A5028130526- Solar and Space Plasma Dynamics
- Ionosphere and magnetosphere dynamics
- Astro and Planetary Science
- Atmospheric Ozone and Climate
- Stellar, planetary, and galactic studies
- Geomagnetism and Paleomagnetism Studies
- Adaptive optics and wavefront sensing
- Astronomy and Astrophysical Research
- Solar Radiation and Photovoltaics
- Calibration and Measurement Techniques
- Astronomical Observations and Instrumentation
University of Catania
2022-2023
Indian Institute of Astrophysics
2014-2022
Osservatorio Astrofisico di Catania
2022
Bangalore University
2016-2019
Using the HMI/SDO vector magnetic field observations, we studied relation of degree non-potentiality with observed flare/CME in active regions. From a sample 77 cases, found general that is positively correlated flare strength and associated CME speeds. Since flux flare-ribbon area more related to reconnection, trace strong gradient polarity inversion line (SGPIL), Schrijver's R value manually along extent. Manually detected SGPIL length values show higher correlation speed than...
This paper presents the project Comprehensive spAce wEather Studies for ASPIS prototype Realization (CAESAR), which aims to tackle relevant aspects of Space Weather (SWE) science and develop a scientific data centre Italian Agency (ASI) called (ASI SPace InfraStructure). To this end, CAESAR involves majority SWE community, bringing together 10 institutions as partners, total 92 researchers. The approach encompasses whole chain phenomena from Sun Earth up planetary environments in...
The background field is assumed to play prime role in the erupting structures like prominences. In flux rope models, critical decay index ($n_c$) a measure of rate at which intensity decreases with height over or structure. real observations, unknown, so typical value $n_{c}=1.5$ adopted from numerical studies. this study, we determined $n_c$ 10 prominence eruptions (PEs). 3D derived two-perspective observations \textit{Solar Dynamics Observatory} and TErrestrial RElations Observatory}....
Abstract Using the observations from Solar Dynamics Observatory, we study an eruption of a hot-channel flux rope (FR) near solar limb on 2015 February 9. The pre-eruptive structure is visible mainly in EUV 131 Å images, with two highly sheared loop structures. They undergo slow rising motion and then reconnect to form eruptive hot channel, as tether-cutting reconnection model. J-shaped flare ribbons trace footpoint FR that identified channel. Initially, channel observed rise slowly at 40 km...
The non-association of coronal mass ejections with high energetic flares is sparse. For this reason, the magnetic conditions required for confinedness major a topic active research. Using multi-instrument observations, we investigated evolution and effects in an X3.1 flare, which occurred region (AR) 12192. decrease net fluxes brightening regions, near footpoints multi-sigmoidal AR photosphere chromosphere, indicative flux cancellation favouring tether-cutting reconnection (TCR), observed...
Abstract Using observations from the Solar Dynamics Observatory , we studied an interesting example of a sigmoid formation and eruption small-scale flux-canceling regions active region (AR) 11942. Through analysis Helioseismic Magnetic Imager Atmospheric Imaging Assembly infer that initially AR is compact bipolar in nature, evolved to sheared configuration consisting inverse J-shaped loops hosting filament channel over couple days. By tracking photospheric magnetic features, shearing...
The abrupt and permanent changes of photospheric magnetic field in the localized regions active during solar flares called imprints (MIs), have been observed for past nearly three decades. well known "coronal implosion" model is assumed to explain such flare associated but complete physical understanding still missing debatable. In this study, we made a systematic analysis flare-related 21 (14 eruptive 7 non-eruptive) using high-cadence (\texttt{135s}) vector-magnetogram data obtained from...