Modeling proton and electron heating in the fast solar wind

Parker Solar Probe: Ushering a new frontier in space exploration

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Table 1

Boundary values for solar wind parameters and turbulence quantities at 0.21 au (45.15 R_⊙).

Parameters	Values	Parameters	Values
	35 008 k m² s⁻²		17 019.3 km² s⁻²
	3179.6 km² s⁻²		907.96 km² s⁻²
	−1134 km² s⁻²		−51.3 km² s⁻²
	1.1 × 10¹⁰ km³ s⁻²		1.14 × 10⁹ km³ s⁻²
	1.46 × 10⁹ km³ s⁻²		1.53 × 10⁸ km³ s⁻²
	−6.12 × 10⁹ km³ s⁻²		−1.72 × 10⁸ km³ s⁻²
U	530 km s⁻¹	n_p	75.55 cm⁻³
T_e	3 × 10⁵ K	T_p	5.15 × 10⁵ K
	60 cm⁻⁶

Notes. We assume the electron density is approximately equal to the proton density, n_e ≈ n_p. The proton thermal pressure is determined by P_p = n_pk_BT_p and the electron thermal pressure is determined by P_e = n_ek_BT_e, where k_B is Boltzmann’s constant.

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