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High Latitude Outer Radiation Belt Boundary Dynamics in Comparison with NOAA POES Polar Ovals V

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High Latitude Outer Radiation Belt Boundary Dynamics in Comparison with NOAA POES Polar Ovals V WDS'14 Proceedings of Contributed Papers — Physics, 331–336, 2014. ISBN 978-80-7378-276-4 © MATFYZPRESS High Latitude Outer Radiation Belt Boundary Dynamics in Comparison with NOAA POES Polar Ovals V. O. Barinova, V. V. Kalegaev, I. N. Myagkova, M. O. Riazantseva D.V. Skobeltsyn Institute of Nuclear Physics (SINP) Of Moscow State University (MSU), Moscow, Russia. Abstract. This paper describes the geometry and the behaviour of the Earth's outer radiation belt polar boundary at the altitudes between 500 and 1000 km from the Earth surface in dependence of universal time and geomagnetic activity expressed by the Dst-index. The quantitative model which was built earlier for the Northern hemisphere in quiet conditions using the Coronas-Photon data measured in 2009 is upgraded in this work using Meteor-M No.1 data for being usable during periods of disturbed magnetosphere. Both hemispheres are studied now. Observations are taking place at different altitudes. The outer radiation belt boundary is compared with the Polar Oval using data of NOAA POES for the period of time from September 2011 till July 2012. Introduction A radiation belt is a structure formed by the trapped radiation. The Earth's outer radiation belt mostly contains electrons. For the ideal dipole magnetic field it can be easily described by two surface equations [van Allen, 1962]. However, the observed boundary differs from the calculated one. The outer radiation belt high-latitude boundary can be observed onboard polar low-altitude orbit satellite using electron fluxes measurements. There are two points at the time profile of the electron fluxes near the timestamp when the satellites latitude achieves its maximum or minimum at every orbit where the abrupt decrease or increase of the flux changes to approximate constant value. These two points are at the time when the satellite orbit crosses the boundary of the outer radiation belt. If the Earth field was the ideal dipole field, the boundary at every altitude would be the circle and could be calculated using the known formula [van Allen, 1962]. The goal of this work was to describe the observed shape of the boundary and variations of its position. It is well known that the outer radiation belt particle fluxes abruptly change during geo- magnetic storms [Kuznetsov et al., 2007] which are induced either by arrival of coronal mass ejections [Panasyuk, 2004; Gopalswamy, 2006] or high-speed fluxes of the solar wind [Li, 2005]. The size of the trapped radiation region is also very sensitive to the solar wind speed and geo- magnetic activity [Kuznetsov et al., 2007]. During the magnetic storm main phase of Coronal Mass Ejections(CME) and (Co-rotating Interaction Region) (CIR)-driven storms when the Dst- index reaches the minimum, the locations of the outer boundary move to L = 4 and L = 5:5, respectively [Yuan, 2011]. Some peculiarities of outer radiation belt dynamics (position of max- imum fluxes of relativistic electrons, location of rapid enhancements of the electron fluxes) were studied by Myagkova [2010]; Tverskaya et al. [2007, 2008]. Building of the Earth's outer radiation belt boundary model can be divided into several stages. The disturbed periods were excluded first and it made it possible to build the statistical model of the Earth's outer radiation belt. It based on the observations only and the best picture was seen when built in Geodetic coordinates with the fixed earth position. The other coordinate systems we tried, especially geo and other magnetic coordinates blurred the boundary, made it became wider and its shape became strictly round due to the Earth rotation and the rotation of the magnetic poles with it. So we decided to build the model in dependence on the universal time only using Coronas-Photon satellite data [Barinova et al., 2011]. Coronas-Photon satellite operated from March till November in 2009. The channel of the electrons > 0:2{1 MeV was selected as the channel with the lowest energy of the electrons, the 331 BARINOVA ET AL.: HIGH LATITUDE OUTER RADIATION BELT BOUNDARY DYNAMICS Figure 1. Northern Hemisphere. Projected crossings of the outer radiation belt boundary by the Coronas-Photon (black) and Meteor-M No.1 (white) orbits. Electrons 0.2{1 MeV onboard Coronas-Photon and Electrons > 0:1 MeV onboard Meteor-M No.1. highest electron fluxes values in the radiation belt and as the result | the most distinguishable boundary of the radiation belt at the time profile graph. An algorithm of automatic boundary detection using particle fluxes time profile was developed in the previous paper by Barinova et al. [2011], a database