PLANET-B magnetic fields investigation

Yamamoto, T.; Matsuoka, A.

doi:10.1186/bf03352102

Cited by 13 publications

(8 citation statements)

References 22 publications

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“…2.1 Instrumentation LMAG, with a triaxial ring-core type fluxgate sensor (MGF-S), was designed on the basis of magnetometers of two previous missions, Geotail (Kokubun et al 1994) and Nozomi (Yamamoto and Matsuoka 1998). The noise level of peak-to-peak is less than 0.1 nT, and basic specification of LMAG is summarized in Table 1. MGF-S has four dynamic ranges of ±64, ±256, ±1024 and ±65536 nT with a resolution of 16 bits and a linearity better than 0.1% .…”

Section: Instrumentation and Calibrationmentioning

confidence: 99%

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

et al. 2010

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The magnetic field around the Moon has been successfully observed at a nominal altitude of ∼100 km by the lunar magnetometer (LMAG) on the SELENE (Kaguya) spacecraft in a polar orbit since October 29, 2007. The LMAG mission has three main objectives:(1) mapping the magnetic anomaly of the Moon, (2) measuring the electromagnetic and plasma environment around the Moon and (3) estimating the electrical conductivity structure of the Moon. Here we review the instrumentation and calibration of LMAG and report the initial global mapping of the lunar magnetic anomaly at the nominal altitude. We have applied a new de-trending technique of the Bayesian procedure to multiple-orbit datasets observed in the tail lobe and in the lunar wake. Based on the nominal observation of 14 months, global maps of lunar magnetic anomalies are obtained with 95% coverage of the lunar surface. After altitude normalization and interpolation of the magnetic anomaly field by an inverse boundary value problem, we obtained full-coverage maps of the vector magnetic field at 100 km altitude and the radial component distribution on the surface. Relatively strong anomalies are identified in several basin-antipode regions and several near-basin and near-crater regions, while the youngest basin on the Moon, the Orientale basin, has no magnetic anomaly. These features well agree with characteristics of previous maps based on the 220 H. Tsunakawa et al.Lunar Prospector observation. Relatively weak anomalies are distributed over most of the lunar surface. The surface radial-component distribution estimated from the inverse boundary value problem in the present study shows a good correlation with the radial component distribution at 30 km altitude by Lunar Prospector. Thus these weak anomalies over the lunar surface are not artifacts but likely to be originated from the lunar crustal magnetism, suggesting possible existence of an ancient global magnetic field such as a dynamo field of the early Moon. The possibility of the early lunar dynamo and the mechanism of magnetization acquisition will be investigated by a further study using the low-altitude data of the magnetic field by Kaguya.

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Section: Instrumentation and Calibrationmentioning

confidence: 99%

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

et al. 2010

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“…The MAST for Arase has nearly the same design as that for Nozomi (Yamamoto and Matsuoka 1998) and is similar to those used for Geotail (Kokubun et al 1994), Kaguya (Tsunakawa et al 2010), and BepiColombo MMO, except for the diameter, length, and material used. The MAST was in the stowed configuration at launch, and was deployed about 1 month after launch.…”

Section: -M Extendable Mastmentioning

confidence: 93%

“…The analogtype magnetometer follows the basic design adopted for many space missions (Gordon and Brown 1972;Fukunishi et al 1990;Kokubun et al 1994;Yamamoto and Matsuoka 1998;Tsunakawa et al 2010). Nevertheless, some elements of the sensor and electronics were newly developed to withstand the harsh radiation environment of Mercury (Matsuoka et al 2013).…”

Section: Overviewmentioning

confidence: 99%

The ARASE (ERG) magnetic field investigation

Matsuoka

Teramoto

Nomura

et al. 2018

Earth Planets Space

142

156

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The fluxgate magnetometer for the Arase (ERG) spacecraft mission was built to investigate particle acceleration processes in the inner magnetosphere. Precise measurements of the field intensity and direction are essential in studying the motion of particles, the properties of waves interacting with the particles, and magnetic field variations induced by electric currents. By observing temporal field variations, we will more deeply understand magnetohydrodynamic and electromagnetic ion-cyclotron waves in the ultra-low-frequency range, which can cause production and loss of relativistic electrons and ring-current particles. The hardware and software designs of the Magnetic Field Experiment (MGF) were optimized to meet the requirements for studying these phenomena. The MGF makes measurements at a sampling rate of 256 vectors/s, and the data are averaged onboard to fit the telemetry budget. The magnetometer switches the dynamic range between ± 8000 and ± 60,000 nT, depending on the local magnetic field intensity. The experiment is calibrated by preflight tests and through analysis of in-orbit data. MGF data are edited into files with a common data file format, archived on a data server, and made available to the science community. Magnetic field observation by the MGF will significantly improve our knowledge of the growth and decay of radiation belts and ring currents, as well as the dynamics of geospace storms.

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“…We also used interplanetary magnetic field (IMF) data. Details of the magnetometer on board Nozomi are described in Yamamoto and Matsuoka (1998). Figure 1 shows the Nozomi orbit projected to the ecliptic plane, where the EarthSun line is fixed in the coordinate.…”

Section: Observationsmentioning

confidence: 99%

A Study of Correlation between Solar Wind Data Observed at Two Points in Interplanetary Space During the Recent Solar Maximum

et al. 2005

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Identifying co-rotating structures in solar wind enables us to predict solar wind variation at the Earth and, hence, geomagnetic disturbances. However, co-rotating structures during solar maximum are sometimes difficult to see. We correlated solar wind data obtained by two spacecraft, Nozomi heading towards Mars and ACE at the L1 point, from late 1999 through early 2002. There were intervals when the solar wind showed specific co-rotating structures even in the midst of the solar maximum, whereas no correlation was found during the other intervals. The coefficient was generally higher between Nozomi and ACE than for the 27-day recurrence at ACE, while there was some correlation, especially when the difference in longitude between the two spacecraft was less than 120 • . Although frequency of occurrence of CMEs is partly responsible for the correlation, the results can be interpreted in terms of rapid changes in co-rotating high-speed streams from near-equatorial coronal holes at the solar maximum.

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PLANET-B magnetic fields investigation

Cited by 13 publications

References 22 publications

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

Lunar Magnetic Field Observation and Initial Global Mapping of Lunar Magnetic Anomalies by MAP-LMAG Onboard SELENE (Kaguya)

The ARASE (ERG) magnetic field investigation

A Study of Correlation between Solar Wind Data Observed at Two Points in Interplanetary Space During the Recent Solar Maximum

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