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1.
Spectro-polarimetric observations of active regions were carried out in the spectral lines of Sii 10827.1 Å and Hei 10830 Å to study the three-dimensional magnetic field structure and associated plasma flow properties. Comparison of Sii and Hei magnetograms with the potential field model shows that a large fraction of the magnetic field is consistent with the potential field structure, by assuming that the height difference between the origin of the two lines is about 1200 km. The slope of the scatter plot between Sii and Hei magnetograms is 0.5, 0.76 in an emerging flux and a larger active region, respectively. These values are lower than the scatter plot slopes obtained from Kitt Peak photospheric and chromospheric magnetograms, in which case the corresponding values are 0.83 and 0.9, respectively. Considering the height difference between these two sets of chromospheric magnetograms, this implies that the magnetic field spreads out faster near the transition region heights. Dopplergrams obtained by determining the centroid of the asymmetric line profiles show that, in case of emerging flux region, the chromospheric upflow regions are located in the magnetic neutral line areas. 相似文献
2.
We study nonthermal production of baryon and dark matter. If we extend the MSSM by introducing some singlet chiral superfields so as to enlarge the conserved global symmetry, the abundance of the baryon and the dark matter in the universe may be explained as the charge asymmetry of that symmetry. In such a case, the baryon energy density and the dark matter energy density in the present universe can be correlated each other and take the similar order values naturally. 相似文献
3.
Ocean Dynamics - A multi-decadal simulation of ocean circulation in the northern Gulf of Mexico produces strong submesoscale instabilities in the Mississippi/Atchafalaya plume fronts. The model... 相似文献
4.
B. W. Lites D. L. Akin G. Card T. Cruz D. W. Duncan C. G. Edwards D. F. Elmore C. Hoffmann Y. Katsukawa N. Katz M. Kubo K. Ichimoto T. Shimizu R. A. Shine K. V. Streander A. Suematsu T. D. Tarbell A. M. Title S. Tsuneta 《Solar physics》2013,283(2):579-599
The joint Japan/US/UK Hinode mission includes the first large-aperture visible-light solar telescope flown in space. One component of the Focal Plane Package of that telescope is a precision spectro-polarimeter designed to measure full Stokes spectra with the intent of using those spectra to infer the magnetic-field vector at high precision in the solar photosphere. This article describes the characteristics of the flight hardware of the Hinode Spectro-Polarimeter, and summarizes its in-flight performance. 相似文献
5.
Daijiro Kaneko Peng Yang Toshiro Kumakura 《Journal of the Indian Society of Remote Sensing》2011,39(3):297-306
A photosynthetic-sterility model for grain production monitoring has been developed and validated under the background of
climate change and Asian economic growth in developing countries. This paper presents an application of the model to evaluate
carbon-fixation rates in yields of paddy rice, winter wheat, and maize in Asia. The validation of the model is based on carbon
partitioning in grain plants. The carbon hydrate in grains has the same chemical formula as that of cellulose in grain vegetation.
The partitioning of carbon in plants can validate fixation amounts of computed carbon using a satellite-based photosynthesis
model. The model estimates the photosynthesis fixation of rice reasonably in Japan and China. Results were validated through
examination of carbon in grains, but the model tends to underestimate results for winter wheat and maize. This study also
provides daily distributions of the PSN, which is the CO2 fixation in Asian areas combined with a land-cover distribution classified from MODIS data, NDVI from SPOT VEGETATION, and
meteorological re-analysis data by European Centre for Medium-Range Forecasts (ECMWF). The mean CO2 and carbon fixation rates in paddy areas were 25.92 (t CO2/ha) and 5.28 (t C/ha) in Japan, respectively. Comparisons between the model’s values and MODIS seasonal PSNs show similar
trends. The writers are preparing to compare computed photosynthesis rates with observed AsiaFlux data for the validation
of this model at field sites of paddy, grassland and forests in Japan and Asian countries. 相似文献
6.
Kazunari Shibata Takara Nishikawa Reizaburo Kitai Yoshinori Suematsu 《Solar physics》1982,75(1-2):99-118
We present a spicule model whose eruption occurs as a result of the sudden pressure enhancement at the bright point located at the root of the spicule. To show this, one dimensional (constant cross sectional) and time dependent hydrodynamic equations are solved numerically in the realistic solar atmosphere extending from the photosphere to the corona. Adiabatic motion is assumed. The pressure enhancement by a bright point at the base of the model atmosphere generates a shock wave. The shock gets stronger as it passes upward through the chromosphere and eventually collides with the chromosphere-corona interface which is a kind of a contact discontinuity. As the result, the interface begins to move upward. We identify the matter following behind this interface as the solar spicule. The model explains many observed features, such as the height and the density of the spicules, although such features have been hitherto considered not to be explained easily by shock theories. 相似文献
7.