of boundary crossings by the satellite orbit was created and the model of the outer radiation belt boundary dynamics for the quiet period, when it depends only on the universal time, was constructed. This boundary cannot be described as an absolytely thin line with no width, a mathematical abstraction which separates the radiation belt and polar cap regions but it was decided to approximate it with an absolutely thin average curved line at the satellite altitude using the elliptic formula as a base. The new goal was to explore the dynamics of the outer radiation belt high-latitude boundary using the magnetic storm database to upgrade the model for calculating the position of the high latitude boundary for the periods of disturbed magnetosphere. Instruments comparison It was impossible to use data of the Coronas-Photon satellite because it stopped operating in 2009, the 30th of November. But since both the Coronas-Photon solar observatory and the Meteor-M No.1 satellites had circular polar orbits (Coronas-Photon: 550 km altitude, 82:5◦ inclination; Meteor-M No.1: 832 km altitude, 101:3◦ inclination), it was possible to use Meteor- M onboard instruments to monitor the Earth's outer radiation belt at low altitudes. The MSGI instrument installed onboard the Meteor-M No.1 spacecraft consists of a number of semiconductor and scintillation detectors and it is used to measure energetic particle fluxes (0.1{13 MeV electrons and 1{260 MeV protons) [Meteor-M No.1 web-page, 2012]. The most similar to the previous channel is electrons > 0:1 MeV measured by the MSGI instrument. Fortunately there was a month when Coronas-Photon and Meteor-M No.1 were in operating together [Barinova et al., 2011]. But since the altitude of the orbit of Meteor-M No.1 differs from the Coronas-Photon one it was necessary to make a special projection of the Coronas-Photon points to the altitude of Meteor-M No.1 orbit using the equation of the dipole field line: (We can use the dipole cause the accuracy of the model cannot be more than the accuracy of the measurements) r = L cos2(φ): (1) 332 BARINOVA ET AL.: HIGH LATITUDE OUTER RADIATION BELT BOUNDARY DYNAMICS Figure 2. Time profile of the particle fluxes. Data was averaged to 30 seconds to better view and processing. Where φ is the geomagnetic latitude, r is the distance to the Earth center measured in the Earth radii and L is an L-shell (Mcilwain coordinate). And the latitude of the searched point of crossing of the outer radiation belt boundary by the Coronas-Photon for the Meteor-M altitude can be found (in degrees): 180 rrmet φmet = ± arccos(cos(φcor) ): (2) π rcor Longitude stays the same. Figure 1 shows the visual result of the data comparison. Disturbed periods Magnetic storm is often caused by CME connected with solar flare and is accompanied by the solar cosmic rays event. In this case both polar caps are filled with the solar particles and the detection of the boundary becomes impossible. But even when it's possible sometimes it's easier to process some periods manually then an algorithm. Figure 2 shows a stormy period but caps have just started to be fulfilled so boundaries can be detected. Over 40 storms, 8 of which were strong (Dst < −100 nT), were observed and studied since November 2009 till June 2012. The result was added to the database of the outer radiation belt boundary crossings by the satellites orbits. Since Meteor-M No.1 has Solar synchronized orbit, this database cannot be effectively split hourly to determine the UT-effect, but it had already been included into the model in the previous work [Barinova et al., 2012]. Now it became possible to split this database by Dst index because it varies from −137 to +80 nT. (In 2009 −40 < Dst < 40 nT except a few times). Figure 3 shows the plot of all the data in the polar geographical coordinate system. Each point is a place where the satellite crosses the outer radiation belt high-latitude boundary in various moments of time. The color of the dot is selected using the Dst scale: the less Dst, the darker color is at the point. The model upgrade By minimizing the RMS deviation, the equation of the ellipse describing the average outer radiation belt boundary was fitted for different intervals of Dst values. The linear dependency of the length of the major axis of the ellipse on DST was found. Non-linear terms are out of the measurement and data processing accuracy. The area filled with points is determined by the structure of geomagnetic field. It is prolate and shifted as expected. The width of this statistical boundary is about 5◦ which shows a good quality of boundary detection algorithm. The width is seen at the picture and also measured by taking average values at the various longitudes. According to the Earth's rotation each meridian 333 BARINOVA ET AL.: HIGH LATITUDE OUTER RADIATION BELT BOUNDARY DYNAMICS Figure 3.
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