Jinsong Ping

Regional ionosphere map over Japanese Islands

Based on the high time and spatial resolution total electron content (TEC) data, which is estimated from the phase and code observables obtained by using GPS (Global Positioning System) Earth Observation Network (GEONET), the TEC distribution and its time variation over Japanese Islands are scaled into 0.5° × 0.5° grid data for each 10 minutes. The TEC daily map time series are arranged in an array to show the TEC evolution. Based on the spherical harmonics expansion of global ionospheric TEC model (GIM), which is estimated from global GPS observation, the TEC maps are expanded firstly through as high as 60 degrees and orders for a spherical harmonic function as a regional ionosphere map (RIM). The evolution history of medium scale traveling ionospheric disturbances (MSTIDs), i.e. polarward intense TEC enhancement and pre-noon rapid irregular fluctuations near the geomagnetic equator, are identified and confirmed in a quiet geomagnetic period.

Same-beam VLBI observations of SELENE for improving lunar gravity field model

The Japanese lunar mission, Selenological and Engineering Explorer (Kaguya), which was successfully launched on 14 September 2007, consists of a main satellite and two small satellites, Rstar and Vstar. Same-beam very long baseline interferometry (VLBI) observations of Rstar and Vstar were performed for 15.4 months from November 2007 to February 2009 using eight VLBI stations. In 2008, S band same-beam VLBI observations totaling 476 h on 179 days were undertaken. The differential phase delays were successfully estimated for most ( about 85%) of the same-beam VLBI observation periods. The high success rate was mainly due to the continuous data series measuring the differential correlation phase between Rstar and Vstar. The intrinsic measurement error in the differential phase delay was less than 1 mm RMS for small separation angles and increased to approximately 2.5 mm RMS for the largest separation angles ( up to 0.56 deg). The long-term atmospheric and ionospheric delays along the line of sight were reduced to a low level ( several tens of milimeters) using the same-beam VLBI observations, and further improved through application of GPS techniques. Combining the eight-station ( four Japanese telescopes of VLBI Exploration of Radio Astrometry and four international telescopes) S band same-beam VLBI data with Doppler and range data, the accuracy of the orbit determination was improved from a level of several tens of meters when only using Doppler and range data to a level of 10 m. As a preliminary test of the technique, the coefficient sigma degree variance of the lunar gravity field was compared with and without 4 months of VLBI data included. A significant reduction below around 10 deg ( especially for the second degree) was observed when the VLBI data were included. These observations confirm that the VLBI data contribute to improvements in the accuracy of the orbit determination and through this to the lunar gravity field model.

Validation of Jason-1 Nadir Ionosphere TEC Using GEONET

The Jason-1 dual-frequency nadir ionosphere Total Electron Content (TEC) for 10-day cycles 1–67 is validated using absolute TEC measured by Japans GPS Earth Observation Network (GEONET), or the GEONET Regional Ionosphere Map (RIM). The bias estimates (Jason–RIM) are small and statistically insignificant: 1.62 ± 9 TECu (TEC unit or 1016 electrons/m2, 1 TECu = 2.2 mm delay at Ku-band) and 0.73 ± 0.05 TECu, using the along-track difference and Gaussian distribution method, respectively. The bias estimates are –3.05 ± 10.44 TECu during daytime passes, and 0.02 ± 8.05 TECu during nighttime passes, respectively. When global Jason-1 TEC is compared with the Global Ionosphere Map (GIM) from the Center for Orbit Determination in Europe (or CODE) TEC, the bias (Jason–GIM) estimate is 0.68 ± 1.00 TECu, indicating Jason-1 ionosphere delay at Ku-band is longer than GIM by 3.1 mm, which is at present statistically insignificant. Significant zonal distributions of biases are found when the differences are projected into a sun-fixed geomagnetic reference frame. The observed biases range from –7 TECu (GIM larger by 15.4 mm) in the equatorial region, to +2 TECu in the Arctic region, and to +7 TECu in the Antarctica region, indicating significant geographical variations. This phenomena is primarily attributed to the uneven and poorly distributed global GPS stations particularly over ocean and near polar regions. Finally, when the Jason-1 and TOPEX/Poseidon (T/P) TECs were compared during Jason-1 cycles 1–67 (where cycles 1–21 represent the formation flight with T/P, cycles 22–67 represent the interleave orbits), the estimated bias is 1.42 ± 0.04 TECu. It is concluded that the offset between Jason/TOPEX and GPS (RIM or GIM) TECs is < 4 mm at Ku-band, which at present is negligible.

