Table 1.

Spectral and Other Selected Parameters for the Most Intense Planetary Energetic Ion Spectra in the Solar System

Planet(Hot Ion)	L	E Low(keV)	C	kT	γ1	Eo	γ2a	γ2b	BD(nT)c	BetaDd	Elec. Den.(1/cc)	CRMe	ErM keVf	Comment
E(H+)	3.0	5	6.54E6	∽0	0.308	77.6	1	1.69	1152	0.123	1100	2.5	38	E×p45; [Lyons and Williams, 1980]
E(H+)	3.5	5	2.41E7	∽0	0.779	223	3.12	1	725	0.265	700	4.1	45	E×p45; [Lyons and Williams, 1980]
E(H+)	4.0	5	4.00E6	∽0	0.244	89.0	4.01	1	486	0.350	350	4.4	48	E×p45; [Lyons and Williams, 1980]
E(H+)	4.0	5	7.66E6	∽0	0.428	4944	1	41.25	486	0.419	350	3.6	45	E×p45; [Lyons and Williams, 1980]
E(H+)	5.0	5	2.67E6	∽0	0.269	87.3	5.74	1	249	0.752	130	3.1	45	E×p45; [Williams and Lyons, 1974b]
E(H+)a	4.0	1	3.12E19	23.2	5.548	.0011	0.018	1	486	0.184	350	2.0	57	CCE; [Krimigis et al., 1985]
E(O+)b	4.0	10	1.33E22	22.7	6.638	1.39	0.614	1	486	0.078	350	0.359	139	CCE; [Krimigis et al., 1985]
J(H+)	9.51	20	4.05E7	30.9	1.62	5660	2.534	1	490	0.017	120	0.93	189	Gal; [Mauk et al., 2004]
J(H+)	7.1	20	3.50E6	847	0.859	2383	3.10	1	1173	0.0097	900	1.00	1030	Gal; [Mauk et al., 2004]
J(S+)	9.51	80	1.60E8	17.2	1.91	4948	2.21	1	490	0.068	120	1.16	23	Gal; [Mauk et al., 2004]
J(S+)	7.1	80	1.49E11	440	2.44	8408	0.844	1	1173	0.013	900	0.051	538	Gal; [Mauk et al., 2004]
J(O/S+)	7.4	100	2.74E4	0	0.276	2821	4.36	1	1036	0.123	640	1.20	267	Voy; [Mauk et al., 1996]
S(H+)	8.4	30	8.86E11	36.5	3.65	382	1.39	1	33.7	0.064	10	0.027	65	Cassini; This work
S(H+)	9.5	30	6.80E11	17.4	3.79	653	2.95	1	23.3	0.315	6	0.087	31	Cassini; This work
S(W+)	9.5	10	3.96E6	1.75	2.36	165	27.7	1	23.3	0.231	6	0.032	47	Cassini; This work
U(H+)	6.5	40	5.81E5	4.95	1.445	1210	4.63	1	26.8	0.280	1	0.050	49	Voy; [Mauk et al., 1987]
N(H+)	9.4	30	1.51E15	30.6	5.15	NA	NA	NA	16.9	0.070	0.1	0.007	79	Voy; [Mauk et al., 1995]

^aThis is a poor fit. It uses only the peaks of very structured proton spectra.

^bThis spectrum also has some unmodeled structure, but the fit is accurate to a factor of 2 everywhere.

^cDipole magnetic field strength at the magnetic equator at the designated L value.

^dRatio of the integrated particle pressure for the designated spectrum, normalized by the dipole magnetic pressure.

^eCRM is the maximum value of the C_m/C_K versus E_r profile.

^fERM is the value of the resonant energy E_r at which CRM occurs.