Carbon chemistry in the envelope of VY Canis Majoris: Implications for oxygen-rich evolved stars

Lucy M Ziurys, E. D. Tenenbaum, R. L. Pulliam, N. J. Woolf, S. N. Milam

Research output: Contribution to journalArticle

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Abstract

Observations of the carbon-bearing molecules CO, HCN, CS, HNC, CN, and HCO+ have been conducted toward the circumstellar envelope of the oxygen-rich red supergiant star, VY Canis Majoris (VY CMa), using the Arizona Radio Observatory (ARO). CO and HCN were also observed toward the O-rich shells of NML Cyg, TX Cam, IK Tau, and W Hya. Rotational transitions of these species at 1 mm, 0.8 mm, and 0.4 mm were measured with the ARO Submillimeter Telescope, including the J = 6→5 line of CO at 691 GHz toward TX Cam and W Hya. The ARO 12 m was used for 2 mm and 3 mm observations. Four transitions were observed for HCO+ in VY CMa, the first definitive identification of this ion in a circumstellar envelope. Molecular line profiles from VY CMa are complex, indicating three separate outflows: a roughly spherical flow and separate red- and blueshifted winds, as suggested by earlier observations. Spectra from the other sources appear to trace a single outflow component. The line data were modeled with a radiative transfer code to establish molecular abundances relative to H2 and source distributions. Abundances for CO derived for these objects vary over an order of magnitude, f ∼ 0.4-5 × 10-4, with the lower values corresponding to the supergiants. For HCN, a similar range in abundance is found (f ∼ 0.9-9 × 10-6), with no obvious dependence on the mass-loss rate. In VY CMa, HCO+ is present in all three outflows with f ∼ 0.4-1.6 × 10-8 and a spatial extent similar to that of CO. HNC is found only in the red- and blueshifted components with [HCN]/[HNC] ∼ 150-190, while [CN]/[HCN] ∼ 0.01 in the spherical flow. All three velocity components are traced in CS, which has a confined spatial distribution and f ∼ 2-6 × 10-7. These observations suggest that carbon-bearing molecules in O-rich shells are produced by a combination of photospheric shocks and photochemistry. Shocks may play a more prominent role in the supergiants because of their macroturbulent velocities.

Original languageEnglish (US)
Pages (from-to)1604-1613
Number of pages10
JournalAstrophysical Journal
Volume695
Issue number2
DOIs
StatePublished - Apr 20 2009

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envelopes
outflow
observatory
chemistry
radio
stars
cams
observatories
oxygen
carbon
shell
shock
photochemistry
supergiant stars
radiative transfer
relative abundance
photochemical reactions
spatial distribution
molecules
ion

Keywords

  • Astrochemistry
  • Circumstellar matter
  • Radio lines: stars
  • Stars: AGB and post-AGB
  • Supergiants

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Carbon chemistry in the envelope of VY Canis Majoris : Implications for oxygen-rich evolved stars. / Ziurys, Lucy M; Tenenbaum, E. D.; Pulliam, R. L.; Woolf, N. J.; Milam, S. N.

In: Astrophysical Journal, Vol. 695, No. 2, 20.04.2009, p. 1604-1613.

Research output: Contribution to journalArticle

Ziurys, Lucy M ; Tenenbaum, E. D. ; Pulliam, R. L. ; Woolf, N. J. ; Milam, S. N. / Carbon chemistry in the envelope of VY Canis Majoris : Implications for oxygen-rich evolved stars. In: Astrophysical Journal. 2009 ; Vol. 695, No. 2. pp. 1604-1613.
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AU - Milam, S. N.

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