Constraining the Properties of SNe~Ia Progenitors from Light Curves

Дата и время публикации : 2011-09-16T14:25:43Z

Авторы публикации и институты :
B. Sadler
P. Hoeflich
E. Baron
K. Krisciunas
G. Folatelli
M. Hamuy
M. Khokhlov. M. Phillips
N. Suntzeff
L. Wang

Ссылка на журнал-издание: in: ‘Binary Path to Type Ia Supernova Explosions, Proceedings of the IAU 281, eds. DiStephano & M. Orio, Cambridge University Press (2012)
Коментарии к cтатье: 4 pages & 4 figures
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO,

Краткий обзор статьи: We present an analysis of high precision V light curves (LC) for 18 local Type Ia Supernovae, SNe Ia, as obtained with the same telescope and setup at the Las Campanas Observatory (LCO). This homogeneity provides an intrinsic accuracy a few hundreds of a magnitude both with respect to individual LCs and between different objects. Based on the Single Degenerate Scenario, SD, we identify patterns which have been predicted by model calculations as signatures of the progenitor and accretion rate which change the explosion energy and the amount of electron capture, respectively. Using these templates as principle components and the overdetermined system of SN pairs, we reconstruct the properties of progenitors and progenitor systems. All LCO SNe Ia follow the brightness decline relation but 2001ay. After subtraction of the two components, the remaining scatter is reduced to 0.01-0.03m. Type SNe Ia seem to originate from progenitors with Main Sequence masses of 3Mo with the exception of two subluminous SNe Ia with < 2Mo. The component analysis indicates a wide range of accretion rates in the progenitor systems closing the gap to accretion induced collapses (AIC). SN1991t-like objects show differences in $dm15$ but no tracers of our secondary parameters. This may point to a different origin such as DD-Scenario or the Pulsating Delayed Detonations. SN2001ay does not follow the decline relation. It can be understood in the framework of C-rich WDs, and this group may produce an anti-Phillips relation. We suggest that this may be a result of a common envelope phase and mixing during central He burning as in SN1987A.

Category: Physics