Hostname: page-component-77c89778f8-fv566 Total loading time: 0 Render date: 2024-07-16T23:43:00.402Z Has data issue: false hasContentIssue false
  • English
  • Français

The variability of hot protoplanetary objects and the stellar wind from central stars of planetary nebulae

Published online by Cambridge University Press:  15 December 2006

V.P. Arkhipova ,
N.P. Ikonnikova ,
G.V. Komissarova  and
R.I. Noskova
V.P. Arkhipova
Affiliation:
Sternberg State Astronomical Institute of Moscow University, Moscow, Russia email: vera@sai.msu.ru
N.P. Ikonnikova
Affiliation:
Sternberg State Astronomical Institute of Moscow University, Moscow, Russia email: vera@sai.msu.ru
G.V. Komissarova
Affiliation:
Sternberg State Astronomical Institute of Moscow University, Moscow, Russia email: vera@sai.msu.ru
R.I. Noskova
Affiliation:
Sternberg State Astronomical Institute of Moscow University, Moscow, Russia email: vera@sai.msu.ru
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The results of longtime systematic UBV-observations of 6 hot protoplanetary nebulae (PPN) with early B spectra are given. Fast stochastic brightness variations in the range of 0.$^{m}$2-0.$^{m}$4 (in $V$-band) have been found. The minimal time scale of the oscillations is from several hours to one day. The repeated spectral observations of hot protoplanetary nebulae have shown obvious variability in the hydrogen emission lines. It is suggested that the stellar wind from the future planetary nebula nucleus with variable $\dot{M}$ is responsible for variations observed in hot PPNs.

Keywords

protoplanetary nebulaephotometryvariability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 357 - 358
Copyright
© 2006 International Astronomical Union