C2 Phillips and CN Red bands in HD 56126 (Bakker+,

Details C2 Phillips and CN Red bands in HD 56126 (Bakker+, C2 Phillips and CN Red bands in HD 56126 (Bakker+,

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..33100893b&link_type=abstract

VizieR On-line Data Catalog: J/A+A/310/893. Originally published in: 1996A&A...310..893B

Physics

Atomic Physics

Atomic Physics, Equivalent Widths

Scientific paper

We present the detection of molecular absorption lines in the optical spectrum of the post-AGB star HD 56126. The C2 Phillips A1{PI}u- X1{SIGMA}+g(1,0), (2,0), and (3,0); Swan d3{PI}g-a3{PI}u(0,0) and (1,0); and CN Red system A2{PI}-X2{SIGMA}+ (1,0), (2,0), (3,0), and (4,0) bands have been identified. From the identification of the molecular bands we find an expansion velocity of 8.5+/-0.6km/s independent of excitation condition or molecular specie. On the basis of the expansion velocity, rotational temperatures, and molecular column densities we argue that the line-forming region is the AGB remnant. This is in agreement with the expansion velocity derived from the CO lines. We find column densities of logNC2=15.3+/-0.3cm-2 and logNCN=15.5+/-0.3cm-2, and rotational temperatures of Trot=242+/-20K and Trot=24+/-5K respectively for C2 and CN. By studying molecular line absorption in optical spectra of post-AGB stars we have found a new tracer of the AGB remnant. From comparison with the results of CO and IR observations it is possible to obtain information on non-spherical behavior of the AGB remnant. Using different molecules with different excitation conditions it should be possible to study the AGB remnant as a function of the distance to the star, and thus as a function of the evolutionary status of the star on the AGB. (6 data files).

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