Peter A. M. van Hoof

Publications (2)31.2 Total impact

• Source

  Available from: Stewart Eyres

  Article: The real-time stellar evolution of Sakurai's object.

  Marcin Hajduk, Albert A Zijlstra, Falk Herwig, Peter A M van Hoof, Florian Kerber, Stefan Kimeswenger, Don L Pollacco, Aneurin Evans, José A Lopéz, Myfanwy Bryce, Stewart P S Eyres, Mikako Matsuura
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  ABSTRACT: After a hot white dwarf ceases its nuclear burning, its helium may briefly and explosively reignite. This causes the star to evolve back into a cool giant, whereupon it experiences renewed mass ejection before reheating. A reignition event of this kind was observed in 1996 in V4334 Sgr (Sakurai's object). Its temperature decrease was 100 times the predicted rate. To understand its unexpectedly fast evolution, we have developed a model in which convective mixing is strongly suppressed under the influence of flash burning. The model predicts equally rapid reheating of the star. Radio emission from freshly ionized matter now shows that this reheating has begun. Such events may be an important source of carbon and carbonaceous dust in the Galaxy.
  Science 05/2005; 308(5719):231-3. · 31.20 Impact Factor
• Source

  Available from: arxiv.org

  Article: Radio and Infrared Emission from a [WC]-Type Planetary Nebula in the LMC

  Albert A. Zijlstra, Peter A. M. van Hoof, Jessica M. Chapman, Cecile Loup
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  ABSTRACT: Radio continuum emission has been detected from a planetary nebula in the Large Magellanic Cloud: this is the first radio continuum detection for any planetary nebula outside our galaxy. The radio flux density is a factor of two lower than predicted from the \hbeta\ flux. This could be due either to a two-component morphology or to a stellar contribution to the \hbeta\ emission. We have modeled the optical and infrared spectrum using the photo-ionisation code Cloudy: a very good fit is obtained if we assume the nebula is carbon rich. The derived diameter implies an evolutionary age of the nebula of $<1000\yr$, similar to what is derived from the IRAS colours alone. The central star, which is of [WC] type, has a much higher stellar temperature than Galactic [WC] stars showing similar circumstellar IRAS colours. An explanation could be that the expansion velocity of the nebula is lower than those of its galactic counterparts. This radio detection indicates that accurate nebular luminosities could be determined from their radio emission for many LMC planetary nebulae.
  04/1994;