Editing Galaxy formation and evolution (section)

====Magnetic fields====

The ideal [[magnetohydrodynamics]] approach is commonly utilized in cosmological simulations since it provides a good approximation for cosmological magnetic fields. The effect of magnetic fields on the dynamics of gas is generally negligible on large cosmological scales. Nevertheless, magnetic fields are a critical component of the interstellar medium since they provide pressure support against gravity<ref name="Ferrière2001">{{cite journal | last1 = Ferrière | first1 = Katia M. | title = The interstellar environment of our galaxy | journal = Reviews of Modern Physics | date = 5 December 2001 | volume = 73 | issue = 4 | pages = 1031–1066 | issn = 0034-6861 | eissn = 1539-0756 | doi = 10.1103/RevModPhys.73.1031 | pmid = | url = | arxiv = astro-ph/0106359 | bibcode = 2001RvMP...73.1031F | s2cid = 16232084 }}</ref> and affect the propagation of cosmic rays.<ref name="KoteraOlinto2011">{{cite journal | last1 = Kotera | first1 = Kumiko | last2 = Olinto | first2 = Angela V. | title = The Astrophysics of Ultrahigh-Energy Cosmic Rays | journal = Annual Review of Astronomy and Astrophysics | date = 22 September 2011 | volume = 49 | issue = 1 | pages = 119–153 | issn = 0066-4146 | eissn = 1545-4282 | doi = 10.1146/annurev-astro-081710-102620 | pmid = | url = | arxiv = 1101.4256 | bibcode = 2011ARA&A..49..119K | s2cid = 118661799 }}</ref>