Abstract
During the several months in 1967 when solar emission was measured in the band 270 to 1310 A by instrumentation aboard the Oso 3 satellite, numerous flare-associated EUV bursts were observed. These provided the first EUV burst data for direct compraison with microwave radio bursts. Comparison of 44 of these events wtih radio bursts observed at the Sagamore Hill Radio Observatory of AFCRL has been made; excellent agreement in the start time and time of burst maximum is found in most instances. On the basis of the burst morphology it is suggested that, as with the microwave burst, different mechanisms are responsible for the impulsive first component and slow burst decay time (second component).
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
