We present a detailed case study of the type II solar radio burst occurred on 06 March 2014 using combined data analysis. It is a classical radio event consisting of type III radio burst and a following type II radio burst in the dynamic spectrum. The type II radio burst is observed between 235 – 130 MHz (120 – 60 MHz) in harmonic (fundamental) bands with the life time of 5 minutes between 09:26 – 09:31 UT. The estimated speed of type II burst by applying two-fold Saito model is ∼ 650 km/s. An extreme ultraviolet (EUV) wave is observed with Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The very close temporal onset association of the EUV wave and flare energy release indicates that the EUV wave is likely produced by a flare pressure pulse. The eruption is also accompanied by a weak coronal mass ejection (CME) observed with the coronagraphs onboard the Solar and Heliospheric Observatory (SOHO) and the twin Solar Terrestrial Relations Observatory (STEREO). The plane of sky speed of the CME was ∼ 252 km/s in the SOHO/LASCO-C2 and ∼ 280 km/s in the STEREO-B/SECCHI-COR1 images. The EUV wave has two wave fronts, one expanding radially outward and the other one moving along the flare loop arcade. The source position of the type II burst imaged by the Nançay Radio Heliograph (NRH) shows that it was associated with the outward moving EUV wave. The CME is independent of the shock wave as confirmed by the location of NRH radio sources below the CME’s leading edge. Therefore the type II radio burst is probably ignited by the flare. This study shows the possibility of EUV wave and coronal shock triggered by flare pressure pulse, generating the observed type II radio burst.

The Grubb refractor, currently located in the southwestern dome of the Cracow Observatory, is the oldest working instrument at the institute. It was manufactured in 1874 in Thomas Grubb's factory in Dublin. However, the history of this instrument at the Jagiellonian University begins much later, in 1929, when Prof. Tadeusz Banachiewicz brought this telescope to Cracow, where it became one of the main scientific instruments.
Now, celebrating the 150th anniversary of the Grubb refractor, we are entering a new era of this instrument's service to the astronomical community. Thanks to the new narrowband solar filters, it is becoming a valuable teaching tool for astronomy students. In this talk I’ll present a brief history of the Grubb refractor and show its current capabilities for solar observations.

Giant Radio Galaxies (GRGs) are home to active supermassive black holes that produce powerful bipolar radio jets, creating structures that extend over megaparsec scales. These are the largest structures in the Universe, growing up to Mpc-scales and even surpassing the size of massive galaxy clusters. Though discovered 50 years ago, significant progress in understanding GRGs has been made only in the past eight years, largely due to the advent of sensitive sky surveys and the efforts of the SAGAN project ('Search & Analysis of GRGs with Associated Nuclei').
Research continues to explore whether the immense size of GRGs is driven by their efficient AGN or the sparser environments in which they reside. The SAGAN project, initiated in 2016, has produced several research papers, including a review, discovering the largest samples of GRGs and refining our understanding of their key properties. The project has rejuvenated global interest in these giant radio sources.
This seminar will review how our understanding of GRGs has evolved with deep radio surveys like LoTSS, which have uncovered the largest and faintest GRGs. We will discuss optical-infrared data from SDSS and WISE, revealing AGN accretion properties, and millimetre-wave data from IRAM, offering insights into AGN fuelling. We will also showcase GMRT radio images revealing previously unseen low-surface-brightness structures in GRGs, enabling more precise age and magnetic field estimates. Lastly, we will demonstrate how GRGs can be used as cosmic probes of large-scale environments and magnetic fields, with key implications for understanding magnetogenesis.