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Lost Apollo heat flow data suggest a different lunar bulk composition
Lunar surface heat flow values were measured on the Apollo missions between 1971 and 1977. However, the late-term data have been lost. We succeeded in archiving the data after March 1, 1976. We will introduce the new set of archived data
AKARI Mission Program: Excavating Mass Loss History in Extended Dust Shells of Evolved Stars (MLHES) I. Far-IR Photometry
We performed a far-IR imaging survey of the circumstellar dust shells of 144
evolved stars as a mission programme of the AKARI infrared astronomical
satellite using the Far-Infrared Surveyor (FIS) instrument. With this survey,
we deliver far-IR surface brightness distributions of roughly 10' x 40' or 10'
x 20' areas of the sky around the target evolved stars in the four FIS bands at
65, 90, 140, and 160 microns. Our objectives are to characterize the far-IR
surface brightness distributions of the cold dust component in the
circumstellar dust shells, from which we derive the amount of cold dust grains
as low as 20 K and empirically establish the history of the early mass loss
history. In this first installment of the series, we introduce the project and
its aims, describe the observations, data reduction, and surface brightness
correction process, and present the entire data set along with the results of
integrated photometry measurements (i.e., the central source and circumstellar
dust shell altogether). We find that (1) far-IR emission is detected from all
but one object at the spatial resolution about 30" - 50" in the corresponding
bands, (2) roughly 60 - 70 % of the target sources show some extension, (3)
previously unresolved nearby objects in the far-IR are now resolved around 28
target sources, (4) the results of photometry measurements are reasonable with
respect to the entries in the AKARI/FIS Bright Source Catalogue, despite the
fact that the targets are assumed to be point-sources when catalogue flux
densities were computed, and (5) an IR two-color diagram would place the target
sources in a roughly linear distribution that may correlate with the age of the
circumstellar dust shell and can potentially be used to identify which targets
are more extended than others.Comment: To be published in PASJ AKARI Special Issue: 25 pages, 5 figures, 5
tables (and 28 supplementary figures available only in PASJ on-line
Observation of an energetic radiation burst from mountain-top thunderclouds
During thunderstorms on 2008 September 20, a simultaneous detection of gamma
rays and electrons was made at a mountain observatory in Japan located 2770 m
above sea level. Both emissions, lasting 90 seconds, were associated with
thunderclouds rather than lightning. The photon spectrum, extending to 10 MeV,
can be interpreted as consisting of bremsstrahlung gamma rays arriving from a
source which is 60 - 130 m in distance at 90% confidence level. The observed
electrons are likely to be dominated by a primary population escaping from an
acceleration region in the clouds.Comment: 12 pages, 3 figures, accepted for publication in Physical Review
Letter
SOLAR CYCLE DEPENDENCE OF THE DIURNAL ANISOTROPY OF 0.6 TeV COSMIC-RAY INTENSITY OBSERVED WITH THE MATSUSHIRO UNDERGROUND MUON DETECTOR
We analyze the temporal variation of the diurnal anisotropy of sub-TeV cosmic-ray intensity observed with the Matsushiro (Japan) underground muon detector over two full solar activity cycles in 1985-2008. We find an anisotropy component in the solar diurnal anisotropy superimposed on the Compton-Getting anisotropy due to Earth's orbital motion around the Sun. The phase of this additional anisotropy is almost constant at similar to 15:00 local solar time corresponding to the direction perpendicular to the average interplanetary magnetic field at Earth's orbit, while the amplitude varies between a maximum (0.043% +/- 0.002%) and minimum (similar to 0.008% +/- 0.002%) in a clear correlation with the solar activity. We find a significant time lag between the temporal variations of the amplitude and the sunspot number (SSN) and obtain the best correlation coefficient of +0.74 with the SSN delayed for 26 months. We suggest that this anisotropy might be interpreted in terms of the energy change due to the solar-wind-induced electric field expected for galactic cosmic rays (GCRs) crossing the wavy neutral sheet. The average amplitude of the sidereal diurnal variation over the entire period is 0.034% +/- 0.003%, which is roughly one-third of the amplitude reported from air shower and deep-underground muon experiments monitoring multi-TeVGCR intensity suggesting a significant attenuation of the anisotropy due to the solar modulation. We find, on the other hand, only a weak positive correlation between the sidereal diurnal anisotropy and the solar activity cycle in which the amplitude in the "active" solar activity epoch is about twice the amplitude in the "quiet" solar activity epoch. This implies that only one-fourth of the total attenuation varies in correlation with the solar activity cycle and/or the solar magnetic cycle. We finally examine the temporal variation of the "single-band valley depth" (SBVD) quoted by the Milagro experiment and, in contrast with recent Milagro's report, we find no steady increase in the Matsushiro observations in a seven-year period between 2000 and 2007. We suggest, therefore, that the steady increase of the SBVD reported by the Milagro experiment is not caused by the decreasing solar modulation in the declining phase of the 23rd solar activity cycle.ArticleThe Astrophysical Journal. 712(2):1100-1106 (2010)journal articl
Scaling quantum computing with dynamic circuits
Quantum computers process information with the laws of quantum mechanics.
