Imaging polarimetry of Comet 9P/Tempel before and after the Deep Impact

Furusho, Reiko; Ikeda, Yuji; Kinoshita, Daisuke; Ip, W.-H.; Kawakita, Hideyo; Kasuga, Toshihiro; Sato, Yusuke; Lin, H. C.; Chang, Ming Shin; Lin, Z.-Y.; Watanabe, Jun

doi:10.1016/j.icarus.2007.03.036

Cited by 26 publications

(22 citation statements)

References 13 publications

(17 reference statements)

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“…Table 1 shows that the both P l aggregates have a positive polarization and that for the com-P l pact aggregates (the high-velocity ejecta) is larger than that for the fluffy aggregates (the low-velocity ejecta). This is consistent with the observation by Furusho et al (2007), who showed that the high-velocity ejecta have a slightly higher compared P l with the low-velocity ejecta. The STO data at time hr after the DI event are shown t p 3.5 by STO-S as infrared spectra at various radial distances.…”

Section: Aggregate Modelsupporting

confidence: 93%

“…Thus, the STO data T c at hr is well explained by the standard model. In sumt p 3.5 mary, the optical properties of the compact and fluffy aggregates based on the standard model well account for the observational data used by STO-K, Furusho et al (2007), and STO-S.…”

Section: Aggregate Modelmentioning

confidence: 61%

“…Finally, they concluded that even at a depth of only several tens of centimeters below the surface, comet materials keep their primordial composition together with submicron-sized silicate grains. Furusho et al (2007) supported this interpretation by measuring slightly higher linear polarizations for the high-velocity ejecta compared with the low-velocity ejecta. Harker et al (2007) also supported these interpretations from their infrared observations.…”

Section: Introductionmentioning

confidence: 61%

“…This agrees with the S si observational data by STO-K that show the high-velocity (∼180 m s Ϫ1 ) ejecta to have higher and lower than the low-T S c si velocity ejecta (∼100 m s Ϫ1 ). We next compare the polarimetric observation by Furusho et al (2007) with in Table 1. Table 1 shows that the both P l aggregates have a positive polarization and that for the com-P l pact aggregates (the high-velocity ejecta) is larger than that for the fluffy aggregates (the low-velocity ejecta).…”

Section: Aggregate Modelmentioning

confidence: 99%

“…1), corresponding to an average t p 3.5 velocity of 60 m s Ϫ1 . Furthermore, STO-K claimed that the high-velocity ejecta (տ160 m s Ϫ1 ) were observed at -9 t p 6 hr by Furusho et al (2007) as highly polarized regions at տ6Љ. Therefore, the KFH model suggests that the high-velocity (∼180 m s Ϫ1 ) carbonaceous grains were suddenly decelerated to ∼60 m s Ϫ1 during -3.5 hr and then accelerated again t p 2 to տ160 m s Ϫ1 after hr.…”

Section: Peculiar Pristine Carbon Crustmentioning

confidence: 99%

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Comet 9P/Tempel 1: Interpretation with theDeep ImpactResults

Yamamoto

Kimura

Zubko

et al. 2008

ApJ

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According to our common understandings, the original surface of a short-period comet nucleus has been lost by sublimation processes during its close approaches to the Sun. Sublimation results in the formation of a dust mantle on the retreated surface and in chemical differentiation of ices over tens or hundreds of meters below the mantle. In the course of NASA's Deep Impact mission, optical and infrared imaging observations of the ejecta plume were conducted by several researchers, but their interpretations of the data came as a big surprise: (1) The nucleus of comet 9P/Tempel 1 is free of a dust mantle but maintains its pristine crust of submicron-sized carbonaceous grains. (2) Primordial materials are accessible already at a depth of several tens of centimeters with abundant silicate grains of submicrometer sizes. In this study, we demonstrate that a standard model of cometary nuclei explains well available observational data: (1) A dust mantle with a thickness of ∼1-2 m builds up on the surface, where compact aggregates larger than tens of micrometers dominate. (2) Large fluffy aggregates are embedded in chemically differentiated layers as well as in the deepest part of the nucleus with primordial materials. We conclude that the Deep Impact results do not need any peculiar view of a comet nucleus.

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Section: Aggregate Modelsupporting

confidence: 93%

Section: Aggregate Modelmentioning

confidence: 61%