557 research outputs found
LOKUSI, ILOKUSI, DAN PERLOKUSI DALAM IKLAN JEPANG TOYOTOWN 「トヨタウンコマーシャルメッセージの発話行為、発話内行為、 発話媒介行為」
ABSTRACT
Putri, Mariska Tiara. “Locution, Illocution, and Perlocution in Japanese Commercial Message, Toyotown”. Thesis Department of Japanese Studies of Faculty of Humanities Diponegoro University. The first advisor is Reny Wiyatasari, SS, M.Hum. The second advisor is Maharani P, Ratna, SS, M.Hum.
This research examines about what kind of locution, illocution, and perlocution that appear in Toyotown commercial message.
This research uses 5 commercial message and found 41 data that has a locution, illocution, and perlocution in it. There are 4 illocution categories that found in the data. They are assertive, directive, expressive, and commisive. Also, the perlocution verbs in the data are persuade, amuse, encourage, get someone to do something, bring someone to learn something, relieve tension, and distract.
Keywords : locution, illocution, perlocution
Observation and Modeling of Coronal "Moss" With the EUV Imaging Spectrometer on Hinode
Observations of transition region emission in solar active regions represent
a powerful tool for determining the properties of hot coronal loops. In this
Letter we present the analysis of new observations of active region moss taken
with the Extreme Ultraviolet Imaging Spectrometer (EIS) on the \textit{Hinode}
mission. We find that the intensities predicted by steady, uniformly heated
loop models are too intense relative to the observations, consistent with
previous work. To bring the model into agreement with the observations a
filling factor of about 16% is required. Furthermore, our analysis indicates
that the filling factor in the moss is nonuniform and varies inversely with the
loop pressure
Relationship between non-thermal electron energy spectra and GOES classes
We investigate the influence of the variations of energy spectrum of
non-thermal electrons on the resulting GOES classes of solar flares. Twelve
observed flares with various soft to hard X-ray emission ratios were modelled
using different non-thermal electron energy distributions. Initial values of
the flare physical parameters including geometrical properties were estimated
using observations. We found that, for a fixed total energy of non-thermal
electrons in a flare, the resulting GOES class of the flare can be changed
significantly by varying the spectral index and low energy cut-off of the
non-thermal electron distribution. Thus, the GOES class of a flare depends not
only on the total non-thermal electrons energy but also on the electron beam
parameters. For example, we were able to convert a M2.7 class solar flare into
a merely C1.4 class one and a B8.1 class event into a C2.6 class flare. The
results of our work also suggest that the level of correlation between the
cumulative time integral of HXR and SXR fluxes can depend on the considered HXR
energy range.Comment: 8 pages, 5 figures, Astronomy and Astrophysics (accepted, March 2009
Hinode EUV Imaging Spectrometer Observations of Solar Active Region Dynamics
The EUV Imaging Spectrometer (EIS) on the Hinode satellite is capable of
measuring emission line center positions for Gaussian line profiles to a
fraction of a spectral pixel, resulting in relative solar Doppler-shift
measurements with an accuracy of less than a km/s for strong lines. We show an
example of the application of that capability to an active region sit-and-stare
observation in which the EIS slit is placed at one location on the Sun and many
exposures are taken while the spacecraft tracking keeps the same solar location
within the slit. For the active region examined (NOAA 10930), we find that
significant intensity and Doppler-shift fluctuations as a function of time are
present at a number of locations. These fluctuations appear to be similar to
those observed in high-temperature emission lines with other space-borne
spectroscopic instruments. With its increased sensitivity over earlier
spectrometers and its ability to image many emission lines simultaneously, EIS
should provide significant new constraints on Doppler-shift oscillations in the
corona.Comment: 7 Pages, 7 figure
Temporal variations of the CaXIX spectra in solar flares
Standard model of solar flares comprises a bulk expansion and rise of
abruptly heated plasma (the chromospheric evaporation). Emission from plasma
ascending along loops rooted on the visible solar disk should be often
dominated, at least temporally, by a blue-shifted emission. However, there is
only a very limited number of published observations of solar flares having
spectra in which the blue-shifted component dominates the stationary one. In
this work we compare observed X-ray spectra of three solar flares recorded
during their impulsive phases and relevant synthetic spectra calculated using
one-dimensional hydro-dynamic numerical model of these flares. The main aim of
the work was to explain why numerous flares do not show blue-shifted spectra.
