A faint type of supernova from a white dwarf with a helium-rich companion

被引：269

作者：

Perets, H. B. ^{[1
,2
]}

Gal-Yam, A. ^{[1
]}

Mazzali, P. A. ^{[3
,4
,5
]}

Arnett, D. ^{[6
]}

Kagan, D. ^{[7
]}

Filippenko, A. V. ^{[8
]}

Li, W. ^{[8
]}

Arcavi, I. ^{[1
]}

Cenko, S. B. ^{[8
]}

Fox, D. B. ^{[9
]}

Leonard, D. C. ^{[10
]}

Moon, D. -S. ^{[11
]}

Sand, D. J. ^{[2
,12
]}

Soderberg, A. M. ^{[2
]}

Anderson, J. P. ^{[13
,14
]}

James, P. A. ^{[14
]}

Foley, R. J. ^{[2
]}

Ganeshalingam, M. ^{[8
]}

Ofek, E. O. ^{[15
]}

Bildsten, L. ^{[16
,17
]}

Nelemans, G. ^{[18
]}

Shen, K. J. ^{[16
]}

Weinberg, N. N. ^{[8
]}

Metzger, B. D. ^{[8
]}

Piro, A. L. ^{[8
]}

Quataert, E. ^{[8
]}

Kiewe, M. ^{[1
]}

Poznanski, D. ^{[8
,19
]}

机构：

[1] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel

[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[3] Scuola Normale Super Pisa, I-56127 Pisa, Italy

[4] Max Planck Inst Astrophys, D-85748 Garching, Germany

[5] INAF Oss Astron Padova, I-35122 Padua, Italy

[6] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA

[7] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA

[8] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[9] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA

[10] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA

[11] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[12] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA

[13] Univ Chile, Dept Astron, Camino El Observ, Santiago, Chile

[14] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England

[15] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[16] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA

[17] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[18] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands

[19] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA

来源：

NATURE | 2010年 / 465卷 / 7296期

基金：

美国国家科学基金会;

关键词：

CORE-COLLAPSE SUPERNOVAE; IA SUPERNOVA; GALAXIES; MODELS; STAR; TELESCOPE;

D O I：

10.1038/nature09056

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Supernovae are thought to arise from two different physical processes. The cores of massive, short-lived stars undergo gravitational core collapse and typically eject a few solar masses during their explosion. These are thought to appear as type Ib/c and type II supernovae, and are associated with young stellar populations. In contrast, the thermonuclear detonation of a carbon-oxygen white dwarf, whose mass approaches the Chandrasekhar limit, is thought to produce type Ia supernovae(1,2). Such supernovae are observed in both young and old stellar environments. Here we report a faint type Ib supernova, SN 2005E, in the halo of the nearby isolated galaxy, NGC 1032. The 'old' environment near the supernova location, and the very low derived ejected mass (similar to 0.3 solar masses), argue strongly against a core-collapse origin. Spectroscopic observations and analysis reveal high ejecta velocities, dominated by helium-burning products, probably excluding this as a subluminous(3,4) or a regular(1) type Ia supernova. We conclude that it arises from a low-mass, old progenitor, likely to have been a helium-accreting white dwarf in a binary. The ejecta contain more calcium than observed in other types of supernovae and probably large amounts of radioactive (44)Ti.

引用

页码：322 / 325

页数：4

共 28 条

[1] Faint thermonuclear supernovae from AM Canum Venaticorum binaries [J].