NEW DETECTIONS of HNC in PLANETARY NEBULAE: EVOLUTION of the [HCN]/[HNC] RATIO

D. R. Schmidt, Lucy M Ziurys

Research output: Contribution to journalArticle

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Abstract

New detections of HNC have been made toward 11 planetary nebulae (PNe), including K4-47, K3-58, K3-17, M3- 28, and M4-14. These sources, which represent a wide range of ages and morphologies, had previously been observed in HCN by Schmidt & Ziurys. Measurements of the J=10 and J = 3 → 2 transitions of HNC near 90 and 271 GHz were conducted using the new 12 m and the Sub-Millimeter Telescope of the Arizona Radio Observatory. HCN and HNC were also identified via their J = 1 → 0 lines toward eight positions across the Helix Nebula (NGC 7293). Column densities for HNC, determined from radiative transfer modeling, were Ntot(HNC) ∼ (0.06-4.0) ×1013 cm-2, corresponding to fractional abundances with respect to H2 of f ∼ (0.02-1.4) × 10-7. The HCN and HNC column densities across the Helix were found to be Ntot (HCN)∼(0.2-2.4)×1012cm-2 and N (HNC) tot ∼ (0.07-1.6)×1012cm-2, with fractional abundances of (0.2-3.2)×10-7 and (0.09-2.2) × 10-7. The [HCN]/[HNC] ratio varied between sim; 1-8 for all PNe, with [HCN]/[HNC] ∼1-4 across the Helix. These values are greatly reduced from what has been found in asymptotic giant branch stars, where the ratio is typically >100. Both the abundance of HNC and the [HCN]/[HNC] ratio do not appear to vary significantly with nebular age across a time span of ∼10,000 years, in contrast to predictions of chemical models. The increase in HNC appears to arise in the proto-planetary stage, but becomes "frozen" once the PN phase is reached.

Original languageEnglish (US)
Article number79
JournalAstrophysical Journal
Volume835
Issue number1
DOIs
StatePublished - Jan 20 2017

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planetary nebulae
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Keywords

  • astrochemistry
  • ISM: molecules
  • planetary nebulae: general
  • radio lines: ISM

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

NEW DETECTIONS of HNC in PLANETARY NEBULAE : EVOLUTION of the [HCN]/[HNC] RATIO. / Schmidt, D. R.; Ziurys, Lucy M.

In: Astrophysical Journal, Vol. 835, No. 1, 79, 20.01.2017.

Research output: Contribution to journalArticle

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abstract = "New detections of HNC have been made toward 11 planetary nebulae (PNe), including K4-47, K3-58, K3-17, M3- 28, and M4-14. These sources, which represent a wide range of ages and morphologies, had previously been observed in HCN by Schmidt & Ziurys. Measurements of the J=10 and J = 3 → 2 transitions of HNC near 90 and 271 GHz were conducted using the new 12 m and the Sub-Millimeter Telescope of the Arizona Radio Observatory. HCN and HNC were also identified via their J = 1 → 0 lines toward eight positions across the Helix Nebula (NGC 7293). Column densities for HNC, determined from radiative transfer modeling, were Ntot(HNC) ∼ (0.06-4.0) ×1013 cm-2, corresponding to fractional abundances with respect to H2 of f ∼ (0.02-1.4) × 10-7. The HCN and HNC column densities across the Helix were found to be Ntot (HCN)∼(0.2-2.4)×1012cm-2 and N (HNC) tot ∼ (0.07-1.6)×1012cm-2, with fractional abundances of (0.2-3.2)×10-7 and (0.09-2.2) × 10-7. The [HCN]/[HNC] ratio varied between sim; 1-8 for all PNe, with [HCN]/[HNC] ∼1-4 across the Helix. These values are greatly reduced from what has been found in asymptotic giant branch stars, where the ratio is typically >100. Both the abundance of HNC and the [HCN]/[HNC] ratio do not appear to vary significantly with nebular age across a time span of ∼10,000 years, in contrast to predictions of chemical models. The increase in HNC appears to arise in the proto-planetary stage, but becomes {"}frozen{"} once the PN phase is reached.",
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N2 - New detections of HNC have been made toward 11 planetary nebulae (PNe), including K4-47, K3-58, K3-17, M3- 28, and M4-14. These sources, which represent a wide range of ages and morphologies, had previously been observed in HCN by Schmidt & Ziurys. Measurements of the J=10 and J = 3 → 2 transitions of HNC near 90 and 271 GHz were conducted using the new 12 m and the Sub-Millimeter Telescope of the Arizona Radio Observatory. HCN and HNC were also identified via their J = 1 → 0 lines toward eight positions across the Helix Nebula (NGC 7293). Column densities for HNC, determined from radiative transfer modeling, were Ntot(HNC) ∼ (0.06-4.0) ×1013 cm-2, corresponding to fractional abundances with respect to H2 of f ∼ (0.02-1.4) × 10-7. The HCN and HNC column densities across the Helix were found to be Ntot (HCN)∼(0.2-2.4)×1012cm-2 and N (HNC) tot ∼ (0.07-1.6)×1012cm-2, with fractional abundances of (0.2-3.2)×10-7 and (0.09-2.2) × 10-7. The [HCN]/[HNC] ratio varied between sim; 1-8 for all PNe, with [HCN]/[HNC] ∼1-4 across the Helix. These values are greatly reduced from what has been found in asymptotic giant branch stars, where the ratio is typically >100. Both the abundance of HNC and the [HCN]/[HNC] ratio do not appear to vary significantly with nebular age across a time span of ∼10,000 years, in contrast to predictions of chemical models. The increase in HNC appears to arise in the proto-planetary stage, but becomes "frozen" once the PN phase is reached.

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