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Probing the morphology of polarized emission induced by fluctuation dynamo using minkowski functionals

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dc.contributor.author Dutta, Riju
dc.contributor.author Sur, Sharanya
dc.contributor.author Basu, Aritra
dc.date.accessioned 2024-12-17T06:35:28Z
dc.date.available 2024-12-17T06:35:28Z
dc.date.issued 2024-12-01
dc.identifier.citation The Astrophysical Journal, Vol. 976, No. 2, 168 en_US
dc.identifier.issn 1538-4357
dc.identifier.uri http://hdl.handle.net/2248/8618
dc.description Open Access en_US
dc.description Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI
dc.description.abstract The morphology and the characteristic scale of polarized structures provide crucial insights into the mechanisms that drive turbulence and maintain magnetic fields in magneto-ionic plasma. We aim to establish the efficacy of Minkowski functionals as quantitative statistical probes of filamentary morphology of polarized synchrotron emission resulting from fluctuation dynamo action. Using synthetic observations generated from magnetohydrodynamic simulations of fluctuation dynamos with varying driving scales (ℓ f) of turbulence in isothermal, incompressible, and subsonic media, we study the relation between different morphological measures and their connection to fractional polarization (p f). We find that Faraday depolarization at low frequencies gives rise to small-scale polarized structures that have higher filamentarity as compared to the intrinsic structures that are comparable to ℓ f. Above ∼3 GHz, the number of connected polarized structures per unit area (N CC,peak) is related to the mean p f (<p f>) of the emitting region as <pf>∝NCC,peak‑1/4 , provided the scale of the detectable emitting region is larger than ℓ f. This implies that N CC,peak represents the number of turbulent cells projected on the plane of the sky and can be directly used to infer ℓ f via the relation ℓf∝NCC,peak‑1/2 . An estimate of ℓ f thus directly allows for pinning down the turbulence-driving mechanism in astrophysical systems. While the simulated conditions are mostly prevalent in the intracluster medium of galaxy clusters, the qualitative morphological features are also applicable in the context of interstellar medium in galaxies. en_US
dc.language.iso en en_US
dc.publisher American Astronomical Society en_US
dc.relation.uri https://doi.org/10.3847/1538-4357/ad891c
dc.rights © 2024. The Author(s).
dc.subject Magnetohydrodynamics en_US
dc.subject Magnetohydrodynamical simulations en_US
dc.subject Magnetic fields en_US
dc.subject Galaxy clusters en_US
dc.subject Intracluster medium en_US
dc.subject Radio astronomy en_US
dc.subject Spectropolarimetry en_US
dc.title Probing the morphology of polarized emission induced by fluctuation dynamo using minkowski functionals en_US
dc.type Article en_US


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