BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Investigation of Astrophysical Sources\, Including the Sun\, via R adio Interferometry Using AX-Offset D90 Antennas DTSTART;VALUE=DATE-TIME:20261027T162500Z DTEND;VALUE=DATE-TIME:20261027T163000Z DTSTAMP;VALUE=DATE-TIME:20261023T152622Z UID:indico-contribution-6507@cern.ch DESCRIPTION:Speakers: Irene . Arkhangelskaja (NRNU MEPhI)\nExtreme energy release in astrophysical sources\, including the Sun\, is associated with the acceleration and interaction of elementary particles—specifically\, with the conversion of magnetic field energy. Consequently\, the systemati c study of radio emission from these sources with high angular resolution makes it possible to identify the mechanisms of particle acceleration\, pl asma heating during flares\, and energy transport processes. \nThis paper discusses the use of offset-focus parabolic mesh antennas (AX-Offset D90) to create the MEPhIst radio interferometer prototype and the scientific in strument itself. The MEPhIst radio interferometer will be based on two spa rse-aperture antenna arrays with maximum baseline lengths of l1max ≈ 49 m and l2max ≈ 61 m. Each antenna field consists of two arrays with a spe cial configuration and comprises up to 46 and 79 individual antenna elemen ts (Main Antenna Modules—MAMs\, based on the AX-Offset D90 antenna)\, re spectively\; the overall system dimensions are ~ 450 m\, which will provid e an angular resolution ranging from ~0.12° to $5.70·10-3° in the frequ ency range of 0.3000–6.5000 GHz. The prototype system will also consist of two arms\; however\, each will comprise a T-shaped array of five MAM mo dules with an initial maximum baseline of l0 ≈ 30 m\, which can be exten ded to l01max ≈ 53 m and l02max ≈ 54 m\, respectively. This configurat ion simplifies the development of techniques for image reconstruction and object coordinate determination. The low weight and compact dimensions of each individual antenna module—based on the AX-Offset D90 design—will allow the system's antenna arrays to be mounted on the roofs of MEPhI buil dings using surface-laid cable runs\; this will significantly reduce equip ment costs compared to interferometers based on traditional parabolic ante nnas (which require underground cabling due to the substantial mass and si ze of individual antenna units). \nA prototype antenna module is currently being developed and assembled at the Department of Experimental Nuclear P hysics and Cosmophysics at NRNU MEPhI. Preliminary calibration has been pe rformed at a frequency of 1.0009 ± 0.0001 GHz\, and an increase in the re ceived signal level has been demonstrated when pointing the antenna at the Sun. \nOne of the primary scientific objectives of the MEPhIst radio inte rferometer will be to study the radio emission from both solar flares and the "quiet" Sun\; this will enable further research into electron accelera tion mechanisms\, plasma heating during flares\, and energy transport proc esses\, as well as the detection and study of shock waves and the evolutio n of large-scale structures in the solar atmosphere. Another application o f the facility will be the development of methods for monitoring solar act ivity in the radio range—specifically\, continuing the comparative analy sis of geomagnetic events identified using various indices. \nThe MEPhIst radio interferometer can be used for Galactic research\, including the stu dy of the discrete radio source Sgr A\, the Galactic radio halo\, and neut ral hydrogen clouds (HI line)\, as well as discrete sources and distributi ons in the HII (1415 MHz)\, H3 (1517 MHz)\, Na23 (1772 MHz)\, Al27 (1506 M Hz)\, and OHI (1666 MHz) lines\, among others\; it also enables the analys is of emission properties in recombination lines. \nOne of the primary obj ectives of the MEPhIst scientific facility will be to study the properties of transient sources both within our Galaxy and beyond: investigating rad io pulsar period variations (including those located in the Galactic halo) \, examining the characteristics of non-stationary radio emission from mag netars\, and studying radio bursts that fall within the instrument's field of view. Furthermore\, the instrument allows for the study of emission ch aracteristics in the neutral hydrogen (HI) spectral line at various redshi fts\, making it possible to establish the principles of the Gal_z scale— an initiative aimed at resolving the discrepancy in Hubble constant (H0) v alues\, which is a key challenge in modern cosmology. This unique new scal e will be employed for the first time\, complementing existing scales base d on data from supernovae (SN) and the cosmic microwave background (CMB).\ n\nhttps://indico.particle.mephi.ru/event/626/contributions/6507/ LOCATION:Sevastopol hotel Conference Hall 1 URL:https://indico.particle.mephi.ru/event/626/contributions/6507/ END:VEVENT END:VCALENDAR