000112519 001__ 112519 000112519 005__ 20240319080958.0 000112519 0247_ $$2doi$$a10.1103/PhysRevD.105.023516 000112519 0248_ $$2sideral$$a128110 000112519 037__ $$aART-2022-128110 000112519 041__ $$aeng 000112519 100__ $$aEggemeier, Benedikt 000112519 245__ $$aGravitational collapse in the postinflationary Universe 000112519 260__ $$c2022 000112519 5060_ $$aAccess copy available to the general public$$fUnrestricted 000112519 5203_ $$aThe Universe may pass through an effectively matter-dominated epoch between inflation and big bang nucleosynthesis during which gravitationally bound structures can form on subhorizon scales. In particular, the inflaton field can collapse into inflaton halos, forming "large scale"structure in the very early universe. We combine N-body simulations with high-resolution zoom-in regions in which the nonrelativistic Schrödinger-Poisson equations are used to resolve the detailed, wave-like structure of inflaton halos. Solitonic cores form inside them, matching structure formation simulations with axion-like particles in the late-time universe. We denote these objects inflaton stars, by analogy with boson stars. Based on a semianalytic formalism we compute their overall mass distribution which shows that some regions will reach overdensities of 1015 if the early matter-dominated epoch lasts for 20 e-folds. The radii of the most massive inflaton stars can shrink below the Schwarzschild radius, suggesting that they could form primordial black holes prior to thermalization. © 2022 American Physical Society. 000112519 536__ $$9info:eu-repo/grantAgreement/ES/AEI-FEDER/PGC2018-095328-B-I00 000112519 540__ $$9info:eu-repo/semantics/openAccess$$aby$$uhttp://creativecommons.org/licenses/by/3.0/es/ 000112519 590__ $$a5.0$$b2022 000112519 592__ $$a1.639$$b2022 000112519 591__ $$aPHYSICS, PARTICLES & FIELDS$$b7 / 29 = 0.241$$c2022$$dQ1$$eT1 000112519 593__ $$aPhysics and Astronomy (miscellaneous)$$c2022$$dQ1 000112519 591__ $$aASTRONOMY & ASTROPHYSICS$$b15 / 69 = 0.217$$c2022$$dQ1$$eT1 000112519 593__ $$aNuclear and High Energy Physics$$c2022$$dQ1 000112519 594__ $$a9.2$$b2022 000112519 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion 000112519 700__ $$aSchwabe, Bodo 000112519 700__ $$aNiemeyer, Jens C. 000112519 700__ $$aEasther, Richard 000112519 773__ $$g105, 2 (2022), 023516 [10 pp]$$pPhys. rev. D$$tPhysical Review D$$x2470-0010 000112519 8564_ $$s4264496$$uhttps://zaguan.unizar.es/record/112519/files/texto_completo.pdf$$yVersión publicada 000112519 8564_ $$s2947915$$uhttps://zaguan.unizar.es/record/112519/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada 000112519 909CO $$ooai:zaguan.unizar.es:112519$$particulos$$pdriver 000112519 951__ $$a2024-03-18-13:52:13 000112519 980__ $$aARTICLE