| Name: | Munjiba M M |
| Affiliation: | Manipal Center for Natural Sciences, Manipal Academy of Higher Education |
| Conference ID : | ASI2024_492 |
| Title : | Study of Solar Atmospheric Heating due to Non-Flaring Active Region |
| Authors : | Munjiba M M 1, Prakhar Singh 1, Adithya H N 1, Sreejith Padinhatteeri 1, P S Athiray 2,3 |
| Authors Affiliation: | 1 Manipal Centre for Natural Sciences, Centre of Excellence, Manipal Academy of Higher Education, Manipal, Karnataka - 576104, India
2 Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, Huntsville, AL - 35899,USA
3 NASA Marshall Space Flight Center, Huntsville - 35808, USA
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| Mode of Presentation: | Poster |
| Abstract Category : | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract : | The layers of the outer atmosphere on the Sun are interconnected with one another. The magnetic field plays a crucial role in this interconnection, where various magnetic activities and features can be seen from the photosphere to the upper atmosphere, such as the chromosphere and corona. Sunspots, for instance, are a significant feature, and usually, a sunspot on the photosphere manifests as an active region in the upper atmosphere. It is well-established that many solar flares and related activities are linked to sunspots. In this study, we explore the evolution of a simpler, non-flaring sunspot (AR NOAA 13304), from May 10, 2023, to May 17, 2023, and its impact on the chromosphere and corona. We used a Helioseismic and Magnetic Imager (HMI) onboard Solar Dynamic Observatory (SDO) to study the magnetic field topology and associated properties like vertical current, Helicity, Lorentz force, magnetic free energy density etc during the sunspot's evolution. The Atmospheric Imaging Assembly (AIA) onboard SDO, and X-ray Telescope (XRT) onboard Hinode were used to study the chromospheric and coronal temperature. It is seen that the sunspot evolution makes a significant impact on the temperature and differential emission measure (DEM) at the higher solar atmospheres. |
