NEAR REAL-TIME SOLAR OBSERVATIONS AND MODEL BASED PREDICTIONS

Corona & hot flare plasma (SDO/AIA 131 Å)
Quiet corona & transition region (SDO/AIA 171 Å)
Flaring regions of the corona (SDO/AIA 193 Å)
Line of Sight Magnetic field (SDO/HMI)
Corona (PROBA2/SWAP 174 Å)
Quiet corona & transition region (GOES SUVI 171 Å)
Hot Corona (STEREO A/SECCHI 195 Å)
GONG H-∝
Magnetic Field Lines Generated Using PFSS on HMI Map
SOHO/LASCO Coronagraph. Credit: SOHO

Note: HMI synoptic magnetic maps are updated once daily. Thus the latest coronal field map is generated using the previous day's magnetic map. The global coronal structure does not vary significantly over one day.

Utilizing a century scale calibrated in-house developed Surface Flux Transport (SFT) model the solar surface magnetic field is evolved. By forward running this model a monthly solar surface magnetic field distribution is predicted (till 2021-06-30). Last active region included in the simulation appeared on 2021-06-09. For more technical details refer to Nandy et. al. 2018, Astrophysical Journal, Vol 853, No 1 (https://doi.org/10.3847/1538-4357/aaa1eb). Using this model the coronal field is extrapolated and predicted over monthly timescales, the details of which can be found here.

Sun's activity output from a coupled solar surface flux transport and internal dynamo model. The simulation covers a century of solar cycle variations. An ensemble forecast with the coupled model indicates the expected strength and timing of solar activity cycle over the next decade. For more details refer to Bhowmik and Nandy, 2018, Nature Communications, 5209 (https://doi.org/10.1038/s41467-018-07690-0).

A simulation of the interaction of magnetized solar plasma wind with the Earth's magnetosphere depicting the formation of the magnetotail in the nightside and the bow shock on the dayside of the Earth. CESSI has developed a Star-Planet Interaction Module (CESSI-SPIM) which is utilized to understand the space enviornment of solar-system planets. For more details refer to Das et. al., 2019, Astrophysical Journal, Vol 877, pp 80 (https://doi.org/10.3847/1538-4357/ab18ad).