415 research outputs found
Solar spin down and neutrino fluxes
Effects of core spin-down process on neutrino flux in solar evolution theor
Microcomputer laboratories in mathematics education
AbstractThis article discusses the mathematical-educational potential of a computational laboratory at the pre-calculus and co-calculus levels. The laboratory envisaged is based on a set of microcomputers, whose use plays a central role in the teaching process, with particular emphasis on algorithmization. A new role for the mathematics teacher and professor is layed out, augmenting the “chalk and talk” methods by active participation as a laboratory instructor. Following a brief description of the integration of such a laboratory into the mathematical education, seven appropriate subjects are discussed, including some new relevant elementary proofs and worked out examples. Emphasis is placed upon the mathematical-educational byproducts (such as error bounds, ill-conditioning, complexity, rate of convergence, etc.) accompanying the implementation of these seven modules. Special attention is given to the removal of “black box” procedures and to the construction of “numerical methods that work”. Extensions and generalizations to more advanced topics are indicated, especially where the results in our modules may serve as points of departure in that direction
An Assessment of Dynamical Mass Constraints on Pre-Main Sequence Evolutionary Tracks
[abridged] We have assembled a database of stars having both masses
determined from measured orbital dynamics and sufficient spectral and
photometric information for their placement on a theoretical HR diagram. Our
sample consists of 115 low mass (M < 2.0 Msun) stars, 27 pre-main sequence and
88 main sequence. We use a variety of available pre-main sequence evolutionary
calculations to test the consistency of predicted stellar masses with
dynamically determined masses. Despite substantial improvements in model
physics over the past decade, large systematic discrepancies still exist
between empirical and theoretically derived masses. For main-sequence stars,
all models considered predict masses consistent with dynamical values above 1.2
Msun, some models predict consistent masses at solar or slightly lower masses,
and no models predict consistent masses below 0.5 Msun but rather all models
systematically under-predict such low masses by 5-20%. The failure at low
masses stems from the poor match of most models to the empirical main-sequence
below temperatures of 3800 K where molecules become the dominant source of
opacity and convection is the dominant mode of energy transport. For the
pre-main sequence sample we find similar trends. There is generally good
agreement between predicted and dynamical masses above 1.2 Msun for all models.
Below 1.2 Msun and down to 0.3 Msun (the lowest mass testable) most
evolutionary models systematically under-predict the dynamically determined
masses by 10-30% on average with the Lyon group models (e.g. Baraffe et al.
1998) predicting marginally consistent masses *in the mean* though with large
scatter.Comment: accepted for publication in ApJ (2004
Evolution and Nucleosynthesis of Zero Metal Intermediate Mass Stars
New stellar models with mass ranging between 4 and 8 Mo, Z=0 and Y=0.23 are
presented. The models have been evolved from the pre Main Sequence up to the
Asymptotic Giant Branch (AGB). At variance with previous claims, we find that
these updated stellar models do experience thermal pulses in the AGB phase. In
particular we show that: a) in models with mass larger than 6 Mo, the second
dredge up is able to raise the CNO abundance in the envelope enough to allow a
"normal" AGB evolution, in the sense that the thermal pulses and the third
dredge up settle on; b) in models of lower mass, the efficiency of the CNO
cycle in the H-burning shell is controlled by the carbon produced locally via
the 3alpha reactions. Nevertheless the He-burning shell becomes thermally
unstable after the early AGB. The expansion of the overlying layers induced by
these weak He-shell flashes is not sufficient by itself to allow a deep
penetration of the convective envelope. However, immediately after that, the
maximum luminosity of the He flash is attained and a convective shell
systematically forms at the base of the H-rich envelope. The innermost part of
this convective shell probably overlaps the underlying C-rich region left by
the inter-shell convection during the thermal pulse, so that fresh carbon is
dredged up in a "hot" H-rich environment and a H flash occurs. This flash
favours the expansion of the outermost layers already started by the weak
thermal pulse and a deeper penetration of the convective envelope takes place.
