000164139 001__ 164139 000164139 005__ 20251121161352.0 000164139 0247_ $$2doi$$a10.1051/0004-6361/202556777 000164139 0248_ $$2sideral$$a146310 000164139 037__ $$aART-2025-146310 000164139 041__ $$adeu 000164139 100__ $$aDomínguez, I. 000164139 245__ $$aThe impact of axion-like particles on late stellar evolution 000164139 260__ $$c2025 000164139 5060_ $$aAccess copy available to the general public$$fUnrestricted 000164139 5203_ $$aContext. Stars with masses ranging from 3 to 11 M⊙ exhibit multiple evolutionary paths. Less massive stars in this range conclude their evolution as carbon-oxygen (CO) white dwarfs (COWDs). However, stars that achieve carbon ignition before the pressure induced by the degenerate electron halts the core contraction would either form massive CONe or ONe WDs, or they might undergo an electron-capture supernova (ECSN). Alternatively, they could photo-disintegrate neon and proceed with further thermonuclear burning, ultimately leading to the formation of a gravitationally unstable iron core. Aims. An evaluation of the impact of the energy loss caused by the production of axion-like-particles (ALPs) on the evolution and final destiny of these stars is the main objective. Methods. We computed various sets of stellar models, all with solar initial composition, varying the strengths of the ALP coupling with photons and electrons. Results. As a consequence of an ALP thermal production, the critical masses for off-center C and Ne ignitions are both shifted upward. When the current bounds for the ALP coupling strengths are assumed, the maximum mass for CO WD progenitors is about 1.1 M⊙ heavier than that obtained without the ALP energy loss, while the minimum mass for a core collapse supernova (CCSN) progenitor is 0.7 M⊙ higher. Conclusions. Current constraints from observed type II-P supernova light curves and pre-explosive luminosity do not exclude an ALP production within the current bounds. However, the maximum age of CCSN progenitors, as deduced from the star formation rate of the parent stellar population, would require a lower minimum mass. This discrepancy can be explained by assuming a moderate extra mixing (as due to core overshooting or rotational induced mixing) above the fully convective core that develops during the main sequence. 000164139 536__ $$9info:eu-repo/grantAgreement/EC/H2020/788781/EU/Towards the detection of the axion with the International Axion Observatory/IAXOplus$$9This project has received funding from the European Union’s Horizon 2020 research and innovation program under grant agreement No H2020 788781-IAXOplus$$9info:eu-repo/grantAgreement/ES/MICINN/PGC2022-126078NB-C21$$9info:eu-repo/grantAgreement/ES/MICINN/PID2019-108122GB-C31 000164139 540__ $$9info:eu-repo/semantics/openAccess$$aby$$uhttps://creativecommons.org/licenses/by/4.0/deed.es 000164139 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion 000164139 700__ $$aStraniero, O. 000164139 700__ $$aPiersanti, L. 000164139 700__ $$0(orcid)0000-0001-9823-6262$$aGiannotti, M.$$uUniversidad de Zaragoza 000164139 700__ $$aMirizzi, A. 000164139 7102_ $$12004$$2038$$aUniversidad de Zaragoza$$bDpto. Física Teórica$$cÁrea Astronomía y Astrofísica 000164139 773__ $$g702 (2025), A240 [9 pp.]$$pAstron. astrophys.$$tAstronomy and Astrophysics$$x0004-6361 000164139 8564_ $$s4303419$$uhttps://zaguan.unizar.es/record/164139/files/texto_completo.pdf$$yVersión publicada 000164139 8564_ $$s3304754$$uhttps://zaguan.unizar.es/record/164139/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada 000164139 909CO $$ooai:zaguan.unizar.es:164139$$particulos$$pdriver 000164139 951__ $$a2025-11-21-14:27:17 000164139 980__ $$aARTICLE