TY - JOUR
T1 - The 10 micron spectra of comet C/2002 V1 (NEAT) and C/2001 RX14 (LINEAR)
AU - Honda, Mitsuhiko
AU - Watanabe, Jun Ichi
AU - Yamashita, Takuya
AU - Kataza, Hirokazu
AU - Okamoto, Yoshiko K.
AU - Miyata, Takashi
AU - Sako, Shigeyuki
AU - Fujiyoshi, Takuya
AU - Kawakita, Hideyo
AU - Furusho, Reiko
AU - Kinoshita, Daisuke
AU - Sekiguchi, Tomohiko
AU - Ootsubo, Takafumi
AU - Onaka, Takashi
PY - 2004/1/20
Y1 - 2004/1/20
N2 - We have carried out mid-infrared 8-13 μm spectroscopic observations of C/2002 V1 (NEAT) and C/2001 RX14 (LINEAR) on 2003 January 10-11 UT using the Cooled Mid-Infrared Camera and Spectrometer (COMICS) on the 8.2 m Subaru Telescope. The spectra of C/2002 V1 showed the broad silicate feature with the 11.2 μm peak, indicating the presence of crystalline olivine grains. The spectra of C/2001 RX14 also showed the broad trapezoidal silicate feature. The silicate feature profile of C/2002 V1 is explained by a combination of small (0.1 μm) amorphous olivine and pyroxene, large (2.0 μm) amorphous silicate, and small crystalline forsterite grains, while that of C/2001 RX14 is explained by small and large amorphous silicate grains without crystalline silicate grains. The ubiquity of large grains and crystalline silicate grains among these Oort Cloud comets indicates processing of the primordial interstellar matter in the early solar system and incorporation into the region where these cometary nuclei were formed.
AB - We have carried out mid-infrared 8-13 μm spectroscopic observations of C/2002 V1 (NEAT) and C/2001 RX14 (LINEAR) on 2003 January 10-11 UT using the Cooled Mid-Infrared Camera and Spectrometer (COMICS) on the 8.2 m Subaru Telescope. The spectra of C/2002 V1 showed the broad silicate feature with the 11.2 μm peak, indicating the presence of crystalline olivine grains. The spectra of C/2001 RX14 also showed the broad trapezoidal silicate feature. The silicate feature profile of C/2002 V1 is explained by a combination of small (0.1 μm) amorphous olivine and pyroxene, large (2.0 μm) amorphous silicate, and small crystalline forsterite grains, while that of C/2001 RX14 is explained by small and large amorphous silicate grains without crystalline silicate grains. The ubiquity of large grains and crystalline silicate grains among these Oort Cloud comets indicates processing of the primordial interstellar matter in the early solar system and incorporation into the region where these cometary nuclei were formed.
KW - Comets: individual (C/2002 V1, C/2001 RX14)
KW - Infrared: solar system
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U2 - 10.1086/380478
DO - 10.1086/380478
M3 - Article
AN - SCOPUS:1642602197
VL - 601
SP - 577
EP - 582
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 I
ER -