Type III solar radioburst profiles and the associated electron energy spectra

✍ Scribed by C. C. Harvey

• Publisher: Springer
• Year: 1976
• Tongue: English
• Weight: 35 KB
• Volume: 46
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00149878

✦ Synopsis

An attempt is made to explain the observed frequency-time profiles of type III solar radiobursts in terms of a rapid plasma wave decay rate combined with the exciter model recently proposed by the author. The decay rate is assumed to be sufficiently rapid for the plasma wave energy density profile to be similar to the excitor power density time profile; this is consistent with the exciter model, the rapid decay being caused by Landau damping on the electrons of the modified high energy tail of the ambient plasma electron velocity distribution. The model is compared with radio observations by making simple assumptions about the dependence of the radio intensity upon the plasma wave energy. A comparison is made with simultaneous radio and electron observations by further assuming a simple power-law velocity distribution for the electrons at their point of ejection from the Sun.

Discussion

Gurnett: What is the justification for the form of the distribution taken? Harvey: This is the solution of the free streaming Vlasov equation neglecting diffusion. D. Smith: Neglect of the diffusion term is only good far from the Sun. Numerical calculations in progress indicate that this term is important close to the Sun.