2,177 research outputs found
Limits on Pop III star formation with the most iron-poor stars
We study the impact of star-forming mini-haloes, and the Initial Mass
Function (IMF) of Population III (Pop III) stars, on the Galactic halo
Metallicity Distribution Function (MDF) and on the properties of C-enhanced and
C-normal stars at [Fe/H]<-3. For our investigation we use a data-constrained
merger tree model for the Milky Way formation, which has been improved to
self-consistently describe the physical processes regulating star-formation in
mini-haloes, including the poor sampling of the Pop III IMF. We find that only
when star-forming mini-haloes are included the low-Fe tail of the MDF is
correctly reproduced, showing a plateau that is built up by C-enhanced
metal-poor (CEMP) stars imprinted by primordial faint supernovae. The
incomplete sampling of the Pop III IMF in inefficiently star-forming
mini-haloes (< /yr) strongly limits the formation of Pair
Instability Supernovae (PISNe), with progenitor masses =[140-260] , even when a flat Pop III IMF is assumed.
Second-generation stars formed in environments polluted at >50% level by PISNe
are thus extremely rare, corresponding to 0.25% of the total stellar
population at [Fe/H]<-2, which is consistent with recent observations. The
low-Fe tail of the MDF strongly depends on the Pop III IMF shape and mass
range. Given the current statistics, we find that a flat Pop III IMF model with
=[10-300] is disfavoured by observations. We present
testable predictions for Pop III stars extending down to lower masses, with
=[0.1-300] .Comment: 15 pages, 11 figures. Accepted for publication in MNRAS. The only
change is the correction of a mistake in the list of author
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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A new CO carbonaceous chondrite from Acfer, Algeria
Many small fragments, totally weighing 118 g were found in the Acfer area by an Italian dealer. Chondrules size and types (predominance of granular olivine type), occurrence of twinned clinoenstatite and absence of plagioclase suggested a classification as CO carbonaceous chondrite
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A new CK carbonaceous chondrite from Hammada Al Hamra, Libya
A single stone weighing 198 g was found in 2001 in the Hammada al Hamra region of Libya. Petrographic features (mean chondrules dimensions, coarse grained matrix and presence of AOIs and CAIs) point to a classification as CK carbonaceous chondrite
The Classical notion of competition revisited
The paper seeks to fill a lacuna within classical economics concerning the
process of market price determination in situations of market disequilibrium. To this aim, first we distinguish the classical notion of free competition from the Walrasian notion of perfect competition and we argue that
the latter is beset with some theoretical difficulties alien to the former.
Second, we reconstruct in some detail Smith\u2019s and Marx\u2019s views concerning market price determination and show that Marx\u2019s extensive use of
metaphors and numerical examples foreshadows the modern taxonomy of
buyers\u2019 market, sellers\u2019 market, and mixed strategy equilibrium in the
capacity space of a standard Bertrand duopoly model. Finally, we highlight similarities and differences between the classical notion of competition and contemporary Bertrand competition models
Observações sobre a biologia de Spodoptera frugiperda (J.E. Smith, 1797) (Lepidoptera-Noctuidae) em trigo.
bitstream/item/65942/1/CPAO-COM.-TEC.-8-82.pd
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Textural and minerochemical features of NWA 1807 and 2180, two new CV3 chondrites from northwest Africa
A textural and minerochemical study has been performed on NWA 1807 and 2180 chondrites in order to determine sizes and typologies of chondrules, relative abundances of mineral phases, compositions of main phases and bulk oxygen isotope composition
Ocorrência de Megascelis satrapa e avaliação de inseticidas para seu controle, em soja.
bitstream/item/133988/1/ID12230-1989-1990sojaresultados-p73-75.pdfTrabalho apresentado na XVIII Reunião de Pesquisa de Soja da Região Sul, Passo Fundo, 1990
Galaxy formation with radiative and chemical feedback
Here we introduce GAMESH, a novel pipeline which implements self-consistent
radiative and chemical feedback in a computational model of galaxy formation.
By combining the cosmological chemical-evolution model GAMETE with the
radiative transfer code CRASH, GAMESH can post process realistic outputs of a
N-body simulation describing the redshift evolution of the forming galaxy.
After introducing the GAMESH implementation and its features, we apply the code
to a low-resolution N-body simulation of the Milky Way formation and we
investigate the combined effects of self-consistent radiative and chemical
feedback. Many physical properties, which can be directly compared with
observations in the Galaxy and its surrounding satellites, are predicted by the
code along the merger-tree assembly. The resulting redshift evolution of the
Local Group star formation rates, reionisation and metal enrichment along with
the predicted Metallicity Distribution Function of halo stars are critically
compared with observations. We discuss the merits and limitations of the first
release of GAMESH, also opening new directions to a full implementation of
feedback processes in galaxy formation models by combining semi-analytic and
numerical methods.Comment: This version has coloured figures not present in the printed version.
Submitted to MNRAS, minor revision
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