Then, the carbon abundance in the envelope rises to a level high enough that
the further evolution of these models closely resembles that of more metal rich
AGB stars. These stars provide an important source of primary carbon and
nitrogen.Comment: 28 pages, 5 tables and 17 figures. Accepted for publication in Ap
The Many Faces of a Character
We prove an identity between three infinite families of polynomials which are
defined in terms of `bosonic', `fermionic', and `one-dimensional configuration'
sums. In the limit where the polynomials become infinite series, they give
different-looking expressions for the characters of the two integrable
representations of the affine algebra at level one. We conjecture yet
another fermionic sum representation for the polynomials which is constructed
directly from the Bethe-Ansatz solution of the Heisenberg spin chain.Comment: 14/9 pages in harvmac, Tel-Aviv preprint TAUP 2125-9
Wave packet propagation by the Faber polynomial approximation in electrodynamics of passive media
Maxwell's equations for propagation of electromagnetic waves in dispersive
and absorptive (passive) media are represented in the form of the Schr\"odinger
equation , where is a linear
differential operator (Hamiltonian) acting on a multi-dimensional vector
composed of the electromagnetic fields and auxiliary matter fields describing
the medium response. In this representation, the initial value problem is
solved by applying the fundamental solution to the initial field
configuration. The Faber polynomial approximation of the fundamental solution
is used to develop a numerical algorithm for propagation of broad band wave
packets in passive media. The action of the Hamiltonian on the wave function
is approximated by the Fourier grid pseudospectral method. The algorithm
is global in time, meaning that the entire propagation can be carried out in
just a few time steps. A typical time step is much larger than that in finite
differencing schemes, . The accuracy and stability
of the algorithm is analyzed. The Faber propagation method is compared with the
Lanczos-Arnoldi propagation method with an example of scattering of broad band
laser pulses on a periodic grating made of a dielectric whose dispersive
properties are described by the Rocard-Powels-Debye model. The Faber algorithm
is shown to be more efficient. The Courant limit for time stepping, , is exceeded at least in 3000 times in the Faber propagation
scheme.Comment: Latex, 17 pages, 4 figures (separate png files); to appear in J.
Comput. Phy
CAST: Recent results & future outlook
Çetin, Serkant Ali (Dogus Author) -- Ezer, Cemile (Dogus Author) -- Yıldız, Süleyman Cenk (Dogus Author) -- Conference full title: 6th Patras Workshop on Axions, WIMPs and WISPs, PATRAS 2010; Zurich; Switzerland; 5 July 2010 through 9 July 2010.The CAST (CERN Axion Solar Telescope) experiment is searching for solar axions by their conversion into photons inside the magnet pipes of an LHC dipole. The analysis of data taken so far has shown no signal above the background, thus implying an upper limit to the axion-photon coupling of ga < 0.85 × 10-10GeV -1 at 95% CL for ma < 0.02 eV/c2. Ongoing measurements, with the magnet bores filled with a buffer gas (3He), are improving the sensitivity of the experiment for higher axion masses towards 1 eV/c2. Recent results, new ideas for Axion-Like Particle (WISPs) searches with CAST in the near future and the prospects of a new generation Helioscope are presented here
Helioseismology, solar models and neutrino fluxes
We present our results concerning a systematical analysis of helioseismic
implications on solar structure and neutrino production. We find
Y, and
gr/cm. In the interval , the quantity is
determined with and accuracy of \permille~or better. At the solar center
still one has remarkable accuracy, . We compare the predictions
of recent solar models (standard and non-standard) with the helioseismic
results. By constructing helioseismically constrained solar models, the central
solar temperature is found to be K with a conservatively
estimated accuracy of 1.4%, so that the major unceratainty on neutrino fluxes
is due to nuclear cross section and not to solar inputs.Comment: 14 pages including 9 figures, LaTex file, espcrc2.sty is needed; to
appear in Nucl. Phys. B Proc. Suppl., Proceedings of TAUP97 conference,
Laboratori Nazionali del Gran Sasso, September 199
Results and perspectives of the solar axion search with the CAST experiment
The status of the solar axion search with the CERN Axion Solar Telescope
(CAST) will be presented. Recent results obtained by the use of He as a
buffer gas has allowed us to extend our sensitivity to higher axion masses than
our previous measurements with He. With about 1 h of data taking at each of
252 different pressure settings we have scanned the axion mass range 0.39 eV 0.64 eV. From the absence of an excess of x rays when the
magnet was pointing to the Sun we set a typical upper limit on the axion-photon
coupling of g GeV at 95% C.L., the
exact value depending on the pressure setting. CAST published results represent
the best experimental limit on the photon couplings to axions and other similar
exotic particles dubbed WISPs (Weakly Interacting Slim Particles) in the
considered mass range and for the first time the limit enters the region
favored by QCD axion models. Preliminary sensitivities for axion masses up to
1.16 eV will also be shown reaching mean upper limits on the axion-photon
coupling of g GeV at 95% C.L.
Expected sensibilities for the extension of the CAST program up to 2014 will be
presented. Moreover long term options for a new helioscope experiment will be
evoked.Comment: 4 pages, 2 pages, to appear in the proceedings of the 24th Rencontres
de Blois V2 A few affiliations were not corrected in previous version V3
Author adde
Diffuse Cosmic Neutrino Background from Population III Stars
We study the expected diffuse cosmic neutrino flux produced by Population III
(PopIII) stars during their nuclear burning phases as well as from their final
stages of evolution (core collapse). Assuming a fraction f_III=10^(-3) of all
baryons forms PopIII stars, our flux estimate is comparable to the diffuse
neutrino flux produced by the ordinary stars and by the ordinary core-collapse
supernovae in the universe, i.e. of order 1-10 cm^(-2) s^(-1). Due to the large
cosmic redshift, however, the typical energies are in the MeV and sub-MeV range
where the solar and geophysical neutrino fluxes are much larger. A direct
detection of the diffuse cosmic flux is out of the question with presently
known experimental techniques.Comment: 17 pages, 7 figure
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