Speaker
Description
Energetically weak bursts contribute most to the solar plasma heating. However, they are difficult to image accurately due to the thermal background from the active region. Broadly, we can distinguish the emission from radio bursts consisting of slowly varying components and transient burst components. To characterise the burst component, we must take out the slowly varying components by subtracting the visibilities of quiet times. For the observations of bursts spanning several hours, removing one static component is too simplistic as the active region's background emission changes in many hours. In this work, we subtract a visibility continuum that quantifies the slowly varying component. This is done by identifying several quiet periods within the observations, later fitting it with an appropriate degree of the polynomial. The residual visibility dataset can be used to image transient burst components and characterise their strength, location and occurrence. By employing this method for an MWA dataset, we have been able to image transient emission up to 10^4 K brightness temperatures.