G. Giono R. Ishikawa N. Narukage R. Kano Y. Katsukawa M. Kubo S. Ishikawa T. Bando H. Hara Y. Suematsu A. Winebarger K. Kobayashi F. Auchère J. Trujillo Bueno S. Tsuneta T. Shimizu T. Sakao J. Cirtain P. Champey A. Asensio Ramos J. Štěpán L. Belluzzi R. Manso Sainz B. De Pontieu K. Ichimoto M. Carlsson R. Casini M. Goto 《Solar physics》2017,292(4):57
The Chromospheric Lyman-Alpha SpectroPolarimeter is a sounding rocket instrument designed to measure for the first time the linear polarization of the hydrogen Lyman-\({\upalpha }\) line (121.6 nm). The instrument was successfully launched on 3 September 2015 and observations were conducted at the solar disc center and close to the limb during the five-minutes flight. In this article, the disc center observations are used to provide an in-flight calibration of the instrument spurious polarization. The derived in-flight spurious polarization is consistent with the spurious polarization levels determined during the pre-flight calibration and a statistical analysis of the polarization fluctuations from solar origin is conducted to ensure a 0.014% precision on the spurious polarization. The combination of the pre-flight and the in-flight polarization calibrations provides a complete picture of the instrument response matrix, and a proper error transfer method is used to confirm the achieved polarization accuracy. As a result, the unprecedented 0.1% polarization accuracy of the instrument in the vacuum ultraviolet is ensured by the polarization calibration. 相似文献
8.
T. Kosugi K. Matsuzaki T. Sakao T. Shimizu Y. Sone S. Tachikawa T. Hashimoto K. Minesugi A. Ohnishi T. Yamada S. Tsuneta H. Hara K. Ichimoto Y. Suematsu M. Shimojo T. Watanabe S. Shimada J. M. Davis L. D. Hill J. K. Owens A. M. Title J. L. Culhane L. K. Harra G. A. Doschek L. Golub 《Solar physics》2007,243(1):3-17
The Hinode satellite (formerly Solar-B) of the Japan Aerospace Exploration Agency’s Institute of Space and Astronautical Science (ISAS/JAXA) was successfully launched
in September 2006. As the successor to the Yohkoh mission, it aims to understand how magnetic energy gets transferred from the photosphere to the upper atmosphere and results
in explosive energy releases. Hinode is an observatory style mission, with all the instruments being designed and built to work together to address the science
aims. There are three instruments onboard: the Solar Optical Telescope (SOT), the EUV Imaging Spectrometer (EIS), and the
X-Ray Telescope (XRT). This paper provides an overview of the mission, detailing the satellite, the scientific payload, and
operations. It will conclude with discussions on how the international science community can participate in the analysis of
the mission data.
T. Kosugi deceased 26 November 2006. 相似文献
9.
Y. Suematsu 《Astronomische Nachrichten》2010,331(6):605-608
Hinode is an observatory‐style satellite, carrying three advanced instruments being designed and built to work together to explore the physical coupling between the photosphere and the upper layers for understanding the mechanism of dynam‐ ics and heating. The three instruments aboard are the Solar Optical Telescope (SOT), which can provide high‐precision photometric and polarimetric data of the lower atmosphere in the visible light (388–668 nm) with a spatial resolution of 0.2–0.3 arcseconds, the X‐Ray Telescope (XRT) which takes a wide field of full sun coverage X‐ray images being capable of diagnosing the physical condition of coronal plasmas, and the EUV Imaging Spectrometer (EIS) which observes the upper transition region and coronal emission lines in the wavelength ranges of 17–21 nm and 25–29 nm. Since first‐light observations in the end of October 2006, Hinode has been continuously providing unprecedented high‐quality solar data. We will present some new findings of the sun with Hinode, focusing on those from SOT (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
10.
Yoshinori Suematsu 《Solar physics》1985,98(1):67-90
The formation of fibrils in low-lying loops is investigated by performing one-dimensional nonlinear hydrodynamic calculations. The loops have the height of 3000–5000 km and have an atmosphere extending from the photosphere to the corona. A shock wave is generated from a pressure pulse in the photosphere and it ejects the chromosphere-corona transition region along the loop, expanding the underlying chromosphere into the corona. This expanding chromospheric material in a loop is regarded as a fibril. The shock propagates in the corona and collides with another transition region where a reflected shock and a penetrating shock are generated. The effect of the reflected shock on the motion of the fibril is weak. The fibril shows a nearly ballistic motion as observations suggest, if it does not extend beyond the summit of the loop. The corona in the loop is compressed nearly adiabatically by the fibril, and the enhanced coronal pressure leads the fibril finally to a retracting motion even if the fibril goes beyond the summit of the loop.Contributions from the Kwasan and Hida Observatories, University of Kyoto, No. 261. 相似文献