A new lunar absolute control point: established by images from the landing camera on Chang'e-3

The establishment of a lunar control network is one of the core tasks in selenodesy, in which defining an absolute control point on the Moon is the most important step. However, up to now, the number of absolute control points has been very sparse. These absolute control points have mainly been lunar laser ranging retroreflectors, whose geographical location can be observed by observations on Earth and also identified in high resolution lunar satellite images. The Chang'e-3(CE-3) probe successfully landed on the Moon, and its geographical location has been monitored by an observing station on Earth. Since its positional accuracy is expected to reach the meter level, the CE-3 landing site can become a new high precision absolute control point. We use a sequence of images taken from the landing camera, as well as satellite images taken by CE-1 and CE-2, to identify the location of the CE-3 lander. With its geographical location known, the CE-3 landing site can be established as a new absolute control point, which will effectively expand the current area of the lunar absolute control network by 22%, and can greatly facilitate future research in the field of lunar surveying and mapping, as well as selenodesy.     

Data processing and initial results from the CE-3 Extreme Ultraviolet Camera

The Extreme Ultraviolet Camera(EUVC) onboard the Chang'e-3(CE-3)lander is used to observe the structure and dynamics of Earth's plasmasphere from the Moon. By detecting the resonance line emission of helium ions(He+) at 30.4 nm, the EUVC images the entire plasmasphere with a time resolution of 10 min and a spatial resolution of about 0.1 Earth radius(RE) in a single frame. We first present details about the data processing from EUVC and the data acquisition in the commissioning phase, and then report some initial results, which reflect the basic features of the plasmasphere well. The photon count and emission intensity of EUVC are consistent with previous observations and models, which indicate that the EUVC works normally and can provide high quality data for future studies.     

基于程函方程与三维速度模型的中国东北地区地幔过渡带接收函数研究

本文利用中国东北地区NECESSArray记录到的45505条接收函数,结合该区域最新三维速度模型,采用快速行进法求解程函方程,计算了P-S转换波相对走时,并通过共转换点叠加成像方法获得了该地区下方地幔间断面起伏情况.结果显示,在长白山—五大连池连线一带东西约300 km,南北约900 km的狭长形区域内,660-km间断面下陷幅度达20~40 km.其结构可细分为南北两部分,南部更为狭窄且与日本海沟走向一致,对应于从日本海沟俯冲的太平洋板块在地幔过渡带的滞留区;北部对应于从千岛海沟俯冲的太平洋板块在地幔过渡带的滞留区.同时,在长白山西部,存在与长白山—五大连池下陷区形状类似的南北向狭长形抬升区,660-km间断面抬升幅度约为10 km,显示俯冲太平洋板块只延伸至松辽盆地东侧;而在盆地西侧,660-km间断面的下陷区可能与该地区岩石圈拆沉有关.同时,410-km间断面在松辽盆地—渤海一带,以及长白山火山西南和东北方向存在明显的下陷区;另外,在阿巴嘎及阿尔山也有小范围的下陷区.所有这些下陷区,均与地表新生代火山活动区/拉伸区有很好的对应关系,表明这些地表构造与深部热物质上涌有关.

     

基于耳石微化学的东海大黄鱼洄游路线推测

近年来,东海频现对大黄鱼（Larimichthys crocea）大网捕获（吨级规模以上）,引起了对衰退中的野生大黄鱼资源保护的担忧。为查明东海野生大黄鱼洄游规律,本文根据2020−2022年在浙江近海产卵场和外海越冬场采集的不同批次野生大黄鱼样本,利用激光剥蚀电感耦合等离子体质谱法（LA-ICP-MS）测定耳石微化学元素,结合聚类分析和主成分分析（PCA）,对不同大黄鱼群体进行了划分,结合耳石的年轮特征,研究大黄鱼群体的栖息生境,推测大黄鱼洄游路线。结果表明,Ba/Ca $\leqslant$0.004 2时可以判定为海洋栖息生境,Ba/Ca $\geqslant$ 0 .008 1时可以判定为河口栖息生境,0.004 2 < Ba/Ca< 0.008 1时可以判定为混合栖息生境。根据该阈值范围,判定本次采样的大黄鱼的5种生境类型：（1）近海产卵,近海混合水域短暂栖息类型（占22.2%）;（2）近海产卵,阶段性往复混合生境栖息类型（占15.6%）;（3）近海产卵,河口水域育幼索饵,外海越冬栖息类型（31.1%）;（4）河口产卵、混合水域育幼,外海越冬栖息类型（6.7%）;（5）近海混合水域短暂产卵,绝大部分时间海洋生境栖息类型（24.4%）。对所有样本的Ba/Ca核心、峰值和边缘值进行PCA,5种栖息类型的样本均匀分布在第一轴的两侧,大部分时间都在海洋生境中的G1、G2和G5,以及受陆源影响较大的G3和G4。同时,PCA结果同时也显示,5种类型样本均会近同步地在近海岛礁处出现,这表明外海、近海和河口的群体由于洄游等因素的影响会出现混合,说明了舟山岛礁水域对大黄鱼产卵育幼的重要性。本研究为东海大黄鱼近海产卵场、索饵场和外海越冬场之间洄游履历,以及大黄鱼洄游路线推测提供一定依据。     

