000002068 001__ 2068
000002068 005__ 20160701171658.0
000002068 0247_ $$2DOI$$a10.1126/science.1108953
000002068 037__ $$aASTROimport-225
000002068 100__ $$aHajduk, M.
000002068 245__ $$aThe Real-Time Stellar Evolution of Sakurai's Object
000002068 260__ $$c2005
000002068 520__ $$aAfter a hot white dwarf ceases its nuclear burning, its helium may briefly and explosively reignite. This causes the star to evolve back into a cool giant, whereupon it experiences renewed mass ejection before reheating. A reignition event of this kind was observed in 1996 in V4334 Sgr (Sakurai's object). Its temperature decrease was 100 times the predicted rate. To understand its unexpectedly fast evolution, we have developed a model in which convective mixing is strongly suppressed under the influence of flash burning. The model predicts equally rapid reheating of the star. Radio emission from freshly ionized matter now shows that this reheating has begun. Such events may be an important source of carbon and carbonaceous dust in the Galaxy. 
000002068 700__ $$a Zijlstra, A. A.
000002068 700__ $$a Herwig, F.
000002068 700__ $$a van Hoof, P. A. M.
000002068 700__ $$a Kerber, F.
000002068 700__ $$a Kimeswenger, S.
000002068 700__ $$a Pollacco, D. L.
000002068 700__ $$a Evans, A.
000002068 700__ $$a Lopéz, J. A.
000002068 700__ $$a Bryce, M.
000002068 700__ $$a Eyres, S. P. S.
000002068 700__ $$a Matsuura, M.
000002068 773__ $$c231-233$$i5719$$pScience$$v308$$y2005
000002068 85642 $$ahttp://esoads.eso.org/abs/2005Sci...308..231H
000002068 905__ $$apublished in
000002068 980__ $$aREFERD