PROTEIN AND CARBOHYDRATE IN P-POM COLLECTED FROM THE FISHING GROUND IN MINNAN-TAIWAN BANK     

苏永全  张寰 《中国海洋湖沼学报》1992,10(2):145-152

The analysis of the protein and carbohydrate in P-POM (Plankton and Particulate Organic Matter) samples collected from the fishing ground in Minnan-Taiwan Bank in five voyages (April, June, July, August and November, 1988) shows that the protein and carbohydrate contents and amounts in samples from four stations (501, 401, 301, 201) along the coast and another four stations (404, 304, 403, 204) south and southeast of the shoal were higher than those in April and November, indicating that this phenomenon is related to the upwelling in the two regions in summer .  相似文献   

Evalution on nutritive value ofPortunus trituberculatus     

Su Xiu-rong  Li Tai-wu  Ding Ming-jin  Paul K. Chien 《中国海洋湖沼学报》1997,15(2):168-172

This study on the nutritive indexes (total nitrogen, amino acids, crude fats, inorganic elements, unsaturated fatty acids) of meat, male and female reproductive gland ofPortunus trituberculatus showed that their nutritive value is in the order meat>female reproductive gland>male reproductive gland and that they do not raise the total cholesterol (TC) and triglyceride (TG) contents of the serum of the animals which eat them but increase the contents of high density lipoprotein cholesterol (HDL-C) in the animal's blood. These findings implied that people who have high blood lipid and aortic atheroma can safely use them as food. This study showed thatP. trituberculatus has high nutritive value.  相似文献   

Observation of Interactions and Eruptions of Two Filaments     

Jiangtao Su  Yu Liu  Hiroki Kurokawa  Xinjie Mao  Shangbin Yang  Hongqi Zhang  Haimin Wang 《Solar physics》2007,242(1-2):53-63

We present new observations of the interactions of two close, but distinct, Hα filaments and their successive eruptions on 5 November 1998. The magnetic fields of the filaments are both of the sinistral type. The interactions between the two filaments were initiated mainly by an active filament of one of them. Before the filament eruptions, two dark plasma ejections and chromospheric brightenings were observed. They indicate that possible magnetic reconnection had occurred between the two filaments. During the first filament eruption, salient dark mass motions transferring from the left erupting filament into the right one were observed. The right filament erupted 40 minutes later. This second filament eruption may have been the result of a loss of stability owing to the sudden mass injection from the left filament. Based on the Hα observations, we have created a sketch for understanding the interactions between two filaments and accompanying activities. The traditional theory of filament merger requires that the filaments share the same filament channel and that the reconnection occurs between the two heads, as simulated by DeVore, Antiochos, and Aulanier (Astrophys. J. 629, 1122, 2005; 646, 1349, 2006). Our interpretation is that the external bodily magnetic reconnection between flux ropes of the same chirality is another possible way for two filament bodies to coalesce. Electronic Supplementary Material The online version of this article () contains supplementary material, which is available to authorized users.  相似文献   

八庙—青山金红石矿床金红石特征及成因     

徐少康  苏茵  周希贤  李博昀  刘振山 《河南国土资源》1997,(4)

本文论述了金红石的地质产状、化学成分、粒度的概率分布、红外光谱、Ｘ射线衍射等特征及金红石成因，对本矿床成因研究及开发利用有一定意义。  相似文献   

Non-isothermal atmosphere,solar wind,shearing and pressing magnetic field and preflare loops     

Su Qing-Rui 《Solar physics》1990,127(1):139-147

Using a finite elements method, the magnetohydrostatic equation in a non-isothermal atmosphere is solved. The result is similar to the case in an isothermal atmosphere (Su, 1985). It is found that at some critical amount of shearing a magnetic island is formed and then breaks out to form an open magnetic configuration in which tearing-mode instability may occur. As the gradient of longitudinal magnetic field at some lower solar corona level increases, shearing loops containing strong currents are formed and the critical magnetic shearing parameter at which the magnetic island occurs, gets larger. In such a case, a lot of magnetic free energy is not easily released. It may be accumulated in a small volume above the polarity inversion line. As magnetic shearing increases, the magnetic free energy gets larger, until the magnetic shearing parameter reaches a higher critical value, a sudden change in magnetic configuration occurs. Such conditions may lead to high-energy solar eruptive phenomenon.  相似文献   

