9,099 research outputs found
At Voyager 1 Starting on about August 25, 2012 at a Distance of 121.7 AU From the Sun, a Sudden Disappearance of Anomalous Cosmic Rays and an Unusually Large Sudden Increase of Galactic Cosmic Ray H and He Nuclei and Electron Occurred
At the Voyager 1 spacecraft in the outer heliosphere, after a series of
complex intensity changes starting at about May 8th, the intensities of both
anomalous cosmic rays (ACR) and galactic cosmic rays (GCR) changed suddenly and
decisively on August 25th (121.7 AU from the Sun). The ACR started the
intensity decrease with an initial e-folding rate of intensity decrease of ~1
day. Within a matter of a few days, the intensity of 1.9-2.7 MeV protons and
helium nuclei had decreased to less than 0.1 of their previous value and after
a few weeks, corresponding to the outward movement of V1 by ~0.1 AU, these
intensities had decreased by factors of at least 300-500 and are now lower than
most estimates of the GCR spectrum for these lower energies and also at higher
energies. The decrease was accompanied by large rigidity dependent anisotropies
in addition to the extraordinary rapidity of the intensity changes. Also on
August 25th the GCR protons, helium and heavier nuclei as well as electrons
increased suddenly with the intensities of electrons reaching levels ~30-50%
higher than observed just one day earlier. This increase for GCR occurred over
~1 day for the lowest rigidity electrons, and several days for the higher
rigidity nuclei of rigidity ~0.5-1.0 GV. After reaching these higher levels the
intensities of the GCR of all energies from 2 to 400 MeV have remained
essentially constant with intensity levels and spectra that may represent the
local GCR. These intensity changes will be presented in more detail in this,
and future articles, as this story unfolds.Comment: 13 Pages, 5 Figure
Termination shock particle spectral features
Spectral features of energetic H ions accelerated at the termination shock may be evidence of two components. At low energies the energy spectrum is ~E^(–1.55), with break at ~0.4 MeV to E^(–2.2). A second component appears above ~1 MeV with a spectrum of E^(–1.27) with a break at ~3.2 MeV. Even though the intensities upstream are highly variable, the same spectral break energies are observed, suggesting that these are durable features of the source spectrum. The acceleration processes for the two components may differ, with the lower energy component serving as the injection source for diffusive shock acceleration of the higher energy component. Alternatively, the spectral features may result from the energy dependence of the diffusion tensor that affects the threshold for diffusive shock acceleration
Voyager observations of galactic and anomalous cosmic rays in the helioshealth
Anomalous cosmic rays display large temporal variations at the time and location where Voyager 1 (V1) crossed the heliospheric termination shock (2004.86) (94AU, 34°N). On a short time scale (3 months) there was a large decrease produced by a series of merged interaction regions (MIR), the first of which was associated with the intense Oct./Nov. 2003 solar events. On a longer time scale there is a remarkable correlation between changes in the galactic cosmic ray (GCR) intensity and those of 10–56 MeV/n ACR He and 30–56 MeV H extending over a 4.3 year period with the GCRs exhibiting their expected behavior over this part of the 11 and 22 year solar activity and heliomagnetic cycle. The relative changes in the ACR and GCR are the same for both the short term and long term variations. The comparative V1/V2 ACR and GCR spectra in the foreshock and heliosheath indicate that at this time most of the higher energy ACRs are not being accelerated near V1 but must have their source region elsewhere — possibly near the equatorial region of the TS as was suggested in our first paper on the TS crossing (1)
Tide and Tidal Current Prediction by High Speed Digital Computer
The Tide and Tidal Current Tables of the U. S. Coast and Geodetic Survey for 1966 have been computed and edited by a digital computer, the IBM 7094. Prediction by this method is found to be more economical and expedient than by the tide prediction machine in use since 1910. The shift to digital predictions has been gradual. The first program was prepared in 1956 to predict hourly tide heights only, for use in storm surge research. The greatest advantage to digital prediction at that time was the elimination of the hour or more required to set up a new problem on the tide predicting machine, when highly accurate predictions were needed for many short periods. Later, as more efficient computers became available, this program was expanded to include the computation of highs and lows, editing the data in a form suitable for publication and the complete prediction and editing of the tidal current tables. The existing program, to a large degree, reproduced the same calculations formerly made on the analogue tide predicting machine, and with comparable accuracy. The greater versatility of this system invites experimentation, not feasible with the analogue computer. Thus, it is expected that in the long run the switch to digital calculations will lead to an increase in the accuracy of the predictions for stations having complex tide problems. The program grew through the years, and is not the most efficient that could be prepared today. Nevertheless, it appears doubtful that the improved efficiency would justify a complete revision. This report gives a general description of the program, the input data specifications and samples of the results
Analytical model of non-Markovian decoherence in donor-based charge quantum bits
We develop an analytical model for describing the dynamics of a donor-based
charge quantum bit (qubit). As a result, the quantum decoherence of the qubit
is analytically obtained and shown to reveal non-Markovian features: The
decoherence rate varies with time and even attains negative values, generating
a non-exponential decay of the electronic coherence and a later recoherence.
