Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters
Primordial magnetic fields (PMFs) are possible candidates for explaining the observed magnetic fields in galaxy clusters. Two competing scenarios of primordial magnetogenesis have been discussed in the literature: inflationary and phase-transitional. We study the amplification of both large- and sma...
| Main Authors: | , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acb04d |
| _version_ | 1797695608619794432 |
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| author | Salome Mtchedlidze Paola Domínguez-Fernández Xiaolong Du Wolfram Schmidt Axel Brandenburg Jens Niemeyer Tina Kahniashvili |
| author_facet | Salome Mtchedlidze Paola Domínguez-Fernández Xiaolong Du Wolfram Schmidt Axel Brandenburg Jens Niemeyer Tina Kahniashvili |
| author_sort | Salome Mtchedlidze |
| collection | DOAJ |
| description | Primordial magnetic fields (PMFs) are possible candidates for explaining the observed magnetic fields in galaxy clusters. Two competing scenarios of primordial magnetogenesis have been discussed in the literature: inflationary and phase-transitional. We study the amplification of both large- and small-scale correlated magnetic fields, corresponding to inflation- and phase transition–generated PMFs, in a massive galaxy cluster. We employ high-resolution magnetohydrodynamic cosmological zoom-in simulations to resolve the turbulent motions in the intracluster medium. We find that the turbulent amplification is more efficient for the large-scale inflationary models, while the phase transition–generated seed fields show moderate growth. The differences between the models are imprinted on the spectral characteristics of the field (such as the amplitude and the shape of the magnetic power spectrum) and therefore also on the final correlation length. We find a one order of magnitude difference between the final strengths of the inflation- and phase transition–generated magnetic fields, and a factor of 1.5 difference between their final coherence scales. Thus, the final configuration of the magnetic field retains information about the PMF generation scenarios. Our findings have implications for future extragalactic Faraday rotation surveys with the possibility of distinguishing between different magnetogenesis scenarios. |
| first_indexed | 2024-03-12T03:14:45Z |
| format | Article |
| id | doaj.art-0ec3a2f9cb45493aa5bd82127bd81427 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:14:45Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-0ec3a2f9cb45493aa5bd82127bd814272023-09-03T14:11:17ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01944110010.3847/1538-4357/acb04dInflationary and Phase-transitional Primordial Magnetic Fields in Galaxy ClustersSalome Mtchedlidze0https://orcid.org/0000-0001-9786-8882Paola Domínguez-Fernández1https://orcid.org/0000-0001-7058-8418Xiaolong Du2https://orcid.org/0000-0003-0728-2533Wolfram Schmidt3https://orcid.org/0000-0001-5233-8087Axel Brandenburg4https://orcid.org/0000-0002-7304-021XJens Niemeyer5https://orcid.org/0000-0002-3063-4325Tina Kahniashvili6https://orcid.org/0000-0003-0217-9852School of Natural Sciences and Medicine, Ilia State University , 3-5 Cholokashvili St., 0194 Tbilisi, Georgia ; salome.mtchedlidze.1@iliauni.edu.ge; Institute for Astrophysics and Geophysics, Georg-August-Universität Göttingen , Friedrich-Hund-Platz 1, D-37077 Göttingen, Germany; E. Kharadze Georgian National Astrophysical Observatory , 47–57 Kostava St., Tbilisi 0179, GeorgiaDipartimento di Fisica e Astronomia, Universitá di Bologna , Via Gobetti 92/3, I-40121, Bologna, Italy; Hamburger Sternwarte, Universität Hamburg , Gojenbergsweg 112, D-21029 Hamburg, GermanyCarnegie Observatories , 813 Santa Barbara Street, Pasadena, CA 91101, USAHamburger Sternwarte, Universität Hamburg , Gojenbergsweg 112, D-21029 Hamburg, GermanySchool of Natural Sciences and Medicine, Ilia State University , 3-5 Cholokashvili St., 0194 Tbilisi, Georgia ; salome.mtchedlidze.1@iliauni.edu.ge; Nordita, KTH Royal Institute of Technology and Stockholm University , Hannes Alfvéns väg 12, SE-10691 Stockholm, Sweden; The Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, Sweden; McWilliams Center for Cosmology and Department of Physics, Carnegie Mellon University , 5000 Forbes Ave, Pittsburgh, PA 15213, USAInstitute for Astrophysics and Geophysics, Georg-August-Universität Göttingen , Friedrich-Hund-Platz 1, D-37077 Göttingen, GermanySchool of Natural Sciences and Medicine, Ilia State University , 3-5 Cholokashvili St., 0194 Tbilisi, Georgia ; salome.mtchedlidze.1@iliauni.edu.ge; E. Kharadze Georgian National Astrophysical Observatory , 47–57 Kostava St., Tbilisi 0179, Georgia; McWilliams Center for Cosmology and Department of Physics, Carnegie Mellon University , 5000 Forbes Ave, Pittsburgh, PA 15213, USAPrimordial magnetic fields (PMFs) are possible candidates for explaining the observed magnetic fields in galaxy clusters. Two competing scenarios of primordial magnetogenesis have been discussed in the literature: inflationary and phase-transitional. We study the amplification of both large- and small-scale correlated magnetic fields, corresponding to inflation- and phase transition–generated PMFs, in a massive galaxy cluster. We employ high-resolution magnetohydrodynamic cosmological zoom-in simulations to resolve the turbulent motions in the intracluster medium. We find that the turbulent amplification is more efficient for the large-scale inflationary models, while the phase transition–generated seed fields show moderate growth. The differences between the models are imprinted on the spectral characteristics of the field (such as the amplitude and the shape of the magnetic power spectrum) and therefore also on the final correlation length. We find a one order of magnitude difference between the final strengths of the inflation- and phase transition–generated magnetic fields, and a factor of 1.5 difference between their final coherence scales. Thus, the final configuration of the magnetic field retains information about the PMF generation scenarios. Our findings have implications for future extragalactic Faraday rotation surveys with the possibility of distinguishing between different magnetogenesis scenarios.https://doi.org/10.3847/1538-4357/acb04dMagnetohydrodynamical simulationsGalaxy clustersPrimordial magnetic fieldsIntracluster medium |
| spellingShingle | Salome Mtchedlidze Paola Domínguez-Fernández Xiaolong Du Wolfram Schmidt Axel Brandenburg Jens Niemeyer Tina Kahniashvili Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters The Astrophysical Journal Magnetohydrodynamical simulations Galaxy clusters Primordial magnetic fields Intracluster medium |
| title | Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters |
| title_full | Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters |
| title_fullStr | Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters |
| title_full_unstemmed | Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters |
| title_short | Inflationary and Phase-transitional Primordial Magnetic Fields in Galaxy Clusters |
| title_sort | inflationary and phase transitional primordial magnetic fields in galaxy clusters |
| topic | Magnetohydrodynamical simulations Galaxy clusters Primordial magnetic fields Intracluster medium |
| url | https://doi.org/10.3847/1538-4357/acb04d |
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