Current quantum hardware is noisy, can only store information for a short time,
and is limited to a few quantum bits, i.e., qubits, typically arranged in a
planar connectivity. However, many applications of quantum computing require
more connectivity than the planar lattice offered by the hardware on more
qubits than is available on a single quantum processing unit (QPU). Here we
overcome these limitations with error mitigated dynamic circuits and
circuit-cutting to create quantum states requiring a periodic connectivity
employing up to 142 qubits spanning multiple QPUs connected in real-time with a
classical link. In a dynamic circuit, quantum gates can be classically
controlled by the outcomes of mid-circuit measurements within run-time, i.e.,
within a fraction of the coherence time of the qubits. Our real-time classical
link allows us to apply a quantum gate on one QPU conditioned on the outcome of
a measurement on another QPU which enables a modular scaling of quantum
hardware. Furthermore, the error mitigated control-flow enhances qubit
connectivity and the instruction set of the hardware thus increasing the
versatility of our quantum computers. Dynamic circuits and quantum modularity
are thus key to scale quantum computers and make them useful
Interaction-induced shift of the cyclotron resonance of graphene using infrared spectroscopy
We report a study of the cyclotron resonance (CR) transitions to and from the
unusual Landau level (LL) in monolayer graphene. Unexpectedly, we find
the CR transition energy exhibits large (up to 10%) and non-monotonic shifts as
a function of the LL filling factor, with the energy being largest at
half-filling of the level. The magnitude of these shifts, and their
magnetic field dependence, suggests that an interaction-enhanced energy gap
opens in the level at high magnetic fields. Such interaction effects
normally have limited impact on the CR due to Kohn's theorem [W. Kohn, Phys.
Rev. {\bf 123}, 1242 (1961)], which does not apply in graphene as a consequence
of the underlying linear band structure.Comment: 4 pages, 4 figures. Version 2, edited for publication. Includes a
number of edits for clarity; also added a paragraph contrasting our work w/
previous CR expts. in 2D Si and GaA
Multiwavelength study of the high-latitude cloud L1642: chain of star formation
L1642 is one of the two high galactic latitude (|b| > 30deg) clouds confirmed
to have active star formation. We examine the properties of this cloud,
especially the large-scale structure, dust properties, and compact sources in
different stages of star formation. We present high-resolution far-infrared and
submm observations with the Herschel and AKARI satellites and mm observations
with the AzTEC/ASTE telescope, which we combined with archive data from near-
and mid-infrared (2MASS, WISE) to mm observations (Planck). The Herschel
observations, combined with other data, show a sequence of objects from a cold
clump to young stellar objects at different evolutionary stages. Source B-3
(2MASS J04351455-1414468) appears to be a YSO forming inside the L1642 cloud,
instead of a foreground brown dwarf, as previously classified. Herschel data
reveal striation in the diffuse dust emission around L1642. The western region
shows striation towards NE and has a steeper column density gradient on its
southern side. The densest central region has a bow-shock like structure
showing compression from the west and a filamentary tail extending towards
east. The differences suggest that these may be spatially distinct structures,
aligned only in projection. We derive values of the dust emission cross-section
per H nucleon for different regions of the cloud. Modified black-body fits to
the spectral energy distribution of Herschel and Planck data give emissivity
spectral index beta values 1.8-2.0 for the different regions. The compact
sources have lower beta values and show an anticorrelation between T and beta.
Markov chain Monte Carlo calculations demonstrate the strong anticorrelation
between beta and T errors and the importance of mm Planck data in constraining
the estimates. L1642 reveals a more complex structure and sequence of star
formation than previously known.Comment: 22 pages, 18 figures, accepted to Astronomy & Astrophysics; abstract
shortened and figures reduced for astrop
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