Monte Carlo modelling of the propagation and annihilation of nucleosynthesis positrons in the Galaxy

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Table 4

Annihilation phase fractions for ²⁶Al, ⁴⁴Ti, and ⁵⁶Ni positrons, using the random ISM model.

Source	SN Ia escape	halo GMF	Disk ISM phases					Bulge ISM phases					Sgr A* region
	fraction (%)	configuration	MM	CNM	WNM	WIM	HIM		MM	CNM	WNM	WIM	HIM	IRH

²⁶Al	N/A	N	3.3	25.8	33.4	25.4	0.0		3.6	1.1	1.2	3.9	0.0	0.0
		D	3.1	25.1	32.6	24.7	0.0		3.9	0.9	1.1	2.8	0.0	1.5
		X	3.0	25.1	32.5	24.6	0.0		2.5	0.8	0.8	3.4	0.0	0.0

⁴⁴Ti	N/A	N	4.1	26.0	32.4	24.7	0.0		4.0	1.1	1.0	3.5	0.0	0.0
		D	4.1	25.3	31.2	23.8	0.0		4.5	0.9	0.8	2.4	0.0	1.4
		X	3.9	25.1	31.2	23.4	0.0		2.7	0.8	0.6	2.6	0.0	0.0

⁵⁶Ni	5%	N	1.8	21.3	34.1	29.3	0.0		0.8	0.6	0.7	8.4	0.0	0.0
		D	1.9	20.7	33.6	28.2	0.0		1.8	0.7	1.2	7.4	0.0	0.8
		X	1.6	20.2	32.7	27.4	0.0		0.6	0.4	0.4	6.1	0.0	0.0

⁵⁶Ni+⁴⁴Ti+²⁶Al	5%	N	2.4	22.6	33.7	28.1	0.0		1.7	0.8	0.8	7.0	0.0	0.0
		D	2.4	22.1	33.1	27.0	0.0		2.5	0.8	1.1	6.0	0.0	1.0
		X	2.2	21.7	32.5	26.4	0.0		1.2	0.5	0.5	5.2	0.0	0.0

Notes. In the third column, N, D, and X stand for no halo field, dipole field, and X-shape field, respectively. The annihilation phase fractions are then given in % for the Galactic disk, the Galactic bulge, and the Sgr A* region. For the last region, only the annihilation fraction in the ionised radio halo (IRH) is given because the annihilation fractions in the other ISM components of the Sgr A* region are negligible. The sum was done over | z | ≤ 1.5 kpc, so totals may differ slightly from 100%.

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