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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Magnetic contribution to outer-disk rotation in the spiral galaxy NGC 5055

  • Natalia Woźniak1
  • Joanna Jałocha2
  • Łukasz Bratek2
  • Szymon Sikora3
  1. 1Doctoral School, University of the National Education Commission , ul. Podchorążych 2, PL-30084 Kraków ,
  2. 2Institute of Physics, Cracow University of Technology , ul. Podchorążych 1, PL-30084 Kraków ,
  3. 3Astronomical Observatory, Jagiellonian University , Orla 171, PL-30244 Kraków ,
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Abstract

We test whether fields of galactic strength enhance NGC 5055’s outer gas rotation. Finite analytic disk decompositions yield consistent rotation–density pairs and a blended gravitational reference approximately retaining inner rotation while its density approaches the measured outer H i+He profile. This reference is modelled, not an independently measured stellar curve. Its difference from fitted gas rotation gives the required purely toroidal field for circular, axisymmetric midplane motion. The prescribed field strength at the reconstruction’s inner radial boundary is Bs. With hydrogen inertia, no pressure and Bs = 0, constant exponential heights of 1 kpc and 250 pc give approximate peaks of 5.47 and 10.95 μG near 34.9 kpc; 0.2 kpc gives approximately 12.24 μG. Extrapolated flaring exponential and Gaussian profiles peak at approximately 5.25 and 5.96 μG, respectively, near 33.8 kpc. For Bs=8 μ G, their fields decline overall to approximately 5.73 and 6.30 μG near 39.7 kpc. These estimates are conditional on the gravitational reference, vertical structure and prescribed boundary field. Comparison with total radio fields supports the field scale without establishing a magnetic origin for the rotation excess.

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Cite

BibTeXRIS
BibTeX
@article{wozniak2026magnetic,
  title = {{Magnetic contribution to outer-disk rotation in the spiral galaxy NGC 5055}},
  author = {Natalia Woźniak and Joanna Jałocha and Łukasz Bratek and Szymon Sikora},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = nov,
  doi = {10.1093/mnras/stag2093},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2093/9012715},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Magnetic contribution to outer-disk rotation in the spiral galaxy NGC 5055
AU  - Natalia Woźniak
AU  - Joanna Jałocha
AU  - Łukasz Bratek
AU  - Szymon Sikora
PY  - 2026
DA  - 2026/11/04
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2093
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2093/9012715
AB  - We test whether fields of galactic strength enhance NGC 5055’s outer gas rotation. Finite analytic disk decompositions yield consistent rotation–density pairs and a blended gravitational reference approximately retaining inner rotation while its density approaches the measured outer H i+He profile. This reference is modelled, not an independently measured stellar curve. Its difference from fitted gas rotation gives the required purely toroidal field for circular, axisymmetric midplane motion. The prescribed field strength at the reconstruction’s inner radial boundary is Bs. With hydrogen inertia, no pressure and Bs = 0, constant exponential heights of 1 kpc and 250 pc give approximate peaks of 5.47 and 10.95 μG near 34.9 kpc; 0.2 kpc gives approximately 12.24 μG. Extrapolated flaring exponential and Gaussian profiles peak at approximately 5.25 and 5.96 μG, respectively, near 33.8 kpc. For B_s=8 μ G, their fields decline overall to approximately 5.73 and 6.30 μG near 39.7 kpc. These estimates are conditional on the gravitational reference, vertical structure and prescribed boundary field. Comparison with total radio fields supports the field scale without establishing a magnetic origin for the rotation excess.
SN  - 0035-8711
SN  - 1365-2966
ER  -