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Tress, RG, Brucy, N, Girichidis, P, Glover, SCO, Göller, J, Hirschmann, M, Klessen, RS, Peter, T, Petersson, J, Sormani, MC, Armillotta, L, Battersby, CD, Donati, M, Feng, ZX, Henshaw, JD 
ORCID: 0000-0001-9656-7682, Lipman, DR, Longmore, SN ORCID: 0000-0001-6353-0170, Nogueras-Lara, F, Pelkonen, VM, Peschken, N et al
(2026)
Rhea-RT: Dynamical impact of Central Molecular Zone conditions on the properties of the interstellar medium and stellar feedback coupling.
Astronomy and Astrophysics, 711.
A103-A103.
ISSN 0004-6361
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Abstract
The Central Molecular Zone (CMZ) is an extreme star formation environment, characterized by higher density, higher turbulence, stronger orbital shear, and stronger magnetic field strength than the solar neighborhood. It is still debated whether classical theories of star formation hold within this extreme environment. In order to assess the impact of these different conditions on the interstellar medium (ISM) and on star formation, we present radiation magnetohydrodynamic AREPO simulations of a Milky Way-type galaxy. We set up a high-resolution (Mcell = 20 M⊙) region in a ring around the solar radius and in the barred region of the Galaxy to have a coherent comparison between the CMZ and the solar neighborhood. Although the high densities and strong levels of turbulence affect star formation and feedback, a key difference in the regulation of star formation between the two environments comes from the short orbital times and the strong shear in the CMZ. In particular, we highlight the role of the quick dynamical decoupling of stars and gas, which leads to periodic re-embedding events in the early lifetimes of radiating O stars. Young stellar associations are efficiently sheared apart, such that the ISM is deprived of the compounding effect of radiation and supernovae in disrupting molecular clouds. This dramatically changes the evolution of giant molecular clouds and how feedback can regulate star formation in the CMZ. Stellar feedback is no longer directly coupled to the molecular cloud from which they formed, and no strong and disruptive superbubbles can develop. The feedback instead rather acts as a background source of turbulence.
| Item Type: | Article |
|---|---|
| Uncontrolled Keywords: | 5101 Astronomical Sciences; 51 Physical Sciences; 5101 Astronomical Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences |
| Subjects: | Q Science > QB Astronomy |
| Divisions: | Astrophysics Research Institute |
| Publisher: | EDP Sciences |
| Date of acceptance: | 27 April 2026 |
| Date of first compliant Open Access: | 17 July 2026 |
| Date Deposited: | 17 Jul 2026 13:42 |
| Last Modified: | 17 Jul 2026 13:42 |
| DOI or ID number: | 10.1051/0004-6361/202558503 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/29027 |
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