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Detection of submillimeter-wave [C I]emission in gaseous debris disks of 49 Ceti and β Pictoris

Published online by Cambridge University Press:  04 September 2018

Aya E. Higuchi ,
Aki Sato ,
Takashi Tsukagoshi ,
Nami Sakai ,
Kazunari Iwasaki ,
Munetake Momose ,
Hiroshi Kobayashi ,
Daisuke Ishihara ,
Hidehiro Kaneda  and
Satoshi Yamamoto
Aya E. Higuchi
Affiliation:
The Institute of Physical and Chemical Research (RIKEN), 2-1, Hirosawa, Wako-shi, Saitama 351-0198, Japan, email: aya.higuchi@riken.jp
Aki Sato
Affiliation:
College of Science, Ibaraki University, Bunkyo 2-1-1, Mito 310-8512, Japan
Takashi Tsukagoshi
Affiliation:
College of Science, Ibaraki University, Bunkyo 2-1-1, Mito 310-8512, Japan
Nami Sakai
Affiliation:
The Institute of Physical and Chemical Research (RIKEN), 2-1, Hirosawa, Wako-shi, Saitama 351-0198, Japan, email: aya.higuchi@riken.jp
Kazunari Iwasaki
Affiliation:
Department of Earth and Space Science, Graduate School of Science Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka 560-0043, Japan
Munetake Momose
Affiliation:
College of Science, Ibaraki University, Bunkyo 2-1-1, Mito 310-8512, Japan
Hiroshi Kobayashi
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan
Daisuke Ishihara
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan
Hidehiro Kaneda
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8602, Japan
Satoshi Yamamoto
Affiliation:
Department of Physics, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
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Abstract

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We have detected [C I] 3P1–3P0 emissions in the gaseous debris disks of 49 Ceti and β Pictoris with the 10 m telescope of the Atacama Submillimeter Telescope Experiment, which is the first detection of such emissions. The line profiles of [C I] are found to resemble those of CO(J=3–2) observed with the same telescope and the Atacama Large Millimeter/submillimeter Array. This result suggests that atomic carbon (C) coexists with CO in the debris disks, and is likely formed by the photodissociation of CO. Assuming an optically thin [C I] emission with the excitation temperature ranging from 30 to 100 K, the column density of C is evaluated to be (2.2 ± 0.2) × 1017 and (2.5 ± 0.7) × 1016 cm−2 for 49 Ceti and β Pictoris, respectively. The C/CO column density ratio is thus derived to be 54 ± 19 and 69 ± 42 for 49 Ceti and β Pictoris, respectively. These ratios are higher than those of molecular clouds and diffuse clouds by an order of magnitude. The unusually high ratios of C to CO are likely attributed to a lack of H2 molecules needed to reproduce CO molecules efficiently from C. This result implies a small number of H2 molecules in the gas disk; i.e., there is an appreciable contribution of secondary gas from dust grains.

Keywords

(stars:) planetary systems: protoplanetary disksISM: atomsradio lines: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 81 - 87
Copyright
Copyright © International Astronomical Union 2018 

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