1,527 research outputs found
Low-Mass Star Formation, Triggered by Supernova in Primordial Clouds
The evolution of a gas shell, swept by the supernova remnant of a massive
first generation star, is studied with H_2 and HD chemistry taken into account.
When a first-generation star explodes as a supernova, H_2 and HD molecules are
formed in the swept gas shell and effectively cool the gas shell to
temperatures of 32 K - 154 K. If the supernova remnant can sweep to gather the
ambient gas, the gas shell comes to be dominated by its self-gravity, and
hence, is expected to fragment. Our result shows that for a reasonable range of
temperatures (200 K - 1000 K) of interstellar gas, the formation of
second-generation stars can be triggered by a single supernova or hypernova.Comment: 38pages, 10 figures, The Astrophysical Journal, accepted 8 Dec. 200
Effect of extreme data loss on long-range correlated and anti-correlated signals quantified by detrended fluctuation analysis
We investigate how extreme loss of data affects the scaling behavior of
long-range power-law correlated and anti-correlated signals applying the DFA
method. We introduce a segmentation approach to generate surrogate signals by
randomly removing data segments from stationary signals with different types of
correlations. These surrogate signals are characterized by: (i) the DFA scaling
exponent of the original correlated signal, (ii) the percentage of
the data removed, (iii) the average length of the removed (or remaining)
data segments, and (iv) the functional form of the distribution of the length
of the removed (or remaining) data segments. We find that the {\it global}
scaling exponent of positively correlated signals remains practically unchanged
even for extreme data loss of up to 90%. In contrast, the global scaling of
anti-correlated signals changes to uncorrelated behavior even when a very small
fraction of the data is lost. These observations are confirmed on the examples
of human gait and commodity price fluctuations. We systematically study the
{\it local} scaling behavior of signals with missing data to reveal deviations
across scales. We find that for anti-correlated signals even 10% of data loss
leads to deviations in the local scaling at large scales from the original
anti-correlated towards uncorrelated behavior. In contrast, positively
correlated signals show no observable changes in the local scaling for up to
65% of data loss, while for larger percentage, the local scaling shows
overestimated regions (with higher local exponent) at small scales, followed by
underestimated regions (with lower local exponent) at large scales. Finally, we
investigate how the scaling is affected by the statistics of the remaining data
segments in comparison to the removed segments
Formation of Primordial Stars in a LCDM Universe
We study the formation of the first generation of stars in the standard cold
dark matter model, using a very high-resolution hydordynamic simulations. Our
simulation achieves a dynamic range of 10^{10} in length scale. With accurate
treatment of atomic and molecular physics, it allows us to study the
chemo-thermal evolution of primordial gas clouds to densities up to n =
10^{16}/cc without assuming any a priori equation of state; a six orders of
magnitudes improvement over previous three-dimensional calculations. All the
relevant atomic and molecular cooling and heating processes, including cooling
by collision-induced continuum emission, are implemented. For calculating
optically thick H2 cooling at high densities, we use the Sobolev method. To
examine possible gas fragmentation owing to thermal instability, we compute
explicitly the growth rate of isobaric perturbations. We show that the cloud
core does not fragment in either the low-density or high-density regimes. We
also show that the core remains stable against gravitational deformation and
fragmentation. We obtain an accurate gas mass accretion rate within a 10 Msun
innermost region around the protostar. The protostar is accreting the
surrounding hot gas at a rate of 0.001-0.01 Msun/yr. From these findings we
conclude that primordial stars formed in early minihalos are massive. We carry
out proto-stellar evolution calculations using the obtained accretion rate. The
resulting mass of the first star is M_ZAMS = 60-100 Msun, with the exact mass
dependent on the actual accretion rate.Comment: 27 pages, 13 embedded figures. Revised versio
Ação do fungicida mepronil no controle de Crinipellis perniciosa em cupuaçuzeiros, no campo.
Publicado tambĂ©m: FRAZĂO, D. A. C.; HOMMA, A. K. O; VIĂGAS, I. de J. M. (Ed.). Contribuição ao desenvolvimento da fruticultura na AmazĂŽnia. BelĂ©m, PA: Embrapa AmazĂŽnia Oriental, 2006. p. 453-457
Effects of a burst of formation of first-generation stars on the evolution of galaxies
First-generation (Population III) stars in the universe play an important
role inearly enrichment of heavy elements in galaxies and intergalactic medium
and thus affect the history of galaxies. The physical and chemical properties
of primordial gas clouds are significantly different from those of present-day
gas clouds observed in the nearby universe because the primordial gas clouds do
not contain any heavy elements which are important coolants in the gas.
