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Solar Activity Observed with the New Nobeyama Radioheliograph

Published online by Cambridge University Press:  12 April 2016

Shinzo Enome ,
Hiroshi Nakajima ,
Kiyoto Shibasaki ,
Masanori Nishio ,
Toshiaki Takano ,
Yoichiro Hanaoka ,
Chikayoshi Torii ,
Hideaki Sekiguchi ,
Susumu Kawashima  and
Takeshi Bushimata
...Show all authors
Shinzo Enome
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Hiroshi Nakajima
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Kiyoto Shibasaki
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Masanori Nishio
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Toshiaki Takano
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Yoichiro Hanaoka
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Chikayoshi Torii
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Hideaki Sekiguchi
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Susumu Kawashima
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Takeshi Bushimata
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Noriyuki Shinohara
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Yoshihisa Irimajiri
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Hideki Koshiishi
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Takeo Kosugi
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Yasuhiko Shiomi
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Masaki Sawa
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan
Keizo Kai
Affiliation:
Nobeyama Radio Observatory Minamisaku, Nagano, 384-13Japan

Abstract

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The new Nobeyama Radioheliograph was completed in March 1992 after two years of construction. It is a T-shaped array operating as a multiple spacing grating-type radio interferometer at 17 GHz and is dedicated to full disk solar observations. Routine observations began in late June, 1992, after three months of system integration, fine tuning, and test observations. During the course of test observations it was shown that major items of the system performance exceeded the designed values, and that the image quality or the dynamic range of the images is better than the designed value. In the three months of routine observations two X-class flares, several M-class flares and a number of small flares were observed. In this report we present a summary of initial observational results and preliminary comparisons with YOHKOH HXT and SXT observations.

Type
Session 5. Fields in the Chromosphere and Corona
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 310 - 320
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

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