62 research outputs found
Comparative Analysis of Super-Kamiokande and SNO Solar-Neutrino Data and the Photospheric Magnetic Field
We analyze Super-Kamiokande, SNO, and photospheric magnetic-field data for
the common time interval, namely the SNO D2O phase. Concerning rotational
modulation, the magnetic-field power spectrum shows the strongest peaks at the
second and sixth harmonics of the solar synodic rotation frequency [3 nu(rot)
and 7 nu(rot)]. The restricted Super-Kamiokande dataset shows strong modulation
at the second harmonic. The SNO D2O dataset shows weak modulation at that
frequency, but strong modulation in the sixth-harmonic frequency band. We
estimate the significance level of the correspondence of the Super-Kamiokande
second-harmonic peak with the corresponding magnetic-field peak to be 0.0004,
and the significance level of the correspondence of the SNO D2O sixth-harmonic
peak with the corresponding magnetic-field peak to be 0.009. By estimating the
amplitude of the modulation of the solar neutrino flux at the second harmonic
from the restricted Super-Kamiokande dataset, we find that the weak power at
that frequency in the SNO D2O power spectrum is not particularly surprising.
Concerning 9.43 yr-1, we find no peak at this frequency in the power spectrum
formed from the restricted Super-Kamiokande dataset, so it is no surprise that
this peak does not show up in the SNO D2O dataset, either.Comment: 32 pages, 8 tables, 16 figure
Comparative analysis of Gallex and GNO solar neutrino data
Since the GALLEX and GNO datasets were derived from closely related
experiments, there is a natural tendency to merge them. This is perhaps
appropriate for any analysis based on the hypothesis that the solar neutrino
flux is constant, but it is not necessarily appropriate for an analysis that
allows for possible variability, since the GALLEX and GNO experiments belong to
different solar cycles. Moreover, we find significant differences between the
GALLEX and GNO datasets. It appears, from inspection of the time series and
histograms, that GNO measurements are compatible with the assumption that the
solar neutrino flux is constant, but GALLEX measurements are not. Furthermore,
power-spectrum analysis yields evidence of rotational modulation in GALLEX data
but not in GNO data. We compare our results with those of Pandola, who claims
that GALLEX-GNO data show no evidence for variability.Comment: 20 pages plus 6 tables plus 11 figure
Evidence for large superhumps in TX Col and V4742 Sgr
Since the discovery of the largest positive superhump period in TV Col, we
have started a program to search for superhumps in CVs with large orbital
periods. Here, we summarize preliminary results of TX Col and V4742 Sgr. TX Col
is an intermediate polar with a 5.7-h orbital period. V4742 Sgr is a recent
nova with no known periods. CCD unfiltered continuous photometry of these 2
objects was carried out during 56 nights in 2002-3. In TX Col, in addition to
the orbital period of 5.7 h, we found peaks at 7.1 h and 5.0 h. These are
interpreted as positive and negative superhumps correspondingly, although the
effects of the quasi-periodic oscillations at about 2 h were not taken into
consideration. In the light curve of V4742 Sgr 2 long periods are detected --
6.1 and 5.4 h as well as a short-term period at 1.6 h. This result suggests
that V4742 Sgr is an intermediate polar candidate and a permanent superhump
system with a large orbital period (5.4 h) and a superhump period excess of 13
percent. If these results are confirmed, TX Col, V4742 Sgr and TV Col form a
group of intermediate polars with extremely large superhump periods. There
seems to be now growing evidence that superhumps can occur in intermediate
polars with long orbital periods, which is very likely inconsistent with the
theoretical prediction that superhumps can only occur in systems with mass
ratios below 0.33. Alternatively, if the mass ratio in these systems is
nevertheless below the theoretical limit, they should harbour undermassive
secondaries and massive white dwarfs, near the Chandrasekhar limit, which would
make them excellent candidates for progenitors of supernovae type Ia.Comment: 9 pages, 8 figures, 3 sty files, To appear in the proceedings of IAU
JD5, `White Dwarfs: Galactic and Cosmological Probes', eds. Ed Sion, Stephane
Vennes and Harry Shipman, Full abstract in pape
MaxEnt power spectrum estimation using the Fourier transform for irregularly sampled data applied to a record of stellar luminosity
The principle of maximum entropy is applied to the spectral analysis of a