Previous theoretical considerations have suggested that typical masses of the
first-generation stars are between several and
although it has been argued that the formation of very massive stars (e.g., ) is also likely. If stars with several are most popular
ones at the epoch of galaxy formation, most stars will evolve to hot (e.g.,
K), luminous () stars with gaseous and dusty
envelope prior to going to die as white dwarf stars. Although the duration of
this phase is short (e.g., yr), such evolved stars could contribute
both to the ionization of gas in galaxies and to the production of a lot of
dust grains if the formation of intermediate-mass stars is highly enhanced. We
compare gaseous emission-line properties of such nebulae with some interesting
high-redshift galaxies such asIRAS F10214+4724 and powerful radio galaxies.Comment: 25 pages, 7 figures, ApJ, in pres
Primordial Star Formation under Far-ultraviolet radiation
Thermal and chemical evolution of primordial gas clouds irradiated with
far-ultraviolet (FUV; < 13.6 eV) radiation is investigated. In clouds
irradiated by intense FUV radiation, sufficient hydrogen molecules to be
important for cooling are never formed. However, even without molecular
hydrogen, if the clouds are massive enough, they start collapsing via atomic
hydrogen line cooling. Such clouds continue to collapse almost isothermally
owing to successive cooling by H^{-} free-bound emission up to the number
density of 10^{16} cm^{-3}. Inside the clouds, the Jeans mass eventually falls
well below a solar mass. This indicates that hydrogen molecules are dispensable
for low-mass primordial star formation, provided fragmentation of the clouds
occurs at sufficiently high density.Comment: 32 pages and 9 figures. ApJ, in pres
Disorder Effect on the Vortex Pinning by the Cooling Process Control in the Organic Superconductor -(BEDT-TTF)Cu[N(CN)]Br
We investigate the influence of disorders in terminal ethylene groups of
BEDT-TTF molecules (ethylene-disorders) on the vortex pinning of the organic
superconductor -(BEDT-TTF)Cu[N(CN)]Br. Magnetization
measurements are performed under different cooling-processes. The second peak
in the magnetization hysteresis curve is observed for all samples studied, and
the hysteresis width of the magnetization becomes narrower by cooling faster.
In contradiction to the simple pinning effect of disorder, this result shows
the suppression of the vortex pinning force by introducing more
ethylene-disorders. The ethylene-disorder domain model is proposed for
explaining the observed result. In the case of the system containing a moderate
number of the ethylene-disorders, the disordered molecules form a domain
structure and it works as an effective pinning site. On the contrary, an excess
number of the ethylene-disorders may weaken the effect of the domain structure,
which results in the less effective pinning force on the vortices.Comment: 6 pages, 6 figure
On the Mass of Population III Stars
Performing 1D hydrodynamical calculations coupled with non-equilibrium
processes for H2 formation, we pursue the thermal and dynamical evolution of
filamentary primordial clouds and attempt to make an estimate on the mass of
population III stars. It is found that, almost independent of initial
conditions, a filamentary cloud continues to collapse nearly isothermally due
to H_2 cooling until the cloud becomes optically thick against the H_2 lines.
During the collapse the cloud structure separates into two parts, i.e., a
denser spindle and a diffuse envelope. The spindle contracts quasi-statically,
and thus the line mass of the spindle keeps a characteristic value determined
solely by the temperature ( K). Applying a linear theory, we find
that the spindle is unstable against fragmentation during the collapse. The
wavelength of the fastest growing perturbation lessens as the collapse
proceeds. Consequently, successive fragmentation could occur. When the central
density exceeds , the successive fragmentation may
cease since the cloud becomes opaque against the H_2 lines and the collapse
decelerates appreciably. The mass of the first star is then expected to be
typically , which may grow up to by accreting
the diffuse envelope. Thus, the first-generation stars are anticipated to be
massive but not supermassive.Comment: 23 pages, 6 figures, accepted by ApJ (April 10
On the Initial Mass Function of Population III Stars
The collapse and fragmentation of filamentary primordial gas clouds are
explored using 1D and 2D hydrodynamical simulations coupled with the
nonequilibrium processes of H2 formation. The simulations show that depending
upon the initial density,there are two occasions for the fragmentation of
primordial filaments. If a filament has relatively low initial density, the
radial contraction is slow due to less effective H2 cooling. This filament
tends to fragment into dense clumps before the central density reaches
cm, where H2 cooling by three-body reactions is effective and
the fragment mass is more massive than some tens . In contrast, if a
filament is initially dense, the more effective H2 cooling with the help of
three-body reactions allows the filament to contract up to
cm. After the density reaches cm, the filament
becomes optically thick to H2 lines and the radial contraction subsequently
almost stops. At this final hydrostatic stage, the fragment mass is lowered
down to because of the high density of the filament. The
dependence of the fragment mass upon the initial density could be translated
into the dependence on the local amplitude of random Gaussian density fields or
the epoch of the collapse of a parent cloud. Hence, it is predicted that the
initial mass function of Population III stars is likely to be bimodal with
peaks of and , where the relative
heights could be a function of the collapse epoch.Comment: Accepted by Ap
Is Thermal Instability Significant in Turbulent Galactic Gas?
We investigate numerically the role of thermal instability (TI) as a
generator of density structures in the interstellar medium (ISM), both by
itself and in the context of a globally turbulent medium. Simulations of the
instability alone show that the condenstion process which forms a dense phase
(``clouds'') is highly dynamical, and that the boundaries of the clouds are
accretion shocks, rather than static density discontinuities. The density
histograms (PDFs) of these runs exhibit either bimodal shapes or a single peak
at low densities plus a slope change at high densities. Final static situations
may be established, but the equilibrium is very fragile: small density
fluctuations in the warm phase require large variations in the density of the
cold phase, probably inducing shocks into the clouds. This result suggests that
such configurations are highly unlikely. Simulations including turbulent
forcing show that large- scale forcing is incapable of erasing the signature of
the TI in the density PDFs, but small-scale, stellar-like forcing causes
erasure of the signature of the instability. However, these simulations do not
reach stationary regimes, TI driving an ever-increasing star formation rate.
Simulations including magnetic fields, self-gravity and the Coriolis force show
no significant difference between the PDFs of stable and unstable cases, and
reach stationary regimes, suggesting that the combination of the stellar
forcing and the extra effective pressure provided by the magnetic field and the
Coriolis force overwhelm TI as a density-structure generator in the ISM. We
emphasize that a multi-modal temperature PDF is not necessarily an indication
of a multi-phase medium, which must contain clearly distinct thermal
equilibrium phases.Comment: 18 pages, 11 figures. Submitted to Ap
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