man-To,Agarwal, Jessica,Ishiguro, Masateru,Kleyna, Jan,Li, Jing,Meech, Karen,Micheli, Marco,Wainscoat, Richard,Weryk, Robert American Astronomical Society 2016 ASTROPHYSICAL JOURNAL LETTERS - Vol.829 No.1
<P>We present initial time-resolved observations of the split comet 332P/Ikeya-Murakami taken using the Hubble Space Telescope. Our images reveal a dust-bathed cluster of fragments receding from their parent nucleus at projected speeds in the range 0.06-3.5 m s(-1) from which we estimate ejection times from 2015 October to December. The number of fragments with effective radii greater than or similar to 20 m follows a differential power law with index gamma = -3.6 +/- 0.6, while smaller fragments are less abundant than expected from an extrapolation of this power law. We argue that, in addition to losses due to observational selection, torques from anisotropic outgassing are capable of destroying the small fragments by driving them quickly to rotational instability. Specifically, the spin-up times of fragments. 20 m in radius are shorter than the time elapsed since ejection from the parent nucleus. The effective radius of the parent nucleus is re <= 275 m (geometric albedo 0.04 assumed). This is about seven times smaller than previous estimates and results in a nucleus mass at least 300 times smaller than previously thought. The mass in solid pieces, 2 x 10(9) kg, is about 4% of the mass of the parent nucleus. As a result of its small size, the parent nucleus also has a short spin-up time. Brightness variations in time-resolved nucleus photometry are consistent with rotational instability playing a role in the release of fragments.</P>
SEARCH FOR THE RETURN OF ACTIVITY IN ACTIVE ASTEROID 176P/LINEAR
Hsieh, Henry H.,Denneau, Larry,Fitzsimmons, Alan,Hainaut, Olivier R.,Ishiguro, Masateru,Jedicke, Robert,Kaluna, Heather M.,Keane, Jacqueline V.,Kleyna, Jan,Lacerda, Pedro,MacLennan, Eric M.,Meech, Kar American Institute of Physics 2014 The Astronomical journal Vol.147 No.4
<P>We present the results of a search for the reactivation of active asteroid 176P/LINEAR during its 2011 perihelion passage using deep optical observations obtained before, during, and after that perihelion passage. Deep composite images of 176P constructed from data obtained between 2011 June and 2011 December show no visible signs of activity, while photometric measurements of the object during this period also show no significant brightness enhancements similar to that observed for 176P between 2005 November and 2005 December when it was previously observed to be active. An azimuthal search for dust emission likewise reveals no evidence for directed emission (i.e., a tail, as was previously observed for 176P), while a one-dimensional surface brightness profile analysis shows no indication of a spherically symmetric coma at any time in 2011. We conclude that 176P did not in fact exhibit activity in 2011, at least not on the level on which it exhibited activity in 2005, and suggest that this could be due to the devolatization or mantling of the active site responsible for its activity in 2005.</P>