data signal with general variance matrix and containing gaps in the record. The
role of the entropic regularizer is to prevent one from overestimating
structure in the spectrum when faced with imperfect data. Several arguments are
presented suggesting that the arbitrary prefactor should not be introduced to
the entropy term. The introduction of that factor is not required when a
continuous Poisson distribution is used for the amplitude coefficients. We
compare the formalism for when the variance of the data is known explicitly to
that for when the variance is known only to lie in some finite range. The
result of including the entropic measure factor is to suggest a spectrum
consistent with the variance of the data which has less structure than that
given by the forward transform. An application of the methodology to example
data is demonstrated.Comment: 15 pages, 13 figures, 1 table, major revision, final version,
Accepted for publication in Astrophysics & Space Scienc
Multidimensional relativistic MHD simulations of Pulsar Wind Nebulae: dynamics and emission
Pulsar Wind Nebulae, and the Crab nebula in particular, are the best cosmic
laboratories to investigate the dynamics of magnetized relativistic outflows
and particle acceleration up to PeV energies. Multidimensional MHD modeling by
means of numerical simulations has been very successful at reproducing, to the
very finest details, the innermost structure of these synchrotron emitting
nebulae, as observed in the X-rays. Therefore, the comparison between the
simulated source and observations can be used as a powerful diagnostic tool to
probe the physical conditions in pulsar winds, like their composition,
magnetization, and degree of anisotropy. However, in spite of the wealth of
observations and of the accuracy of current MHD models, the precise mechanisms
for magnetic field dissipation and for the acceleration of the non-thermal
emitting particles are mysteries still puzzling theorists to date. Here we
review the methodologies of the computational approach to the modeling of
Pulsar Wind Nebulae, discussing the most relevant results and the recent
progresses achieved in this fascinating field of high-energy astrophysics.Comment: 29 pages review, preliminary version. To appear in the book
"Modelling Nebulae" edited by D. Torres for Springer, based on the invited
contributions to the workshop held in Sant Cugat (Barcelona), June 14-17,
201
Statistical Models for Solar Flare Interval Distribution in Individual Active Regions
This article discusses statistical models for solar flare interval
distribution in individual active regions. We analyzed solar flare data in 55
active regions that are listed in the GOES soft X-ray flare catalog. We discuss
some problems with a conventional procedure to derive probability density
functions from any data set and propose a new procedure, which uses the maximum
likelihood method and Akaike Information Criterion (AIC) to objectively compare
some competing probability density functions. We found that lognormal and
inverse Gaussian models are more likely models than the exponential model for
solar flare interval distribution in individual active regions. The results
suggest that solar flares do not occur randomly in time; rather, solar flare
intervals appear to be regulated by solar flare mechanisms. We briefly mention
a probabilistic solar flare forecasting method as an application of a solar
flare interval distribution analysis.Comment: 15 pages, 2 figures, 3 tables, accepted for publication in Solar
Physic
Observations of quasi-periodic solar X-ray emission as a result of MHD oscillations in a system of multiple flare loops
We investigate the solar flare of 20 October 2002. The flare was accompanied
by quasi-periodic pulsations (QPP) of both thermal and nonthermal hard X-ray
emissions (HXR) observed by RHESSI in the 3-50 keV energy range. Analysis of
the HXR time profiles in different energy channels made with the Lomb
periodogram indicates two statistically significant time periods of about 16
and 36 seconds. The 36-second QPP were observed only in the nonthermal HXR
emission in the impulsive phase of the flare. The 16-second QPP were more
pronounced in the thermal HXR emission and were observed both in the impulsive
and in the decay phases of the flare. Imaging analysis of the flare region, the
determined time periods of the QPP and the estimated physical parameters of
magnetic loops in the flare region allow us to interpret the observations as
follows. 1) In the impulsive phase energy was released and electrons were
accelerated by successive acts with the average time period of about 36 seconds
