Gas-phase models for the evolved planetary nebulae NGC 6781, M4-9 and NGC 7293
| Autor: | O. M. Shalabiea, Tom J. Millar, M. S. El-Nawawy, Alaa Ali |
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| Rok vydání: | 2001 |
| Předmět: |
Physics
Reflection nebula Astrophysics::High Energy Astrophysical Phenomena Astronomy Astronomy and Astrophysics Bipolar nebula Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Planetary nebula Stars Emission nebula Orders of magnitude (time) Space and Planetary Science Ionization Astrophysics::Solar and Stellar Astrophysics Asymptotic giant branch Astrophysics::Earth and Planetary Astrophysics Astrophysics::Galaxy Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 325:881-885 |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1046/j.1365-8711.2001.04513.x |
| Popis: | We have studied the chemistry of the molecular gas in evolved planetary nebulae. Three pseudo-time-dependent gas-phase models have been constructed for dense (104–105 cm−3) and cool (T∼15 K) clumpy envelopes of the evolved nebulae NGC 6781, M4-9 and NGC 7293. The three nebulae are modelled as carbon-rich stars evolved from the asymptotic giant branch to the late planetary nebula phase. The clumpy neutral envelopes are subjected to ultraviolet radiation from the central star and X-rays that enhance the rate of ionization in the clumps. With the ionization rate enhanced by four orders of magnitude over that of the ISM, we find that resultant abundances of the species HCN, HNC, HC3N and SiC2 are in good agreement with observations, while those of CN, HCO+, CS and SiO are in rough agreement. The results indicate that molecular species such as CH, CH2, CH2+, HCl, OH and H2O are anticipated to be highly abundant in these objects. |
| Databáze: | OpenAIRE |
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