| Name: | Divya Oberoi |
| Affiliation: | NCRA-TIFR |
| Conference ID : | ASI2023_593 |
| Title : | Augmenting Aditya-L1 Science with High Fidelity Radio Imaging |
| Authors : | Divya Oberoi, Devojyoti Kansabanik, Soham Dey, Puja Majee (NCRA-TIFR)
Atul Mohan (RoCS, Univ. of Oslo, Finland)
Surajit Mondal (NJIT, USA)
Rohit Sharma (FHNW, Switzerland) |
| Mode of Presentation: | Oral |
| Abstract Category : | Sun and the Solar System |
| Abstract : | Solar radio imaging observations offer a wide variety of complementary information to what can be gleaned. While this has been amply demonstrated, instrumental and algorithmic limitations on the one hand, and the steep learning curve which needs to be negotiated in absence of suitable analysis tools, have severely limited the use of radio imaging observations in the larger community. Many new generation radio interferometers, especially the precursors for the Square Kilometer Array (SKA), now provide data well matched to the needs of solar science. We have developed algorithms and their robust implementations to build robust end-to-end interferometric imaging pipelines which deliver state-of-the-art spectro-polarimetric snapshot imaging. These pipelines have been designed with a non-specialist user in mind and we aspire to make them public. At the low radio frequencies, where we have focused thus far, these capabilities have been convincingly demonstrated in a large number of publications using data from the Murchison Widefield Array (MWA) spanning the 80-300 MHz part of the band. The dynamic range of these images and their polarisation purity is unprecedented. Here we highlight the various different ways in which radio imaging observations can enrich and augment the science being envisaged from Aditya-L1, scheduled for launch in 2023. Examples range from coronal magnetography at a range of coronal heights; estimating magnetic fields entrained in the coronal mass ejection (CME) plasma from a few to many tens of solar radii; exploring spatial-temporal evolution of particle acceleration processes during active phenomenon and understanding coronal turbulence via studying radio propagation effects. We will also briefly touch upon our plans to extend our work to higher frequencies using the MeerKAT which offers a frequency range from 580 MHz to 1670 MHz. Together these instruments allow us to probe the solar corona from just above the transition region to high coronal heights. |