in different parts of two spatially separated, but interacting loop systems of
the flare region. 2) The 36-second periodicity of energy release could be
caused by the action of fast MHD oscillations in the loops connecting these
flaring sites. 3) During the first explosive acts of energy release the MHD
oscillations (most probably the sausage mode) with time period of 16 seconds
were excited in one system of the flare loops. 4) These oscillations were
maintained by the subsequent explosive acts of energy release in the impulsive
phase and were completely damped in the decay phase of the flare.Comment: 14 pages, 4 figure
Nonlinear time-series analysis of Hyperion's lightcurves
Hyperion is a satellite of Saturn that was predicted to remain in a chaotic
rotational state. This was confirmed to some extent by Voyager 2 and Cassini
series of images and some ground-based photometric observations. The aim of
this aticle is to explore conditions for potential observations to meet in
order to estimate a maximal Lyapunov Exponent (mLE), which being positive is an
indicator of chaos and allows to characterise it quantitatively. Lightcurves
existing in literature as well as numerical simulations are examined using
standard tools of theory of chaos. It is found that existing datasets are too
short and undersampled to detect a positive mLE, although its presence is not
rejected. Analysis of simulated lightcurves leads to an assertion that
observations from one site should be performed over a year-long period to
detect a positive mLE, if present, in a reliable way. Another approach would be
to use 2---3 telescopes spread over the world to have observations distributed
more uniformly. This may be achieved without disrupting other observational
projects being conducted. The necessity of time-series to be stationary is
highly stressed.Comment: 34 pages, 12 figures, 4 tables; v2 after referee report; matches the
version accepted in Astrophysics and Space Scienc
Analysis of bimodality in histograms formed from GALLEX and GNO solar neutrino data
A histogram display of the solar neutrino capture-rate measurements made by
the GALLEX experiment appears to be bimodal, but that of the follow-on GNO
experiment does not. To assess the significance of these results, we introduce
a "bimodality index" based on the probability-transform procedure. This
confirms that the GALLEX measurements are indeed bimodal (at the 99.98 percent
confidence level), and that the GNO measurements are not. Tracking the
bimodality index as a function of time shows that the strongest contribution to
bimodality comes from runs 42 to 62, i.e. from the time interval 1995.1 to
1996.9. The bimodality index for the first half (runs 1 through 33) is 2.56,
whereas that for the second half (runs 33 through 65) is 7.05. Power-spectrum
analysis shows a similar distinction: the peaks in the power spectrum formed
from the second half are stronger than those in the power spectrum formed from
the first half, suggesting that bimodality and rotational modulation are
related.Comment: 14 pages, 8 figure
Combined analysis of solar neutrino and solar irradiance data: further evidence for variability of the solar neutrino flux and its implications concerning the solar core
A search for any particular feature in any single solar neutrino dataset is
unlikely to establish variability of the solar neutrino flux since the count
rates are very low. It helps to combine datasets, and in this article we
examine data from both the Homestake and GALLEX experiments. These show
evidence of modulation with a frequency of 11.85 yr-1, which could be
indicative of rotational modulation originating in the solar core. We find that
precisely the same frequency is prominent in power spectrum analyses of the
ACRIM irradiance data for both the Homestake and GALLEX time intervals. These
results suggest that the solar core is inhomogeneous and rotates with sidereal
frequency 12.85 yr-1. We find, by Monte Carlo calculations, that the
probability that the neutrino data would by chance match the irradiance data in
this way is only 2 parts in 10,000. This rotation rate is significantly lower
than that of the inner radiative zone (13.97 yr-1) as recently inferred from
analysis of Super-Kamiokande data, suggesting that there may be a second, inner
tachocline separating the core from the radiative zone. This opens up the
possibility that there may be an inner dynamo that could produce a strong
internal magnetic field and a second solar cycle.Comment: 22 pages, 9 tables, 10 figure
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