592 research outputs found
Event anisotropy in 4.2A GeV/c C+C collisions
The directed and elliptic flow of protons and negative pions in 4.2A GeV/c
C+C collisions is studied using the Fourier analysis of azimuthal
distributions. It is found that the protons exhibit pronounced directed flow,
while the flow of pions is either non existent or too weak to be detected
experimentally. Also, it is found that in the entire rapidity interval the
elliptic flow is very small if not zero. These results are confirmed by the
Quark-Gluon-String Model (QGSM) and the relativistic transport model (ART 1.0),
except that these models predict very weak antiflow of pions. The more detailed
comparison with the QGSM suggests that the decay of resonances and rescattering
of secondaries dominantly determine the proton and negative pion flow at this
energy.Comment: 7 pages, 3 figures, TeX file changed from double to single-spacin
Correlator Analysis of Multiparticle Events
A procedure for the evaluation of correlators of any order in a reasonable
computer time is presented. Connection between correlators and fluctuations of
the event mean values of observables is discussed. Extension of the procedure
to event-by-event approach is suggested. The usefulness of the method is
demonstrated using the events simulated within various models of multipaticle
production.Comment: LaTeX, 15 pages including 4 table
Light-Front Analysis of pi^{-} Mesons Produced in Mg - Mg Collisions at 4.3 a Gev/c
Light-front analysis of pi^{-} mesons in Mg-Mg collisions is carried out. The
phase space of secondary pions is naturally divided into two parts in one of
which the thermal equilibration assumption seems to be in a good agreement with
data. Corresponding temperatures are extracted and compared to the results of
other experiments. The experimental results have been compared with the
predictions of the Quark Gluon String Model (QGSM) and satisfactory agreement
between the experimental data and the model has been found.Comment: 14 pages with 7 postscript figures. accepted for publication in Nucl.
Phys.
Synchonisation of Resonances with Thresholds
The mechanism by which a resonance may be attracted to a sharp threshold is
described with several examples. It involves a threshold cusp interfering
constructively with either or both (i) a resonance produced via confinement,
(ii) attractive t- and u-channel exchanges. More generally, it is suggested
that resonances are eigenstates generated by mixing between confined states and
long-range meson and baryon exchanges.Comment: 8 pages, 4 figures. For Meson08 Proceedings. One important typo
correcte
Microscopic study of freeze-out in relativistic heavy ion collisions at SPS energies
The freeze-out conditions in the light (S+S) and heavy (Pb+Pb) colliding
systems of heavy nuclei at 160 AGeV/ are analyzed within the microscopic
Quark Gluon String Model (QGSM). We found that even for the most heavy systems
particle emission takes place from the whole space-time domain available for
the system evolution, but not from the thin ''freeze-out hypersurface", adopted
in fluid dynamical models. Pions are continuously emitted from the whole volume
of the reaction and reflect the main trends of the system evolution. Nucleons
in Pb+Pb collisions initially come from the surface region. For both systems
there is a separation of the elastic and inelastic freeze-out. The mesons with
large transverse momenta, , are predominantly produced at the early stages
of the reaction. The low -component is populated by mesons coming mainly
from the decay of resonances. This explains naturally the decreasing source
sizes with increasing , observed in HBT interferometry. Comparison with
S+S and Au+Au systems at 11.6 AGeV/ is also presented.Comment: REVTEX, 26 pages incl. 9 figures and 2 tables, to be published in the
Physical Review
The initial state of ultra-relativistic heavy ion collision
A model for energy, pressure and flow velocity distributions at the beginning
of ultra-relativistic heavy ion collisions is presented, which can be used as
an initial condition for hydrodynamic calculations. Our model takes into
account baryon recoil for both target and projectile, arising from the
acceleration of partons in an effective field, produced in the collision. The
typical field strength (string tension) for RHIC energies is about 5-12 GeV/fm,
what allows us to talk about "string ropes". The results show that a QGP forms
a tilted disk, such that the direction of the largest pressure gradient stays
in the reaction plane, but deviates from both the beam and the usual transverse
flow directions. Such initial conditions may lead to the creation of "antiflow"
or "third flow component".Comment: 28 pages, 9 figures. The presentation has been changed considerably.
