Gauribidanur Low-Frequency Solar Spectrograph

Abstract

A new radio spectrograph, dedicated to observe the Sun, has been recently commissioned by the Indian Institute of Astrophysics (IIA) at the Gauribidanur Radio Observatory, about 100 km North of Bangalore. The instrument, called the Gauribidanur Lowfrequency Solar Spectrograph (GLOSS), operates in the frequency range ≈ 40 -440 MHz. Radio emission in this frequency range originates close to the Sun, typically in the radial distance range r ≈ 1.1 -2.0 R . This article describes the characteristics of the GLOSS and the first results. (UK). SOHO is a project of international cooperation between ESA and NASA. The SOHO-LASCO CME catalog is generated and maintained at the CDAW Data Center by NASA and the Catholic University of America in cooperation with the Naval Research Laboratory. The SDO/AIA data are courtesy of the NASA/SDO and the AIA science teams. We are grateful to the referee for his/her comments, which helped us to bring out the results more clearly.

Low‐Frequency Radio Observations of the “Quiet” Corona During the Descending Phase of Sunspot Cycle 24

“…So, even when the Sun is at −23° decl., its elevation for GRAPH would be high (≈53°). For radio spectral data, we used observations with the Gauribidanur LOw‐frequency Solar Spectrograph (GLOSS; Ebenezer et al, 2001, 2007; Hariharan et al, 2016; Kishore et al, 2014), Gauribidanur RAdio Spectro‐Polarimeter (GRASP; Hariharan et al, 2015; Kishore et al, 2015; Sasikumar Raja et al, 2013), and e‐CALLISTO (Benz et al, 2009; Monstein et al, 2007). We also used data obtained with the Gauribidanur Radio Interferometric Polarimeter (GRIP; Ramesh et al, 2008).…”

Automated Detection of Solar Radio Bursts Using a Statistical Method

“…Since then, so far > 150 stations are installed around the globe as previously mentioned. Most of the stations use the log-periodic dipole antenna (LPDA) as the primary receiving element (see for example Kishore et al (2014);Sasikumar Raja et al (2013a)). The e-CALLISTO receiver is designed to operate over the bandwidth 45-870 MHz.…”

An Estimate of the Magnetic Field Strength Associated With a Solar Coronal Mass Ejection From Low Frequency Radio Observations

“…The radio data were obtained on 2013 March 15 at 80 MHz with the Gauribidanur RAdioheliograPH (GRAPH; Ramesh et al 1998;Ramesh et al 1999aRamesh et al ,b, 2006a in the imaging mode, the Gauribidanur Radio Interference Polarimeter (GRIP; Ramesh et al 2008) at 80 MHz and 40 MHz in the transit mode, and over the 85 -35 MHz band with the Gauribidanur LOw frequency Solar Spectrograph (GLOSS; Ebenezer et al 2001;Ebenezer et al 2007;Kishore et al 2014) in the spectral mode. All the aforementioned instruments are located in the Gauribidanur radio observatory 1 , about 100 km north of Bangalore in India (Ramesh 2011a source region in the solar atmosphere, is presently difficult to detect at low radio frequencies because of the differential Faraday rotation of the plane of polarization within the typical observing bandwidths (Grognard & McLean 1973).…”