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- W2012375622 abstract "We have observed cyclic C|$_3$|H|$_2$| (|$J_{K_{a}K_{c}}= 2_{12}$|–|$1_{01}, 2_{02}$|–|$1_{11}, 3_{12}$|–|$3_{03}$|) lines at the 3 mm wavelength region toward the starless TMC-1C cloud and the protostellar core of L 1527 with the 45 m telescope at Nobeyama Radio Observatory. In both clouds, the |$2_{12}$|–|$1_{01}$| and |$2_{02}$|–|$1_{11}$| lines are strongly detected, while the |$3_{12}$|–|$3_{03}$| line is only detected toward the center of the protostellar core L 1527. From our statistical equilibrium analyses of the ortho-C|$_3$|H|$_2$| (|$2_{12}$|–|$1_{01}$|) and the para-C|$_3$|H|$_2$| (|$2_{02}$|–|$1_{11}$|) lines, the ortho-to-para ratios of C|$_3$|H|$_2$| are determined to be |$2.4pm0.1$| and |$2.5pm0.5$| in TMC-1C and L 1527, respectively. These values are lower than the statistical value of 3, although the error of the ratio in L 1527 is large. Since thermal equilibrium with a dust temperature of 10 K still gives a ratio of 3 in c-C|$_3$|H|$_2$|, this result should suggest the lower ortho-to-para ratio of the precursor molecule, c-C|$_3$|H|$_{3}^{+}$|, which is thought to be mainly produced by C|$_3$|H|$^{+} +$| H|$_2$|. Thus, we conclude that the lower ortho-to-para ratio of c-C|$_3$|H|$_2$| is due to a lower ortho-to-para ratio of H|$_{2}$| than the statistical value." @default.
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- W2012375622 date "2001-04-25" @default.
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- W2012375622 title "The Ortho-to-Para Ratio and the Chemical Properties of C<sub>3</sub>H<sub>2</sub>in Dark Cloud Cores" @default.
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