Multi beam observations of cosmic radio noise using a VHF radar with beam forming by a Butler matrix

• Published in: Advances in Radio Science
• Main Authors: Renkwitz, T., Singer, W., Latteck, R., Rapp, M.
• Format: Article in Journal/Newspaper
• Language: English
• Published: Copernicus Publications 2011
• Subjects: article; Verlagsveröffentlichung; Alomar; Andøya; Saura
• Online Access: https://doi.org/10.5194/ars-9-349-2011; https://noa.gwlb.de/receive/cop_mods_00027086; https://noa.gwlb.de/servlets/MCRFileNodeServlet/cop_derivate_00027041/ars-9-349-2011.pdf; https://ars.copernicus.org/articles/9/349/2011/ars-9-349-2011.pdf

The Leibniz-Institute of Atmospheric Physics (IAP) in Kühlungsborn started to install a new MST radar on the North-Norwegian island Andøya (69.30° N, 16.04° E) in 2009. The new Middle Atmosphere Alomar Radar System (MAARSY) replaces the previous ALWIN radar which has been successfully operated for more than 10 years. The MAARSY radar provides increased temporal and spatial resolution combined with a flexible sequential point-to-point steering of the radar beam. To increase the spatiotemporal resolution of the observations a 16-port Butler matrix has been built and implemented to the radar. In conjunction with 64 Yagi antennas of the former ALWIN antenna array the Butler matrix simultaneously provides 16 individual beams. The beam forming capability of the Butler matrix arrangement has been verified observing the galactic cosmic radio noise of the supernova remnant Cassiopeia A. Furthermore, this multi beam configuration has been used in passive experiments to estimate the cosmic noise absorption at 53.5 MHz during events of enhanced solar and geomagnetic activity as indicators for enhanced ionization at altitudes below 90 km. These observations are well correlated with simultaneous observations of corresponding beams of the co-located imaging riometer AIRIS (69.14° N, 16.02° E) at 38.2 MHz. In addition, enhanced cosmic noise absorption goes along with enhanced electron densities at altitudes below about 90 km as observed with the co-located Saura MF radar using differential absorption and differential phase measurements.