1. Dust measurements in the coma of comet 67P/Churyumov-Gerasimenko inbound to the Sun
by Alessandra Rotundi, Holger Sierks, Vincenzo Della Corte, Marco Fulle, Pedro J. Gutierrez, Luisa Lara, Cesare Barbieri, Philippe L. Lamy, Rafael Rodrigo, Detlef Koschny, Hans Rickman, Horst Uwe Keller, José J. López-Moreno, Mario Accolla, Jessica Agarwal, Michael F. A’Hearn, Nicolas Altobelli, Francesco Angrilli, M. Antonietta Barucci, Jean-Loup Bertaux, Ivano Bertini, Dennis Bodewits, Ezio Bussoletti, Luigi Colangeli, Massimo Cosi, Gabriele Cremonese, Jean-Francois Crifo, Vania Da Deppo, Björn Davidsson, Stefano Debei, Mariolino De Cecco, Francesca Esposito, Marco Ferrari, Sonia Fornasier, Frank Giovane, Bo Gustafson, Simon F. Green, Olivier Groussin, Eberhard Grün, Carsten Güttler, Miguel L. Herranz, Stubbe F. Hviid, Wing Ip, Stavro Ivanovski, José M. Jerónimo, Laurent Jorda, Joerg Knollenberg, Rainer Kramm, Ekkehard Kührt, Michael Küppers, Monica Lazzarin, Mark R. Leese, Antonio C. López-Jiménez, Francesca Lucarelli, Stephen C. Lowry, Francesco Marzari, Elena Mazzotta Epifani, J. Anthony M. McDonnell, Vito Mennella, Harald Michalik, Antonio Molina, Rafael Morales, Fernando Moreno, Stefano Mottola, Giampiero Naletto, Nilda Oklay, José L. Ortiz, Ernesto Palomba, Pasquale Palumbo, Jean-Marie Perrin, Julio Rodríguez, Lola Sabau, Colin Snodgrass, Roberto Sordini, Nicolas Thomas, Cecilia Tubiana, Jean-Baptiste Vincent, Paul Weissman, Klaus-Peter Wenzel, Vladimir Zakharov, and John C. Zarnecki
Science
Volume 347(6220):aaa3905
January 23, 2015
Published by AAAS

2. Fig. 1 Detections of single grains by OSIRIS.
Detections of single grains by OSIRIS. (Top) Bound grains detected in the first set of NAC images (each labeled by a number from 001 to 353) and the brightest three tracks of the 48 outflowing grains (each labeled by letters a, b, and c). The 67P nucleus is visible at the top of the panel. (Bottom) Zoom centered on track c. The images were shifted to align stars on the same pixels. The spacecraft motion is to the right, with an angle of 6° counterclockwise from the +x image axis. Grain c shows all of the expected four white and black tracks; grains a and b have two tracks outside the image. The detections of bound grains (white-black-white-black dots) show a uniform space distribution. Further details and explanations are available in the supplementary materials.
Alessandra Rotundi et al. Science 2015;347:aaa3905
Published by AAAS

3. Fig. 2 67P grain mass distribution.
67P grain mass distribution. (Left) Mass distribution of 67P dust grains as measured by GIADA and OSIRIS. Dot-dashed line: dust loss rate by GIADA (three lower-mass bins) and OSIRIS (three higher-mass bins) at bulk density 1 × 103 kg m−3. Dashed line: dust loss rate by GIADA (three lower-mass bins) and OSIRIS (three higher-mass bins) at bulk density 3 × 103 kg m−3. Both the mass distributions have differential size distribution power law indices close to –2 in the three lower-mass bins. Solid line: average dust loss rate predicted by (18) at 3.2 AU. Differential size distribution power index = –4 in the three higher-mass bins and –3 elsewhere. (Right) Solid line: dust coma brightness-equivalent size Afρ derived from GIADA (three lower-mass bins) and OSIRIS (three higher-mass bins) data with bulk density 1 × 103 kg m−3. Dot-dashed line: Afρ derived from GIADA (three lower-mass bins) and OSIRIS (three higher-mass bins) data with bulk density 3 × 103 kg m−3. Both of these distributions have a clear maximum in the 10−8- to 10−7-kg mass bin, corresponding to a size of hundreds of micrometers.
Alessandra Rotundi et al. Science 2015;347:aaa3905
Published by AAAS