Statistical analysis of the interplay between interstellar magnetic fields and filaments hosting Planck Galactic cold clumps

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dc.contributor.authorAlina, D.
dc.contributor.authorRistorcelli, I.
dc.contributor.authorMontier, L.
dc.contributor.authorAbdikamalov, E.
dc.contributor.authorJuvela, M.
dc.contributor.authorFerriere, K.
dc.contributor.authorBernard, J. Ph.
dc.contributor.authorMicelotta, E. R.
dc.date.accessioned2019-12-11T05:16:53Z
dc.date.available2019-12-11T05:16:53Z
dc.date.issued2019-02
dc.descriptionhttps://academic.oup.com/mnras/article/485/2/2825/5347951en_US
dc.description.abstractWe present a statistical study of the relative orientation in the plane of the sky between interstellar magnetic fields and filaments hosting cold clumps. For the first time, we consider both the density of the environment and the density contrast between the filaments and their environment. Moreover, we geometrically distinguish between the clumps and the remaining portions of the filaments. We infer the magnetic field orientations in the filaments and in their environment from the Stokes parameters,1 assuming optically thin conditions. Thus, we analyse the relative orientations between filaments, embedded clumps, internal and background magnetic fields, depending on their environment and evolutionary stages. We recover the previously observed trend for filaments in low column density environments to be aligned parallel to the background magnetic field; however, we find that this trend is significant only for low-contrast filaments, whereas high-contrast filaments tend to be randomly orientated with respect to the background magnetic field. Filaments in high column density environments do not globally show any preferential orientation, although low-contrast filaments alone tend to have perpendicular relative orientation with respect to the background magnetic field. For a subsample of nearby filaments, for which volume densities can be derived, we find a clear transition in the relative orientation with increasing density, at nH ∼ 103 cm−3, changing from mostly parallel to mostly perpendicular in the off-clump portions of filaments and from even to bimodal in clumps. Our results confirm a strong interplay between interstellar magnetic fields and filaments during their formation and evolution.en_US
dc.identifier.citationAlina, D., Ristorcelli, I., Montier, L., Abdikamalov, E., Juvela, M., Ferrière, K., … Micelotta, E. R. (2019). Statistical analysis of the interplay between interstellar magnetic fields and filaments hostingPlanckGalactic cold clumps. Monthly Notices of the Royal Astronomical Society, 485(2), 2825–2843. https://doi.org/10.1093/mnras/stz508en_US
dc.identifier.other000474886200098
dc.identifier.urihttp://nur.nu.edu.kz/handle/123456789/4348
dc.language.isoenen_US
dc.publisherOXFORD UNIV PRESSen_US
dc.rightsAttribution-NonCommercial-ShareAlike 3.0 United States*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/3.0/us/*
dc.subjectpolarizationen_US
dc.subjectISMen_US
dc.subjectmagnetic fieldsen_US
dc.subjectPlanck Galactic cold clumpsen_US
dc.titleStatistical analysis of the interplay between interstellar magnetic fields and filaments hosting Planck Galactic cold clumpsen_US
dc.typeArticleen_US
workflow.import.sourcescience

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