Primarily I work in Radio Instrumentation and Observational Solar Radio Astrophysics. I am interested in building/developing radio telescopes and related instruments to observe the Solar Corona and other celestial objects at low-frequencies. 

 

During Ph.D.: I involved in building the radio interferometric polarimeter (Gauribidanur Radio Interferometric Polarimeter, GRIP) at Gauribidanur Observatory, operated by Indian Institute of Astrophysics and Raman Research Institute located 100 km north of Bangalore, India. After the successful installation of GRIP, we carried out the observations of the solar corona every day along with the other celestial sources for calibration. The data analysis of the polarimetric data have been carried out.

 

I also involved in designing and developing the Cross-polarized log-periodic dipole antenna and build a simple two-element radio interferometric polarimeter. We observed the noise storms using the developed system in Stokes I and V.

 

We recently installed a Callisto spectrometer at IISER Pune and carrying out the observations of the Sun every day since September 2015. The radio spectrometer is a part of an e-CALLISTO network which is a worldwide network to monitor the radio emissions/bursts 24 hours in a day.

 

 

Basically, I work on different radio bursts: Noise storms or Type I bursts, fast drifting Type III bursts, Broadband Type IV continuum bursts. Mainly I am interested in the polarization properties of these bursts and therefore magnetic field measurements in the solar corona. At present, there are no direct methods to estimate the magnetic field strength in the inner solar corona. But magnetic field is a crucial parameter in solving many mysteries of the solar physics.

 

Density turbulence in the solar corona and solar wind:

At IISER Pune, I study the density turbulence in the solar corona and solar wind using angular broadening observations. When the point-like radio sources observed through a solar wind/ corona, it experiences angular broadening and decrease in flux density. Using these observed quantities we measure the structure function and therefore the amplitude of density turbulence and density modulation index. We recently study how these quantities change with heliocentric distance and solar cycle. We use the data obtained using Gauribidanur Radioheliograph, Gaint Meter wave Radio Telescope, and Very Large Array.