Volume 517, July 2010
|Number of page(s)||9|
|Section||Planets and planetary systems|
|Published online||12 August 2010|
Polarimetric observations of comet 67P/Churyumov-Gerasimenko during its 2008–2009 apparition*
UPMC Univ. Paris 06 / LATMOS-IPSL, 11 bld d'Alembert, 78280 Guyancourt, France e-mail: [edith.hadamcik;aclr]@latmos.ipsl.fr
2 Assam Univ., Silchar 788001, India e-mail: firstname.lastname@example.org
3 IUCAA, Post Bag 4, Ganeshkhind, Pune-411007, India e-mail: email@example.com
4 LPI, 3600 Bay Area Blvd, Houston, TX 77058-1113, USA e-mail: firstname.lastname@example.org
Accepted: 12 April 2010
Context. Remote observations of the light scattered by comet 67P/Churyumov-Gerasimenko dust coma are of major importance for determining the physical properties of the particles and prepare the rendezvous with the ESA/Rosetta spacecraft in 2014.
Aims. Light scattering and especially linear polarization observations allow comparison between different coma regions and different comets, including comets that have been studied by space probes. Our aim is to retrieve physical properties of the dust particles and to characterize their evolution around perihelion passage.
Methods. Recent imaging polarimetric observations were conducted at the Haute-Provence observatory (France) on 2009 March 17–19 at 35° phase angle and at IUCAA Girawali observatory (India) on 2008 December 25-27 at 36° phase angle and on 2009 April 30–May 1 at 29° phase angle. With the imaging technique, the intensity and linear polarization variations are studied through the various coma regions. These observations are compared to other cometary data (e.g. Jupiter family comets) and to numerical and experimental simulations.
Results. The decrease in intensity as a function of the distance to nucleus in log-log scale is on average close to –1, although important variations with values down to –1.5 are noticed, in agreement with previous observations in 1982–83 and 1995–96. The intensity along the tailward direction decreases with a slope between –1.2 two months before perihelion (2009 February 28) to –1.0 two months after perihelion, and the decrease is more pronounced in the sunward direction. Before perihelion, aperture polarization values are comparable to polarization values measured on other comets at similar phase angles. The sharp decrease in intensity and the feature in the tailward direction, without any difference in polarization in the coma before perihelion, could suggest the presence of large dark particles. The post-perihelion increase in intensity and in polarization suggests that an outburst has occurred. The freshly ejected dust polarizes more the scattered light and is more sensitive to the solar radiation pressure, suggesting small micron- or submicron-sized grains.
Conclusions. Polarization and intensity variations in the coma of 67P/Churyumov-Gerasimenko are reminiscent of those noticed for some comets such as comet 81P/Wild 2 and comet 9P/Tempel 1. The presence of rather large particles can thus be suggested before and just after perihelion and the ejection of post-perihelion smaller grains, eventually in fluffy aggregates. A strong seasonal effect related to the obliquity of the comet suggests that the different grains originate in different hemispheres of the nucleus.
Key words: comets: individual: 67P/Churyumov-Gerasimenko / polarization / scattering / techniques: polarimetric
© ESO, 2010
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