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The return of activity in main-belt comet 133P/Elst-Pizarro

Hsieh, H.H., Jewitt, D., Lacerda, P., Lowry, S.C., Snodgrass, C. (2010) The return of activity in main-belt comet 133P/Elst-Pizarro. Monthly Notices of the Royal Astronomical Society: Letters, 403 (1). pp. 363-377. ISSN 0035-8711. E-ISSN 1745-3933. (doi:10.1111/j.1365-2966.2009.16120.x) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided) (KAR id:52289)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided.
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Comet 133P/Elst-Pizarro is the first known and currently best-characterized member of the main-belt comets, a recently identified class of objects that exhibit cometary activity but which are dynamically indistinguishable from main-belt asteroids. We report here on the results of a multiyear monitoring campaign from 2003 to 2008, and present observations of the return of activity in 2007. We find a pattern of activity consistent with seasonal activity modulation. Additionally, recomputation of phase function parameters using data in which 133P was inactive yields new IAU parameters of HR = 15.49 ± 0.05 mag and GR = 0.04 ± 0.05, and linear parameters of mR(1, 1, 0) = 15.80 ± 0.05 mag and ? = 0.041 ± 0.005 mag deg-1. The comparison between predicted magnitudes using these new parameters and the comet's actual brightnesses during its 2002 and 2007 active periods reveals the presence of unresolved coma during both episodes, of the order of ~0.20 of the nucleus cross-section in 2002 and ~0.25 in 2007. Multifilter observations during 133P's 2007 active outburst yield mean nucleus colours of B - V = 0.65 ± 0.03, V - R = 0.36 ± 0.01 and R - I = 0.32 ± 0.01, with no indication of significant rotational variation, and similar colours for the trail. Finally, while 133P's trail appears shorter and weaker in 2007 than in 2002, other measures of activity strength such as dust velocity and coma contamination of nucleus photometry are found to remain approximately constant. We attribute changes in trail strength to the timing of observations and projection effects, thus finding no evidence of any substantial decrease in the activity strength between 2002 and 2007. © 2010 The Authors. Journal compilation. © 2010 RAS.

Item Type: Article
DOI/Identification number: 10.1111/j.1365-2966.2009.16120.x
Additional information: Unmapped bibliographic data: LA - English [Field not mapped to EPrints] J2 - Mon. Not. R. Astron. Soc. [Field not mapped to EPrints] AD - Astrophysics Research Centre, Queen's University, Belfast BT7 1NN, United Kingdom [Field not mapped to EPrints] AD - Department of Earth and Space Sciences and Institute for Geophysics and Planetary Physics, UCLA, 3713 Geology Building, Box 951567, Los Angeles, CA 90095, United States [Field not mapped to EPrints] AD - Centre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, United States [Field not mapped to EPrints] AD - Max Planck Institute for Solar System Research, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany [Field not mapped to EPrints] AD - European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile [Field not mapped to EPrints] DB - Scopus [Field not mapped to EPrints]
Uncontrolled keywords: Asteroids, Comets: General, Comets: Individual: 133P/Elst-Pizarro, Minor planets
Subjects: Q Science > QB Astronomy
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User: Stephen Lowry
Date Deposited: 08 Dec 2015 22:04 UTC
Last Modified: 16 Nov 2021 10:21 UTC
Resource URI: (The current URI for this page, for reference purposes)

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