User:Melaniejaime/sandbox
The Akebono satellite, also known as EXOS-D previous to its launch, is a satellite designed to study the Earth’s magnetosphere and aurora (polar lights). Akebono was developed by the Japanese national research organization of astrophysics: Institute of Space and Astronautical Science (ISAS) and was first launched on February 22, 1989. [1]The satellite operates through eight instruments on board as well as additional facilities to assist the operation of the instruments.
History
Origin
Termination
by the M-3SII-4 launch vehicle from the Uchinoura Space Center (USC).[2] [9]
into a semi-polar orbit with an inclination of 75°.The Akebono satellite has an initial perigee and apogee of 274 km and 10500km, respectively, with an orbital period of 212 minutes. This spacecraft is spinstabilized with a spin rate of 7.5 rpm and its spin axis is always directed toward the sun.
The expected target life of the satellite was a year, but remained in operation for over 26 years.[2] [9]
Akebono, meaning “the dawn”, is the fourth satellite within the EXOS series of satellites that were launched by ISAS to investigate the Earth’s upper atmosphere. [3][11] The satellite’s intention is dedicated to studying auroral particle acceleration as well as related over the polar region.[4][12] For maximum data coverage, four ground stations track Akebono’s path[3]11]:
- The Kagoshima Space Center (Japan)
- Esrange Space Center (Sweden)
- Prince Albert Satellite Station (Canada)
- Syowa station (Antarctica)
Components
The 8 instruments onboard the Akebono include:
Electric Field Detector (EFD)
The satellite includes two electric field detector systems, (EFD-B) and (EFD-P), which are utilized to measure both the static and quasi-static vector electric field though two techniques:standard double probe and ion beam, which was developed specifically for the Akebono satellite. The electric field has three components, through the standard double probe technique (EFD-P), the field is measured as the possible differences between three orthogonal (intersecting at right angles) pairs of sensors, the sensors are separated and later divided by the distance between their separation. [5][6]
Magnetic Field Detector (MGF)
Akebono carries both triaxial [three directions] search coil and triaxial fluxgate magnetometers [a device used to measure magnetic fields]. Fluxgate is mounted on a 5-m extendable mast and used for vector magnetic fields, collecting data at a 3,000-10,000 km altitude. Search coils are mounted at a on a 3-m extendable mast and measure low frequency magnetic field fluctuations and waves, the measurements are collected with a frequency response up to 800 Hz.[7][8]
Very Low Frequency Plasma Wave Detectors (VLF)
Plasma Wave Detectors in High Frequency Range and Sounder (PWS)
Low Energy Particle Spectra Analyzer (LEP)
Supra Thermal Mass Spectrometer (SMS)
Thermal Electron Detectors (TED)
Auroral Television Camera (ATV)
To improve the quality of the electric field measurement, the satellite's surface is designed conductive to decrease possible electrical disturbances surrounding Akebono.[3]
To support the operation of the instruments, the satellite contains: [subcategory]
Two sets of 60 m tip-to-tip wire antennas
One three-axial loop antenna with a 60 cm X 60cm rectangular shaped winding
5m and 3m extensible masts
A despun-mirror system
Observations
Akebono’s orbit covers a vast region of the plasmasphere. From 500 to 10,500 kilometers.[9] [1]
observed by the Akebono satellite in the altitude region around 3200–10,000 km (L= 1.5–3.4) in 1989 and 1990, which is the highest altitude where at which M/Q = 2 ion cyclotron whistlers have been observed till date. We discuss the ion concentration in the inner magnetosphere estimated from crossover frequencies of ion cyclotron whistlers observed by Akebono. [Need to work on revising this area, just have trouble with keeping it accurate]
have shown that small-scale field-aligned currents always exist in large-scale region 1, region 2, cusp and polar cap current systems. (throught the fluxgate, source 7, the science journal one)
See Also
References
- ^ "Akebono (satellite)", Wikipedia, 2021-01-31, retrieved 2021-10-20
- ^ a b "JAXA | Aurora Observation Satellite "AKEBONO" (EXOS-D)". JAXA | Japan Aerospace Exploration Agency. Retrieved 2021-10-20.
- ^ a b c Tsuruda, K.; Oya, H. (1991). "Introduction to the EXOS-D (Akebono) Project". Geophysical Research Letters. 18 (2): 293–295. doi:10.1029/91GL00039. ISSN 1944-8007.
- ^ Miyake, W.; Miyoshi, Y.; Matsuoka, A. (2015-12-01). "An empirical modeling of spatial distribution of trapped protons from solar cell degradation of the Akebono satellite". Advances in Space Research. 56 (11): 2575–2581. doi:10.1016/j.asr.2015.10.021. ISSN 0273-1177.
- ^ Mozer, F. S. (2016). "DC and low-frequency double probe electric field measurements in space". Journal of Geophysical Research: Space Physics. 121 (11): 10, 942–10, 953. doi:10.1002/2016JA022952. ISSN 2169-9402.
- ^ Hayakawa, H.; Okada, T.; Ejiri, M. (1990). "Electric field measurement on the Akebono (EXOS-D) satellite". Journal of Geomagnetism and Geoelectricity (Tokyo). 42 (4): 371–384. ISSN 0022-1392.
- ^ "akebono exos-d satellite: Topics by WorldWideScience.org". worldwidescience.org. Retrieved 2021-10-30.
- ^ Fukunishi, H.; Fujii, R.; Kokubun, S.; Hayashi, K.; Tohyama, T.; Tonegawa, Y.; Okano, S.; Sugiura, M.; Yumoto, K.; Aoyama, I.; Sakurai, T. (1990). "Magnetic Field Observations on the Akebono (EXOS-D) Satellite". Journal of geomagnetism and geoelectricity. 42 (4): 385–409. doi:10.5636/jgg.42.385.
- ^ Matsuda, Shoya; Kasahara, Yoshiya; Goto, Yoshitaka (2015). "M/Q = 2 ion distribution in the inner magnetosphere estimated from ion cyclotron whistler waves observed by the Akebono satellite". Journal of Geophysical Research: Space Physics. 120 (4): 2783–2795. doi:10.1002/2014JA020972. ISSN 2169-9402.