| Name: | Tariq Ahmad Mir |
| Affiliation: | Bhabha Atomic Research Centre |
| Conference ID: | ASI2025_651 |
| Title: | Significant first digit distribution of Coronal Mass Ejections characteristics |
| Authors: | T. A. Mir, M. Ausloos, M. A. Darzi, P. M. Ishtiaq |
| Authors Affiliation: | T. A. Mir, M. A. Darzi, P. M. Ishtiaq
Nuclear Research Laboratory, Astrophysical Sciences Division,
Bhabha Atomic Research Centre, Srinagar-190024, Jammu and Kashmir, India
M. Ausloos
1. GRAPES,
rue de la Belle Jardiniere 483, B-4031, Angleur, Belgium
1. School of Business, University of Leicester, Brookfield,
Leicester, LE2 1RQ, UK.
3. Uniiversitatea Babe-Bolyai,
Str. Mihail Kogniceanu nr. 1, 400084, Cluj-Napoca, Romania
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| Mode of Presentation: | Oral |
| Abstract Category: | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract: | Benford's Law (BL) is an interesting empirical phenomenon that describes how the first significant digits (FSDs) of many real-world datasets are distributed. Specifically, it states that in a wide range of data, smaller digits—like 1, 2, and 3—appear as the FSDs much more frequently than larger digits, such as 7, 8, and 9. Massive data collected from the observation of different astrophysical phenomena can provide new testing grounds for the ubiquity of this law. In this investigation, we systematically analyze the distribution of FSDs for various characteristics of Coronal Mass Ejections (CMEs) to assess the relevance of BL. The parameters examined include width, mass, acceleration, momentum, force, and kinetic energy, all of which conform to the expected FSD distribution as prescribed by BL. In contrast, the central position angle, measurement position angle, and speeds of the CMEs exhibit significant deviations from this law. These results indicate that while certain CME characteristics adhere to the principles of BL, others reveal substantial departures, thereby revealing the intricate complexities inherent in the numerical distributions of astrophysical phenomena. The deviations observed in above parameters may indicate complexities in the physical mechanisms at play, such as variations in solar magnetic field interactions or differences in the spatial and temporal dynamics of CMEs. By further exploring these discrepancies, we can gain deeper insights into the intricate processes that drive solar activity.
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