Radio Observations of comets C/2002 X5 (Kudo-Fujikawa) and C/2002 V1 (NEAT) at very small heliocentric distances.

Details Radio Observations of comets C/2002 X5 (Kudo-Fujikawa) and C/2002 V1 (NEAT) at very small heliocentric distances. Radio Observations of comets C/2002 X5 (Kudo-Fujikawa) and C/2002 V1 (NEAT) at very small heliocentric distances.

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.2805b&link_type=abstract

American Astronomical Society, DPS meeting #35, #28.05; Bulletin of the American Astronomical Society, Vol. 35, p.968

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Scientific paper

Comets C/2002 X5 (Kudo-Fujikawa) and C/2002 V1 (NEAT), discovered in fall 2002, have been the brightest comets to come closer than 0.2 AU from the Sun for several years. Target-of-opportunity observations of both comets were made at IRAM close to their perihelion, at 0.19 AU on Jan. 29, 2003, for C/2002 X5 and 0.10 AU on Feb. 18, for C/2002 V1. In addition, C/2002 X5 was observed at 0.55 AU pre-perihelion and 1.18 AU post-perihelion. The water outgassing rate was monitored almost daily from the observations of the OH radical with the Nançay radio-telescope between Jan. 1 and April 9 (C/2002 X5) and Dec. 31, 2002 and April 26 (C/2002 V1). The Odin satellite also observed and detected the water line at 557 GHz in C/2002 X5 between March 3 and 30, 2003.
The near perihelion observations at IRAM were challenging because of small solar elongations (5-8o) and lack of precise astrometry at that time.
HCN, CS, CH3OH and HNC were detected in both comets. CH3CN and HC3N were also detected in C/2002 X5. The high S/N (>50) detections of the HCN(3-2) line at 0.21 and 0.11 AU show that the maximum gas velocity observed in both comets did not exceed 2.1 km/s. The HNC/HCN ratio was found to be around 20% at 0.2--0.1 AU, similar to the maximum value observed in other comets. We may have expected a higher ratio if HNC was produced by the thermal degradation of organic grains. The detection of CS very close to the Sun provides constraints on its photodissociation. Upper limits on other species abundances will be presented and the origin of molecular species in the coma will be discussed.

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