The synthesized BCS spectra of the flares were compared with the relevant
observed BCS spectra. We conclude that stationary component of the spectrum
should be observed almost for all flares during their early phases of
evolution. In opposite, the blue-shifted component of the spectrum could be not
detected in flares having plasma rising along the flaring loop even with high
velocity due to the geometrical dependences only. After the start of the
up-flow motion, the blue-shifted component dominate temporally the synthetic
spectra of the investigated flares at their early phases.Comment: 9 pages, 6 figures, Astronomy and Astrophysics (accepted, September
2009
Mean shear flows generated by nonlinear resonant Alfven waves
In the context of resonant absorption, nonlinearity has two different
manifestations. The first is the reduction in amplitude of perturbations around
the resonant point (wave energy absorption). The second is the generation of
mean shear flows outside the dissipative layer surrounding the resonant point.
Ruderman et al. [Phys. Plasmas 4, 75 (1997)] studied both these effects at the
slow resonance in isotropic plasmas. Clack et al. [Astron. Astrophys. 494}, 317
(2009)] investigated nonlinearity at the Alfven resonance, however, they did
not include the generation of mean shear flow. In this present paper, we
investigate the mean shear flow, analytically, and study its properties. We
find that the flow generated is parallel to the magnetic surfaces and has a
characteristic velocity proportional to , where is
the dimensionless amplitude of perturbations far away from the resonance. This
is, qualitatively, similar to the flow generated at the slow resonance. The
jumps in the derivatives of the parallel and perpendicular components of mean
shear flow across the dissipative layer are derived. We estimate the generated
mean shear flow to be of the order of in both the solar
upper chromosphere and solar corona, however, this value strongly depends on
the choice of boundary conditions. It is proposed that the generated mean shear
flow can produce a Kelvin--Helmholtz instability at the dissipative layer which
can create turbulent motions. This instability would be an additional effect,
as a Kelvin--Helmholtz instability may already exist due to the velocity field
of the resonant Alfven waves. This flow can also be superimposed onto existing
large scale motions in the solar upper atmosphere.Comment: 11 page
Comprehensive Determination of the Hinode/EIS Roll Angle
We present a new coalignment method for the EUV Imaging Spectrometer (EIS) on
board the Hinode spacecraft. In addition to the pointing offset and spacecraft
jitter, this method determines the roll angle of the instrument, which has
never been systematically measured, and is therefore usually not corrected. The
optimal pointing for EIS is computed by maximizing the cross-correlations of
the Fe XII 195.119 \r{A} line with images from the 193 \r{A} band of the
Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory
(SDO). By coaligning 3336 rasters with high signal-to-noise ratio, we estimate
the rotation angle between EIS and AIA and explore the distribution of its
values. We report an average value of (-0.387 0.007)\deg. We also provide
a software implementation of this method that can be used to coalign any EIS
raster.Comment: Accepted for publication in Solar Physics, 11 pages, 7 figure
Velocity measurements for a solar active region fan loop from Hinode/EIS observations
The velocity pattern of a fan loop structure within a solar active region
over the temperature range 0.15-1.5 MK is derived using data from the EUV
Imaging Spectrometer (EIS) on board the Hinode satellite. The loop is aligned
towards the observer's line-of-sight and shows downflows (redshifts) of around
15 km/s up to a temperature of 0.8 MK, but for temperatures of 1.0 MK and above
the measured velocity shifts are consistent with no net flow. This velocity
result applies over a projected spatial distance of 9 Mm and demonstrates that
the cooler, redshifted plasma is physically disconnected from the hotter,
stationary plasma. A scenario in which the fan loops consist of at least two
groups of "strands" - one cooler and downflowing, the other hotter and
stationary -- is suggested. The cooler strands may represent a later
evolutionary stage of the hotter strands. A density diagnostic of Mg VII was
used to show that the electron density at around 0.8 MK falls from 3.2 x 10^9
cm^-3 at the loop base, to 5.0 x 10^8 cm^-3 at a projected height of 15 Mm. A
filling factor of 0.2 is found at temperatures close to the formation
temperature of Mg VII (0.8 MK), confirming that the cooler, downflowing plasma
occupies only a fraction of the apparent loop volume. The fan loop is rooted
within a so-called "outflow region" that displays low intensity and blueshifts
of up to 25 km/s in Fe XII 195.12 A (formed at 1.5 MK), in contrast to the
loop's redshifts of 15 km/s at 0.8 MK. A new technique for obtaining an
absolute wavelength calibration for the EIS instrument is presented and an
instrumental effect, possibly related to a distorted point spread function,
that affects velocity measurements is identified.Comment: 42 pages, 15 figures, submitted to Ap
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