Modelling the X-ray, EUV and infrared coronal-line emission from PNe.

Details Modelling the X-ray, EUV and infrared coronal-line emission from PNe. Modelling the X-ray, EUV and infrared coronal-line emission from PNe.

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...309..648z&link_type=abstract

Astronomy and Astrophysics, v.309, p.648-654

Astronomy and Astrophysics

Astrophysics

26

Planetary Nebulae: General, X-Ray: Interstellar, Infrared: Interstellar: Lines

Scientific paper

We present spherically symmetric interacting-winds model of planetary nebulae aimed at the study of the hot bubble in their structure. A similarity solution for the hot-bubble structure is derived in the case of a time-dependent wind of the central star and taking into account the effects of thermal conductivity. This solution is used to model the X-ray, EUV and infrared-coronal line emission (λ>1μ) from planetary nebulae. These results can be used to check the consistency of the interacting-winds model by a comparison with space and ground-based observations with high spatial resolution.

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