VLBI observation of narrow bandwidth signals from the spacecraft

We carried out a series of VLBI observations of Nozomi by using a dedicated narrow bandwidth VLBI system. The three carrier waves with frequency interval of 515 kHz were recorded in 3 channels of the system and correlated by a software method. As a result of the correlation, the residual fringe phases of the main carrier wave are obtained for every 1.3 seconds. We can also continuously track them for 100 minutes. The variation of the residual fringe phase is +/− 150 degrees. Moreover, we can derive succesively the group delay for every 100 seconds by using these three carrier waves. The RMS of the group delays is 13 nsec and its average is well accorded with the delay determined by the range and Doppler measurements within an error of 2 nsec. Consequently, we confirmed the validity of the narrow bandwidth VLBI system, and it could be expected that this system, in addition to range and Doppler measurements, can be applied to three-dimensional tracking of a spacecraft and the precise gravity measurement of the Moon and the planets.

New method of measuring phase characteristics of antenna using Doppler frequency measurement technique

This paper reports on a new method of measuring the phase characteristics of an antenna using the Doppler frequency measurement technique. With this method, the antenna being tested is rotated at a rate of f/sub sp/ around an axis through its geometrical center, and the phase characteristics of the antenna are calculated from the harmonic components of f/sub sp/ during time variations in the Doppler frequency of radio waves emitted from the antenna. Using this, we obtained three-dimensional phase characteristics of a patch antenna with a root-mean-square error of about 0.5/spl deg/, and confirmed its efficacy through experimental results.

A degree 180 spherical harmonic model for the lunar topography

Using multiple step least squares fitting method and 0.25° gridded altimetry data (http://pds-geophys.wustl.edu/pds) from Clementine, a lunar topography model, NLT180A, is determined complete to spherical harmone degree (n) 180 This model is compared with the GLTM2 model (70x70) and shows good agreement for the long-wavelength component (longer than n=70).Other important parameters, including the offset between the center of figure (COF) and the center of mass (COM) of the Moon, and the topographical flattening of the Moon, have also been estimated. The estimates are similar to those obtained by other researchers. Possibility to obtain higher (than n=180) degree spherical harmonic model from the Clementine gridded data is discussed.Based on NLT180A, the lunar Moho topography and crustal thickness are estimated by assuming a traditional single layered crust on the top of Moho. The method used in this article will benefit the research of the future lunar mission, SELENE (SELenological and ENgineering Explorer).

Same-beam VLBI observation of SELENE

The Japanese lunar mission, SELENE (Kaguya) consists of a main satellite and two small satellites, Rstar and Vstar. In same-beam VLBI observations of Rstar and Vstar, phase fluctuations caused by atmosphere, ionosphere and instruments were reduced to a low level of 1–2 deg, and the differential phase delay between Rstar and Vstar was obtained with a very low error of 2 pico-seconds. We corrected the long-term atmospheric and ionospheric delays by using GPS techniques and analyzed other possible influence such as phase-frequency characteristic of the receivers and phase variation in the main beam of telescopes. We performed orbit determination for Rstar and Vstar, the accuracy was much improved from a few tens meters when using only Doppler and range data, to a level of about 10 m when same-beam VLBI data are also used. In addition, the lunar gravity field model was also improved by combing VLBI data.

Three-way Doppler observation of Mars Express

Using the radio telescopes in Chinese VLBI Net (CVN) and the sampling board, we have developed algorithms that extract three-way Doppler information from the radio tracking data of Mars Express (MEX) — a Martian probe that belongs to European Space Agency (ESA). Our latest results indicate the accuracy of three-way Doppler is about 1mm/s in 1 second integration time, relative to an 8.4GHz carrier. The three-way Doppler data have been used in orbit determination of Mars Express.

Open loop doppler tracking in Chinese forthcoming Mars mission

Using the radio telescopes in Chinese VLBI Network and the K5/VSSP32 VLBI system of NICT in Japan, we have developed algorithms that can extract open loop Doppler information from the Chang’E-1 and Mars Express radio tracking data. Our latest results indicate the Doppler accuracy of open loop three-way Doppler is about 1mm/s in 1 second integration time, relative to a 8.4GHz carrier. In the forthcoming joint Russian-Chinese Martian mission in 2009, the current software algorithms and hardware performance will be improved, and we will attempt to use the high precision Doppler shift and phase information to test gravitation theories.