Some parts of the model have been reformulated, what led to modifications in
several equations: (20-38), Apps. A, B. All the figures have been changed
from 100 GeV/nucl initial energy to the achieved RHIC energy of 65 GeV/nucl.
The last subplots in the Figs. 3, 4, 5, 6 present E=T^{00} in the laboratory
frame now, instead of the energy density in the local rest frame, e, shown in
the initial version. We also added the App. C to clarify the transformation
from space-time to lightcone coordinates and bac
Cross-sections for nuclide production in 56Fe target irradiated by 300, 500,750, 1000, 1500, and 2600 MeV protons compared with data on hydrogen target irradiation by 300, 500, 750, 1000, and 1500 MeV/nucleon 56Fe ions
Cross-sections for radioactive nuclide production in 56Fe(p,x) reactions at
300, 500, 750, 1000, 1500, and 2600 MeV were measured using the ITEP U-10
proton accelerator. In total, 221 independent and cumulative yields of products
of half-lives from 6.6 min to 312 days have been obtained via the
direct-spectrometry method. The measured data have been compared with the
experimental data obtained elsewhere by the direct and inverse kinematics
methods and with calculations by 15 codes, namely: MCNPX (INCL, CEM2k, BERTINI,
ISABEL), LAHET (BERTINI, ISABEL), CEM03 (.01, .G1, .S1), LAQGSM03 (.01, .G1,
>.S1), CASCADE-2004, LAHETO, and BRIEFF. Most of our data are in a good
agreement with the inverse kinematics results and disprove the results of some
earlier activation measurements that were quite different from the inverse
kinematics measurements. The most significant calculation-to-experiment
differences are observed in the yields of the A<30 light nuclei, indicating
that further improvements in nuclear reaction models are needed, and pointing
out as well to a necessity of more complete measurements of such reactions.Comment: 53 pages, 9 figures, 6 tables, only pdf file, submitted to Phys. Rev.
Universal Mass Dependence for Particle Production Rates in , and Collisions from the Quark-Gluon Plasma Perspective
It is demonstrated that universal mass dependence for meson and baryon
inclusive cross-sections advocated recently in annihilation and in
hadronic reactions is consistent also with heavy ion collisions data and can
therefore be used as a reference for quark-gluon plasma studies.Comment: LaTex file, 8 pages, hard copies of 3 (multiple) figures available on
request to [email protected] or [email protected]. PROCSLA.STY file
appended at the end of the LaTeX file for convenienc
The origin of short-lived radionuclides and the astrophysical environment of solar system formation
Based on early solar system abundances of short-lived radionuclides (SRs),
such as Al (T Myr) and Fe (T Myr),
it is often asserted that the Sun was born in a large stellar cluster, where a
massive star contaminated the protoplanetary disk with freshly
nucleosynthesized isotopes from its supernova (SN) explosion. To account for
the inferred initial solar system abundances of short-lived radionuclides, this
supernova had to be close ( 0.3 pc) to the young ( 1 Myr)
protoplanetary disk.
Here we show that massive star evolution timescales are too long, compared to
typical timescales of star formation in embedded clusters, for them to explode
as supernovae within the lifetimes of nearby disks. This is especially true in
an Orion Nebular Cluster (ONC)-type of setting, where the most massive star
will explode as a supernova 5 Myr after the onset of star formation,
when nearby disks will have already suffered substantial photoevaporation
and/or formed large planetesimals.
We quantify the probability for {\it any} protoplanetary disk to receive SRs
from a nearby supernova at the level observed in the early solar system. Key
constraints on our estimate are: (1) SRs have to be injected into a newly
formed ( 1 Myr) disk, (2) the disk has to survive UV
photoevaporation, and (3) the protoplanetary disk must be situated in an
enrichment zone permitting SR injection at the solar system level without disk
disruption. The probability of protoplanetary disk contamination by a supernova
ejecta is, in the most favorable case, 3 10
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