Insights into thermonuclear supernovae from the incomplete Si-burning process

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Volume 550 (February 2013)

A&A, 550 (2013) A24

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Table 2

Parent species of Si-b elements at the optical and X-ray epochs.

Element	Optical epoch^a	Variation^b	X-ray epoch^c

Sc	⁴⁵Ti (0.18 s)	~	⁴⁵Ti (0.18 s)
Ti	⁴⁸Cr (21.6 h) → ⁴⁸V (16.0 d)	↑	⁴⁸Cr (21.6 h) → ⁴⁸V (16.0 d)
V	⁴⁸Cr (21.6 h) → ⁴⁸V (16.0 d)	↓	⁵¹Mn (0.05 s) → ⁵¹Cr (27.7 d)
	⁴⁹Cr (0.04 s) → ⁴⁹V (330 d)	~
	⁵¹Mn (0.05 s) → ⁵¹Cr (27.7 d)	↑
Cr	⁵²Fe (8.3 h) → ⁵²Mn (5.6 d)	↑	⁵²Fe (8.3 h) → ⁵²Mn (5.6 d)
Mn	⁵²Fe (8.3 h) → ⁵²Mn (5.6 d)	↓	⁵⁵Co (17.5 h) → ⁵⁵Fe (2.7 y)
	⁵³Fe (0.009 s) → ⁵³Mn (3.7 Myr)	~
Fe	⁵⁴Fe		⁵⁶Ni (6.1 d) → ⁵⁶Co (77 d)

Notes.

^(a)

Main contributor to the abundance of the element at the optical epoch (in parenthesis, if it is an unstable isotope, its radioactive lifetime).

^(b)

This column indicates if the contribution of a radioactive chain to the element abundance in the optical phase increases with time (↑ ), decreases (↓ ), or remains about constant (~).

^(c)

Main contributor to the abundance of the element at the X-ray epoch (in parenthesis, if it is an unstable isotope, its radioactive lifetime).

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