Editing Galaxy formation and evolution (section)

====Stellar feedback====

Stars have an influence on their surrounding gas by injecting energy and momentum. This creates a feedback loop that regulates the process of star formation. To effectively control star formation, stellar feedback must generate galactic-scale outflows that expel gas from galaxies. Various methods are utilized to couple energy and momentum, particularly through supernova explosions, to the surrounding gas. These methods differ in how the energy is deposited, either thermally or kinetically. However, excessive radiative gas cooling must be avoided in the former case. Cooling is expected in dense and cold gas, but it cannot be reliably modeled in cosmological simulations due to low resolution. This leads to artificial and excessive cooling of the gas, causing the supernova feedback energy to be lost via radiation and significantly reducing its effectiveness.  In the latter case, kinetic energy cannot be radiated away until it thermalizes. However, using hydrodynamically decoupled wind particles to inject momentum non-locally into the gas surrounding active star-forming regions may still be necessary to achieve large-scale galactic outflows.<ref name="PillepichSpringelNelson2017">{{cite journal | last1 = Pillepich | first1 = Annalisa | last2 = Springel | first2 = Volker | last3 = Nelson | first3 = Dylan | last4 = Genel | first4 = Shy | last5 = Naiman | first5 = Jill | last6 = Pakmor | first6 = Rüdiger | last7 = Hernquist | first7 = Lars | last8 = Torrey | first8 = Paul | last9 = Vogelsberger | first9 = Mark | last10 = Weinberger | first10 = Rainer | last11 = Marinacci | first11 = Federico | title = Simulating galaxy formation with the IllustrisTNG model | journal = Monthly Notices of the Royal Astronomical Society | date = 12 October 2017 | volume = 473 | issue = 3 | pages = 4077–4106 | issn = 0035-8711 | eissn = 1365-2966 | doi = 10.1093/mnras/stx2656 | doi-access = free | pmid = | url = | arxiv = 1703.02970 }}</ref> Recent models explicitly model stellar feedback.<ref name="MuratovKerešFaucher-Giguère2015">{{cite journal | last1 = Muratov | first1 = Alexander L. | last2 = Kereš | first2 = Dušan | last3 = Faucher-Giguère | first3 = Claude-André | last4 = Hopkins | first4 = Philip F. | last5 = Quataert | first5 = Eliot | last6 = Murray | first6 = Norman | title = Gusty, gaseous flows of FIRE: galactic winds in cosmological simulations with explicit stellar feedback | journal = Monthly Notices of the Royal Astronomical Society | date = 13 October 2015 | volume = 454 | issue = 3 | pages = 2691–2713 | issn = 0035-8711 | eissn = 1365-2966 | doi = 10.1093/mnras/stv2126 | doi-access = free | pmid = | url = | arxiv = 1501.03155 }}</ref> These models not only incorporate supernova feedback but also consider other feedback channels such as energy and momentum injection from stellar winds, photoionization, and radiation pressure resulting from radiation emitted by young, massive stars.<ref name="StinsonBrookMacciò2012">{{cite journal | last1 = Stinson | first1 = G. S. | last2 = Brook | first2 = C. | last3 = Macciò | first3 = A. V. | last4 = Wadsley | first4 = J. | last5 = Quinn | first5 = T. R. | last6 = Couchman | first6 = H. M. P. | title = Making Galaxies In a Cosmological Context: the need for early stellar feedback | journal = Monthly Notices of the Royal Astronomical Society | date = 23 October 2012 | volume = 428 | issue = 1 | pages = 129–140 | issn = 0035-8711 | eissn = 1365-2966 | doi = 10.1093/mnras/sts028 | doi-access = free | pmid = | url = | arxiv = 1208.0002 }}</ref> During the [[Cosmic Dawn]], galaxy formation occurred in short bursts of 5 to 30 Myr due to stellar feedbacks.<ref>{{Cite journal |last1=Furlanetto |first1=Steven R |last2=Mirocha |first2=Jordan |date=22 February 2022 |title=Bursty star formation during the Cosmic Dawn driven by delayed stellar feedback |url=https://academic.oup.com/mnras/article/511/3/3895/6522193 |journal=[[Monthly Notices of the Royal Astronomical Society]] |language=en |volume=511 |issue=3 |pages=3895–3909 |doi=10.1093/mnras/stac310 |issn=0035-8711 |access-date=23 December 2023|doi-access=free |arxiv=2109.04488 }}</ref>