skip to main content

Title: The long lives of giant clumps and the birth of outflows in gas-rich galaxies at high redshift

Star-forming disk galaxies at high redshift are often subject to violent disk instability, characterized by giant clumps whose fate is yet to be understood. The main question is whether the clumps disrupt within their dynamical timescale (≤50 Myr), like the molecular clouds in today's galaxies, or whether they survive stellar feedback for more than a disk orbital time (≈300 Myr) in which case they can migrate inward and help building the central bulge. We present 3.5-7 pc resolution adaptive mesh refinement simulations of high-redshift disks including photoionization, radiation pressure, and supernovae feedback. Our modeling of radiation pressure determines the mass loading and initial velocity of winds from basic physical principles. We find that the giant clumps produce steady outflow rates comparable to and sometimes somewhat larger than their star formation rate, with velocities largely sufficient to escape the galaxy. The clumps also lose mass, especially old stars, by tidal stripping, and the stellar populations contained in the clumps hence remain relatively young (≤200 Myr), as observed. The clumps survive gaseous outflows and stellar loss, because they are wandering in gas-rich turbulent disks from which they can reaccrete gas at high rates compensating for outflows and tidal stripping, overall keeping realisticmore » and self-regulated gaseous and stellar masses. The outflow and accretion rates have specific timescales of a few 10{sup 8} yr, as opposed to rapid and repeated dispersion and reformation of clumps. Our simulations produce gaseous outflows with velocities, densities, and mass loading consistent with observations, and at the same time suggest that the giant clumps survive for hundreds of Myr and complete their migration to the center of high-redshift galaxies. These long-lived clumps are gas-dominated and contain a moderate mass fraction of stars; they drive inside-out disk evolution, thickening, spheroid growth, and fueling of the central black hole.« less
Authors:
; ; ; ; ; ; ; ;  [1] ; ; ;  [2] ;  [3] ;  [4] ;  [5] ;  [6]
  1. CEA, IRFU/SAp, F-91191 Gif-Sur-Yvette (France)
  2. Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), F-13388 Marseille (France)
  3. Center for Astrophysics and Planetary Science, Racah Institute of Physics, The Hebrew University, Jerusalem 91904 (Israel)
  4. IBM Research Division, T.J. Watson Research Center, Yorktown Heights, NY 10598 (United States)
  5. Department of Physics and Astronomy, Vassar College, Poughkeepsie, NY 12604 (United States)
  6. Institute for Theoretical Physics, University of Zurich, CH-8057 Zurich (Switzerland)
Publication Date:
OSTI Identifier:
22348351
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 780; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLACK HOLES; COMPARATIVE EVALUATIONS; DENSITY; DISPERSIONS; EVOLUTION; GALAXIES; INSTABILITY; LOSSES; MASS; PHOTOIONIZATION; RADIATION PRESSURE; RED SHIFT; RESOLUTION; SIMULATION; SPHEROIDS; STRIPPING; SUPERNOVAE; VELOCITY