Abstract
We report the detection of an Ha emission-line structure in the upstream side of the planetary nebula NGC 40, which is predicted by numerical simulations, and which is attributed to Rayleigh-Taylor instability. Such a Rayleigh-Taylor instability is expected to occur at early stages of the interaction process between the interstellar medium (ISM) and a fast moving planetary nebula, as is the case for NGC 40. We resolved the Rayleigh-Taylor instability "tongues", as well as the flatness of the nebula around the "tongues", which results from the deceleration by the ISM.
Original language | English |
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Pages (from-to) | 689-692 |
Number of pages | 4 |
Journal | Astronomy and Astrophysics |
Volume | 391 |
Issue number | 2 |
DOIs | |
State | Published - Aug 2002 |
Externally published | Yes |
Keywords
- Instabilities
- ISM: structure
- Planetary nebulae: general
- Planetary nebulae: individual: NGC 40