The resulting coherence time is inversely proportional to the temperature, thus
leading to low decoherence below a material dependent characteristic
temperature.Comment: 19 pages, 3 figure
Large periodic time variations of termination shock particles between ~0.5-20 mev and 6-14 mev electrons measured by the crs experiment on Voyager 2 as it crossed into the heliosheath in 2007: An example of freshly accelerated cosmic rays?
We have examined features in the structure of the heliosheath using the fine scale time variations of termination shock particles (TSP) between ~0.5 - 20 MeV and electrons between 2.5-14 MeV measured by the CRS instrument as the V2 spacecraft crossed the heliospheric termination shock in 2007. The very disturbed heliosheath at V2 is particularly noteworthy for strong periodic intensity variations of the TSP just after V2 crossed the termination shock (2007.66) reaching a maximum between 2007.75 and 2008.0. A series of 42/21 day periodicities was observed at V2 along with spectral changes of low energy TSP and the acceleration of 6-14 MeV electrons. Evidence is presented for the acceleration of TSP and electrons at the times of the 42/21 day periodicities just after V2 crossed the HTS. Spectra for TSP between 2-20 MeV and electrons between 2.5-14 MeV are derived for three time periods including the time of the HTS crossing. The energy spectra of TSP and electrons at these times of intensity peaks are very similar above ~3 MeV, with exponents of a power law spectrum between -3.0 and -3.6. The ratio of TSP intensities to electron intensities at the same energy is ~500. The electron intensity peaks and minima are generally out of phase with those of nuclei by ~1/2 of a 42 day cycle. These charge dependent intensity differences and the large periodic intensity changes could provide new clues as to a possible acceleration mechanism
Dynamics of Atom-Field Entanglement from Exact Solutions: Towards Strong Coupling and Non-Markovian Regimes
We examine the dynamics of bipartite entanglement between a two-level atom
and the electromagnetic field. We treat the Jaynes-Cummings model with a single
field mode and examine in detail the exact time evolution of entanglement,
including cases where the atomic state is initially mixed and the atomic
transition is detuned from resonance. We then explore the effects of other
nearby modes by calculating the exact time evolution of entanglement in more
complex systems with two, three, and five field modes. For these cases we can
obtain exact solutions which include the strong coupling regimes. Finally, we
consider the entanglement of a two-level atom with the infinite collection of
modes present in the intracavity field of a Fabre-Perot cavity. In contrast to
the usual treatment of atom-field interactions with a continuum of modes using
the Born-Markov approximation, our treatment in all cases describes the full
non-Markovian dynamics of the atomic subsystem. Only when an analytic
expression for the infinite mode case is desired do we need to make a weak
coupling assumption which at long times approximates Markovian dynamics.Comment: 12 pages, 5 figures; minor changes in grammar, wording, and
formatting. One unnecessary figure removed. Figure number revised (no longer
counts subfigures separately
Monitoring Supergiant Fast X-ray Transients with Swift. Results from the first year
Swift has allowed the possibility to give Supergiant Fast X-ray Transients
(SFXTs), the new class of High Mass X-ray Binaries discovered by INTEGRAL, non
serendipitous attention throughout all phases of their life. We present our
results based on the first year of intense Swift monitoring of four SFXTs, IGR
J16479-4514, XTE J1739-302, IGR J17544-2619 and AX J1841.0-0536. We obtain the
first assessment of how long each source spends in each state using a
systematic monitoring with a sensitive instrument. The duty-cycle of inactivity
is 17, 28, 39, 55% (5% uncertainty), for IGR J16479-4514, AX J1841.0-0536, XTE
J1739-302, and IGR J17544-2619, respectively, so that true quiescence is a rare
state. This demonstrates that these transients accrete matter throughout their
life at different rates. AX J1841.0-0536 is the only source which has not
undergone a bright outburst during our campaign. Although individual sources
behave somewhat differently, common X-ray characteristics of this class are
emerging such as outburst lengths well in excess of hours, with a multiple
peaked structure. A high dynamic range (including bright outbursts) of 4 orders
of magnitude has been observed. We performed out-of-outburst intensity-based
spectroscopy. Spectral fits with an absorbed blackbody always result in
blackbody radii of a few hundred meters, consistent with being emitted from a
small portion of the neutron star surface, very likely the neutron star polar
caps. We also present the UVOT data of these sources. (Abridged)Comment: Accepted for publication in MNRAS. 20 pages, 9 figures, 8 table
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