| Name: | SAYANEE HALDAR |
| Affiliation: | CSSTEAP - SPACE AND ATMOSPHERIC SCIENCE, PHYSICAL RESEARCH LABORATORY |
| Conference ID : | ASI2024_704 |
| Title : | Ionospheric disturbances induced by consecutive solar eclipse and geomagnetic storms |
| Authors : | Sayanee Haldar1, Samadrita Basu2 |
| Authors Affiliation: | 1. Sayanee Haldar (CSSTEAP - Space and Atmospheric Sciences, Physical Research Laboratory (PRL), Ahmedabad 380009, Gujarat)
2. Samadrita Basu (CSSTEAP – Satellite Meteorology, Space Application Centre (SAC) – ISRO, Ahmedabad 380058, Gujarat) |
| Mode of Presentation: | Poster |
| Abstract Category : | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract : | On October 14, 2023, a total solar eclipse graced the equatorial region of South America. Coinciding with the culmination of the 25th solar cycle, solar activity exhibited a consistent daily uptick. By October 24th, a substantial geomagnetic storm struck Earth, followed by another robust geomagnetic disturbance on October 30th. Solar activity, exemplified by phenomena such as coronal mass ejections, triggered geomagnetic storms characterized by ionization and ionospheric heating. Solar activity, like coronal mass ejection, induces geomagnetic storm ionization and heats the ionosphere. Initially, the irradiance induced by solar eruptive activity elevates the photoionization rate within the ionosphere, with the most substantial elevation observed till F2 region. Following this, highly energetic photoelectrons proceed to augment atmospheric ionization through impact ionization mechanisms. Consequently, there is a corresponding increase in the plasma density within the ionosphere, mirroring the enhancement in irradiance caused by the mentioned geomagnetic storms. In contrast, when a solar eclipse occurs on Earth, there is a noticeable reduction in the number of electrons that are present in the atmosphere of the planet. Having a strong magnetic field, especially in the equatorial region, significant fluctuations in the current flow can be noticed. Changes in plasma densities between two different contrasting solar events are required in order to distinguish the solar-event-induced phenomena that occur in the upper atmosphere of Earth. |
