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PreprintarXiv licencearXiv

Stability of rotation axis of galactic disks in HESTIA suite

  • Naira R. Arakelyan
  • Sergey V. Pilipenko
  • Stefan Gottlöber
  • Noam I. Libeskind
  • Gustavo Yepes
  • Yehuda Hoffman
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Abstract

We have found that in approximately 1/4 of Milky Way or M31 analogues in the HESTIA suite of simulations there is a significant, >45∘, change in the axis of rotation orientation of the gaseous disk during the last 6 Gyr. In 6 out of 7 such cases the change is likely caused by the accretion of individual satellites, while in one case such a connection is not obvious. All galaxies that underwent a significant change in rotation axis direction also had angular momentum amplitudes below the sample median 6 Gyr ago. Our findings support the idea that last 6~Gyr was a quiet phase of evolution in the LG. On the other hand, the mechanism we detect, that satellites can flip galaxy orientation, can explain the difficulties in identifying correlations between the rotation axis and the orientation of large-scale structure elements.

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Cite

BibTeXRIS
BibTeX
@misc{arakelyan2026stability,
  title = {{Stability of rotation axis of galactic disks in HESTIA suite}},
  author = {Naira R. Arakelyan and Sergey V. Pilipenko and Stefan Gottlöber and Noam I. Libeskind and Gustavo Yepes and Yehuda Hoffman},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.30922},
  eprint = {2610.30922},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.30922},
}
RIS
TY  - UNPB
TI  - Stability of rotation axis of galactic disks in HESTIA suite
AU  - Naira R. Arakelyan
AU  - Sergey V. Pilipenko
AU  - Stefan Gottlöber
AU  - Noam I. Libeskind
AU  - Gustavo Yepes
AU  - Yehuda Hoffman
PY  - 2026
DA  - 2026/10/22
PB  - arXiv
DO  - 10.48550/arxiv.2610.30922
UR  - https://arxiv.org/abs/2610.30922
AB  - We have found that in approximately 1/4 of Milky Way or M31 analogues in the HESTIA suite of simulations there is a significant, >45^∘, change in the axis of rotation orientation of the gaseous disk during the last 6 Gyr. In 6 out of 7 such cases the change is likely caused by the accretion of individual satellites, while in one case such a connection is not obvious. All galaxies that underwent a significant change in rotation axis direction also had angular momentum amplitudes below the sample median 6 Gyr ago. Our findings support the idea that last 6~Gyr was a quiet phase of evolution in the LG. On the other hand, the mechanism we detect, that satellites can flip galaxy orientation, can explain the difficulties in identifying correlations between the rotation axis and the orientation of large-scale structure elements.
ER  -