2,902 research outputs found
The formation of supermassive black holes in rapidly rotating disks
Massive primordial halos exposed to moderate UV backgrounds are the potential
birthplaces of supermassive black holes. In such a halo, an initially
isothermal collapse will occur, leading to high accretion rates of
~M~yr. During the collapse, the gas in the interior
will turn into a molecular state, and form an accretion disk due to the
conservation of angular momentum. We consider here the structure of such an
accretion disk and the role of viscous heating in the presence of high
accretion rates for a central star of , and ~M. Our
results show that the temperature in the disk increases considerably due to
viscous heating, leading to a transition from the molecular to the atomic
cooling phase. We found that the atomic cooling regime may extend out to
several ~AU for a ~M central star and provides substantial
support to stabilize the disk. It therefore favors the formation of a massive
central object. The comparison of clump migration and contraction time scales
shows that stellar feedback from these clumps may occur during the later stages
of the evolution. Overall, viscous heating provides an important pathway to
obtain an atomic gas phase within the center of the halo, and helps in the
formation of very massive objects. The latter may collapse to form a massive
black hole of about ~M.Comment: Accepted for publication in Astronomy & Astrophysics, comments are
still welcom
Primordial star formation: relative impact of H2 three-body rates and initial conditions
Population III stars are the first stars in the Universe to form at z=20-30
out of a pure hydrogen and helium gas in minihalos of 10^5-10^6 M .
Cooling and fragmentation is thus regulated via molecular hydrogen. At
densities above 10^8 cm, the three-body H2 formation rates are
particularly important for making the gas fully molecular. These rates were
considered to be uncertain by at least a few orders of magnitude. We explore
the impact of new accurate three-body H2 formation rates derived by Forrey
(2013) for three different minihalos, and compare to the results obtained with
three-body rates employed in previous studies. The calculations are performed
with the cosmological hydrodynamics code ENZO (release 2.2) coupled with the
chemistry package KROME (including a network for primordial chemistry), which
was previously shown to be accurate in high resolution simulations. While the
new rates can shift the point where the gas becomes fully molecular, leading to
a different thermal evolution, there is no trivial trend in how this occurs.
While one might naively expect the results to be inbetween the calculations
based on Palla et al. (1983) and Abel et al. (2002), the behavior can be close
to the former or the latter depending on the dark matter halo that is explored.
We conclude that employing the correct three-body rates is about as equally
important as the use of appropriate initial conditions, and that the resulting
thermal evolution needs to be calculated for every halo individually.Comment: 10 pages, 9 figures, A&A, 561, A13 (2014
Episodic accretion in binary protostars emerging from self-gravitating solar mass cores
Observations show a large spread in the luminosities of young protostars,
which are frequently explained in the context of episodic accretion. We here
test this scenario using numerical simulations following the collapse of a
solar mass molecular cloud using the GRADSPH code, varying the strength of the
initial perturbations and the temperature of the cores. A specific emphasis of
this paper is to investigate the role of binaries and multiple systems in the
context of episodic accretion, and to compare their evolution to the evolution
in isolated fragments. Our models form a variety of low mass protostellar
objects including single, binary and triple systems with binaries more active
in exhibiting episodic accretion than isolated protostars. We also find a
general decreasing trend for the average mass accretion rate over time,
suggesting that the majority of the protostellar mass is accreted within the
first 10^5 years. This result can potentially help to explain the surprisingly
low average luminosities in the majority of the protostellar population.Comment: 16 pages, 13 figures, 4 tables. Accepted for publication with A&
The formation of the primitive star SDSS J102915+172927: effect of the dust mass and the grain-size distribution
Understanding the formation of the extremely metal poor star
SDSS-J102915+172927 is of fundamental importance to improve our knowledge on
the transition between the first and second generation of stars in the
Universe. In this paper, we perform three-dimensional cosmological
hydrodynamical simulations of dust-enriched halos during the early stages of
the collapse process including a detailed treatment of the dust physics. We
employ the astrochemistry package \krome coupled with the hydrodynamical code
\textsc{enzo} assuming grain size distributions produced by the explosion of
core-collapse supernovae of 20 and 35 M primordial stars which are
suitable to reproduce the chemical pattern of the SDSS-J102915+172927 star. We
find that the dust mass yield produced from Population III supernovae
explosions is the most important factor which drives the thermal evolution and
the dynamical properties of the halos. Hence, for the specific distributions
relevant in this context, the composition, the dust optical properties, and the
size-range have only minor effects on the results due to similar cooling
functions. We also show that the critical dust mass to enable fragmentation
provided by semi-analytical models should be revised, as we obtain values one
order of magnitude larger. This determines the transition from disk
fragmentation to a more filamentary fragmentation mode, and suggests that
likely more than one single supernova event or efficient dust growth should be
invoked to get such a high dust content.Comment: Accepted on Ap
Initial mass function of intermediate mass black hole seeds
We study the Initial Mass Function (IMF) and host halo properties of
Intermediate Mass Black Holes (IMBH, 10^{4-6} Msun) formed inside metal-free,
UV illuminated atomic cooling haloes (virial temperature T_vir > 10^4 K) either
via the direct collapse of the gas or via an intermediate Super Massive Star
(SMS) stage. We achieve this goal in three steps: (a) we derive the gas
accretion rate for a proto-SMS to undergo General Relativity instability and
produce a direct collapse black hole (DCBH) or to enter the ZAMS and later
collapse into a IMBH; (b) we use merger-tree simulations to select atomic
cooling halos in which either a DCBH or SMS can form and grow, accounting for
metal enrichment and major mergers that halt the growth of the proto-SMS by gas
fragmentation. We derive the properties of the host halos and the mass
distribution of black holes at this stage, and dub it the "Birth Mass
Function"; (c) we follow the further growth of the DCBH due to accretion of
leftover gas in the parent halo and compute the final IMBH mass.We consider two
extreme cases in which minihalos (T_vir < 10^4 K) can (fertile) or cannot
(sterile) form stars and pollute their gas leading to a different IMBH IMF. In
the (fiducial) fertile case the IMF is bimodal extending over a broad range of
masses, M= (0.5-20)x10^5 Msun, and the DCBH accretion phase lasts from 10 to
100 Myr. If minihalos are sterile, the IMF spans the narrower mass range M=
(1-2.8)x10^6 Msun, and the DCBH accretion phase is more extended (70-120 Myr).
We conclude that a good seeding prescription is to populate halos (a) of mass
7.5 < log (M_h/Msun) < 8, (b) in the redshift range 8 < z < 17, (c) with IMBH
in the mass range 4.75 < log (M_BH/Msun) < 6.25.Comment: MNRAS, in press. Comments welcom
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