SOHM-4与MHM-2010氢原子频标的特点比较

基于对已投入国家授时中心守时运转的SOHM-4型与MHM-2010型氢原子频标的长期关注,对这两种氢原子频标的性能作了较详细的比较和分析。讨论了它们共同的优点、各自的特长和不足之处,还给出了稳定度的测试结果。     

The causality between the rapid rotation of a sunspot and an X3.4 flare

Using multi-wavelength data of Hinode, the rapid rotation of a sunspot in ac-tive region NOAA 10930 is studied in detail. We found extraordinary counterclockwise rotation of the sunspot with positive polarity before an X3.4 flare. From a series of vector magnetograms, it is found that magnetic force lines are highly sheared along the neu-tral line accompanying the sunspot rotation. Furthermore, it is also found that sheared loops and an inverse S-shaped magnetic loop in the corona formed gradually after the sunspot rotation. The X3.4 flare can be reasonably regarded as a result of this movement. A detailed analysis provides evidence that sunspot rotation leads to magnetic field linestwisting in the photosphere. The twist is then transported into the corona and triggers flares.     

Sensitive response of desert vegetation to moisture change based on a near-annual resolution pollen record from Gahai Lake in the Qaidam Basin, northwest China

We present a 50-year pollen record at near-annual resolution from Gahai Lake in the Qaidam Basin on the northeastern Tibetan Plateau. Chronology of a 22-cm short core was established by ²¹⁰Pb and ¹³⁷Cs analysis. The pollen results at 0.5 cm intervals show large changes in Artemisia/Chenopodiaceae (A/C) ratios from < 0.2 to 0.95 in the last 50 years. High (low) A/C ratios represent increase (decrease) in steppe pollen production, which correspond to high (low) relative humidity observed at nearby Delingha weather station. On the basis of good correspondence with instrumental records and carbonate content from Gahai Lake, we conclude that A/C ratio is sensitive to moisture change and can be a very useful index in reconstructing paleoclimate of arid regions. Comparison with pollen and snow accumulation data from Dunde ice core suggests that effective moisture at low and high elevations shows the opposite relationship when mountain precipitation was extremely high, possibly due to topography-induced uplifting and subsiding air dynamics.     

Solar Radio Spikes in 2.6 – 3.8 GHz during the 13 December 2006 Event

On 13 December 2006, some unusual radio bursts in the range 2.6?–?3.8 GHz were observed during an X3.4 flare/CME event from 02:30 to 04:30 UT in active region NOAA 10930 (S06W27) with the digital spectrometers of the National Astronomical Observatories of China (NAOC). During this event many spikes were detected with the high temporal resolution of 8 ms and high frequency resolution of 10 MHz. Many of them were found to have complex structures associated with other radio burst types. The new observational features may reflect certain emission signatures of the electron acceleration site. In this paper, we present the results of the analysis of the new observational features of the complex spikes. According to the observed properties of the spikes, we identify five classes. Their observational parameters, such as duration, bandwidth, and relative bandwidth, were determined. Most spikes had negative polarization, but spikes with positive polarization were observed during a short time interval and were identified as a separate class. Based on the analysis of observations with Hinode/SOT (Solar Optical Telescope) we suggest that the sources of the spikes with opposite polarizations were different. Combined observations of spikes and fiber bursts are used to estimate the magnetic field strength in the source.     

Correction of the temperature effect in calibration of a solar radio telescope

This work analyzes the annual fluctuation of the observation data of the Mingantu Solar radio Telescope(MST) in S, C and X bands. It is found that the data vary with local air temperature as the logarithmic attenuation of equipment increases with temperature and frequency. A simplified and effective calibration method is proposed, which is used to calibrate the MST data in 2018–2020, while the correction coefficients are calculated from data in 2018–2019. For S, C and X bands, the root mean square errors of one polarization are 2.7, 5.7 and 20 sfu, and the relative errors are 4%, 6% and 8% respectively. The calibration of MUSER and SBRS spectra is also performed. The relative errors of MUSER at 1700 MHz,SBRS at 2800 MHz, 3050 MHz and 3350 MHz are 8%, 8%, 11% and 10% respectively. We found that several factors may affect the calibration accuracy, especially at X-band. The method is expected to work for other radio telescopes with similar design.     

The improvement of the one-dimensional Mellor-Yamada and K-profile parameterization turbulence schemes with the non-breaking surface wave-induced verticalmixing

Both the level 2.5 Mellor-Yamada turbulence closure scheme(MY) and K-profile parameterization(KPP) are popularly used by the ocean modeling community.The MY and the KPP are improved through including the non-breaking surface wave-induced vertical mixing(Bv),and the improved schemes were tested by using continuous data at the Papa ocean weather station(OWS) during 1961–1965.The numerical results showed that the Bv can make the temperature simulations fit much better with the continuous data from Papa Station.The two improved schemes overcame the shortcomings of predicting too shallow upper mixed layer depth and consequently overheated sea surface temperature during summertime,which are in fact common problems for all turbulence closure models.Statistical analysis showed that the Bv effectively reduced the mean absolute error and root mean square error of the upper layer temperature and increased the correlation coefficient between simulation and the observation.Furthermore,the performance of vertical mixing induced by shear instability and the Bv is also compared.Both the temperature structure and its seasonal cycle significantly improved by including the Bv,regardless of whether shear instability was included or not,especially for the KPP mixing scheme,which suggested that Bv played a dominant role in the upper ocean where the mean current was relatively weak,such as at Papa Station.These results may provide a clue to improve ocean circulation models.