PRIMARY STUDY OF SULFATE AND CARBONACEOUS AEROSOLS IN BEIJING     

Su Weihan  Zhang Qiupeng  Song Wenzhi  R. L. Do  R. D. Giauque  T. Novakov 《大气科学进展》1987,4(2):225-232

Results of our aerosol study, performed during 1983–1984 in Beijing, demonstrate that ambient carbonaceous aerosols are derived mainly from coal combustion. Different SO₂ oxidation processes have been observed in summer and winter. The winter sulfate appears to be produced locally and associated with products of incomplete combustion.  相似文献   

Polarization of loop-top and footpoint sources in microwave bursts     

Su  Y.N.  Huang  G.L. 《Solar physics》2004,219(1):159-168

The polarization is analyzed in four microwave bursts with one loop-top and two footpoint sources observed at 17 GHz with the Nobeyama Radioheliograph (NoRH). The loop-like structure of the four events is confirmed by simultaneous SOHO/MDI magnetograms and TRACE/EUV images or Yohkoh/SXT images. The heliocentric distance of the four events is greater than 30°. The three microwave sources in each given burst are polarized in the same sense. This may be interpreted in terms of extraordinary mode emission, taking into account the polarity of the underlying magnetic field and propagation effects, which may lead to inversion of the sense of polarization in the limbward foot and loop-top source of the flaring loop.  相似文献   

青海省大柴旦镇红柳沟金矿床地质特征及其成因     

吴正寿  邓元良  苏生顺 《青海国土经略》2001,(1)

通过对红柳沟金矿床地质特征及围岩蚀变的研究,总结了金矿控矿因素及其富集规律,认为该矿床的成因为动力变质热液型。  相似文献   

A One-Dimensional Relativistic Shock Model for the Light Curve of Gamma-ray Bursts     

Cheng-Yue Su  Yi-Ping Qin  Jun-Hui Fan  Zhang-Yu Han National Astronomical Observatories/Yunnan Observatory  Chinese Academy of Sciences  Kunming  Graduate School of Chinese Academy of Sciences  Beijing Department of Physics  Guangdong University of Technology  Guangzhou Center for Astrophysics  Guangzhou University  Guangzhou Department of Mechanics  University of Science  Technology of China  Hefei 《中国天文和天体物理学报》2006,6(3):323-330

We investigate the forming of gamma-ray burst pulses with a simple one-dimensional relativistic shock model. The mechanism is that a "central engine" drives forward the nearby plasma inside the fireball to generate a series of pressure waves. We give a relativistic geometric recurrence formula that connects the time when the pressure waves are produced and the time when the corresponding shocks occurred. This relation enables us to relate the pulse magnitude with the observation time. Our analysis shows that the evolution of the pressure waves leads to a fast rise and an exponential decay pulses. In determining the width of the pulses, the acceleration time is more important than that of the deceleration.  相似文献   

A Statistical Study of Rhessi Flares     

Yang Su  W. Q. Gan  Y. P. Li 《Solar physics》2006,238(1):61-72

A statistical analysis of RHESSI X-ray flares in the 12–25 keV band during the period from February 2002 to June 2005 is presented. We found that a power-law with an index of 1.80± 0.02 can fit well the frequency distribution of the peak count rates. This power-law does not change significantly with time. However, the frequency distribution of the flare durations cannot be fitted well by a single power-law. There is a weak correlation between the peak count rates and the characteristic times like rise times, decay times, or durations. But the correlation between the rise times and decay times seems to be strong. We discuss the results obtained and compare them with previous works. The frequency distribution of rise times for the sub-group events with a similar magnitude of peak count rates is also shown. In particular, we propose a new parameter R _a , the growth factor of the count rate, defined as the peak count rate divided by the rise time, to reflect the characteristics of the rising phases of flares. The distribution of R _a is shown and discussed.  相似文献