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

doi:10.1126/science.1108953

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

Cyfadran Cyfrifiadureg, Peirianneg a Gwyddoniaeth

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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.

Iaith wreiddiol	Saesneg
Tudalennau (o-i)	231-3
Nifer y tudalennau	3
Cyfnodolyn	Science
Cyfrol	308
Rhif cyhoeddi	5719
Dynodwyr Gwrthrych Digidol (DOIs)	https://doi.org/10.1126/science.1108953
Statws	Cyhoeddwyd - 8 Ebrill 2005

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10.1126/science.1108953Trwydded: CC BY-NC-ND

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@article{de6150e83d86467b8954a1ef7ca96030,

title = "The real-time stellar evolution of Sakurai's object",

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.",

author = "Marcin Hajduk and Zijlstra, {Albert A.} and Falk Herwig and {van Hoof}, {Peter A M} and Florian Kerber and Stefan Kimeswenger and Pollacco, {Don L} and Aneurin Evans and Lop{\'e}z, {Jos{\'e} A} and Myfanwy Bryce and Eyres, {Stewart P S} and Mikako Matsuura",

year = "2005",

month = apr,

day = "8",

doi = "10.1126/science.1108953",

language = "English",

volume = "308",

pages = "231--3",

journal = "Science",

issn = "1095-9203",

publisher = "American Association for the Advancement of Science ",

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TY - JOUR

T1 - The real-time stellar evolution of Sakurai's object

AU - Hajduk, Marcin

AU - Zijlstra, Albert A.

AU - Herwig, Falk

AU - van Hoof, Peter A M

AU - Kerber, Florian

AU - Kimeswenger, Stefan

AU - Pollacco, Don L

AU - Evans, Aneurin

AU - Lopéz, José A

AU - Bryce, Myfanwy

AU - Eyres, Stewart P S

AU - Matsuura, Mikako

PY - 2005/4/8

Y1 - 2005/4/8

N2 - 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.

AB - 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.

U2 - 10.1126/science.1108953

DO - 10.1126/science.1108953

M3 - Article

C2 - 15821085

VL - 308

SP - 231

EP - 233

JO - Science

JF - Science

SN - 1095-9203

IS - 5719

ER -

The real-time stellar evolution of Sakurai's object

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