Investigations on Type III/V Bursts of Solar Radio Emission. Part I: Phenomenology and Properties of Type V Bursts

✍ Scribed by H. Daene; A. KrüGER

• Publisher: John Wiley and Sons
• Year: 2007
• Tongue: English
• Weight: 922 KB
• Volume: 289
• Category: Article
• ISSN: 0004-6337
• DOI: 10.1002/asna.19662890302

✦ Synopsis

With 13 figurcs. (Keccived 1965 July 15) Thc phenomenological features of type V radiation arc discussed a t the basis of fine structure rccords taken a t the Astrophysical Observatory Potsdam since 1958. A phenomenological subclassification is derived from the various forms of appearance. It is believed that significant qualities are only the longer duration than that of normal type 111 bursts and the fact that nearly always a type 111 burst is preceding. It seems that there are no urgent reasons to consider type V emission as continuum radiation. It is assumed that no different excitation mechanism is effective for type I11 and type V. The obscrvational facts arc tentatively explainable by special assumptions about the structurc of the exciting electron stream. Additionally it is taken into consideration that the prolonged duration of type V is due to a merging process. I t is suggested that merging occurs if the same coronal area is reexcited by a second electron stream, whereas superposition occurs if different areas are excited by both the streams. Thc possibility is considered that harmonics partly contribute to the observed features.