Table 3.

Final Model Parameters

Parameter	SA0	SA50	SA100
D0,xx [1028 cm2 s−1]a	4.37	4.47	4.71
δ a	0.494	0.508	0.483
νA[km s−1]	7.64	9.19	7.34
γ 0 b	1.47	1.61	1.66
γ 1 b	2.366	2.350	2.381
R1 [GV]b	3.64	3.92	4.12
γ 0,H	1.74	1.78	1.74
γ 1,H b	2.350	2.342	2.351
γ 2,H b	2.178	2.206	2.207
R1,H [GV]b	5.78	6.18	5.62
R2,H [GV]b	304	226	332
ΔHe	0.026	0.018	0.017
γ 0,e b	1.63	1.66	1.61
γ 1,e b	2.765	2.756	2.756
γ 2,e b	2.378	2.332	2.329
R1,e [GV]b	5.95	6.18	6.06
R2,e[GV]b	103	120	100
Jp [10−9 cm−2 s−1 sr−1 MeV−1]c	4.598	4.562	4.599
Je [10−11 cm−2 s−1 sr−1 MeV−1]c	1.221	1.209	1.250
q0,4He/q0,p × 10−6d	93892	94157	93416
q0,12C/q0,p × 10−6d	2882	2867	2746
q0,16O/q0,p × 10−6d	3780	3873	3645
q0,20Ne/q0,p × 10−6d	356	358	333
q0,24Mg/q0,p × 10−6d	644	654	609
q0,28Si/q0,p × 10−6d	742	762	718
ΦHEAO3–C2 [MV]e	857	849	827
ΦPAMELA [MV]e	578	578	572
ΦAMS [MV]e	610	640	594

Notes.

^aD(R) ∝ βR^δ; D(R) is normalized to D₀ at 4 GV.

^bThe injection spectrum is parameterized as $q(R)\propto R_0^{\gamma }$ for R < R₁ q(R) ∝ R^γ1 for R₁ < R < R₂, and q(r) ∝ R^γ2 for R > R₂. The spectral shape of the injection spectrum is the same for all species except H.

^cThe proton and e⁻ flux is normalized at the solar location at a kinetic energy of 100 GeV.

^dThe injection spectra for isotopes are adjusted as a ratio of the proton injection spectrum at 100 GeV. The isotopes not listed here have the same value as that found in Jóhannesson et al. (2016).

^eThe force-field approximation is used for the solar modulation of CRs. The modulation potential is assumed to be dependent only on the time and location of the observations.