Towards a European Infrastructure for Lunar Observatories Towards a European Infrastructure for Lunar Observatories Bremen, Wednesday 23 Bremen, Wednesday 23 rd rd March 2005 March 2005 A 3D cosmic ray detector on the Moon A 3D cosmic ray detector on the Moon X. X. Moussas Moussas University of Athens University of Athens [email protected]3D cosmic ray time dependent distributions can be obtained using properly positioned cosmic ray detectors on the Moon. This system can give new insight to the study of the modulation of both galactic and solar cosmic rays It will provide measurements outside the Earth’s magnetosphere of: 1. the cosmic ray intensity time variability 2. the cosmic ray anisotropy time variability 3. Earth directed strong solar wind shocks and hence 4. space weather predictions complementary to other methods 5. time and directional variations of the spectrum, possibly variations of the composition and temperature of cosmic rays can also be measured 6. Magnetar activity studies will also benefit from such an observatory
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Towards a European Infrastructure for Lunar Observatories Bremen, Wednesday 23 rd March 2005
A 3D cosmic ray detector on the Moon X. Moussas University of Athens [email protected]. 3D cosmic ray time dependent distributions can be obtained using properly positioned cosmic ray detectors on the Moon. - PowerPoint PPT Presentation
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Towards a European Infrastructure for Lunar ObservatoriesTowards a European Infrastructure for Lunar ObservatoriesBremen, Wednesday 23Bremen, Wednesday 23rdrd March 2005 March 2005
A 3D cosmic ray detector on the MoonA 3D cosmic ray detector on the MoonX.X. MoussasMoussas
3D cosmic ray time dependent distributions can be obtained using properly positioned cosmic ray detectors on the Moon.
This system can give new insight to the study of the modulation of both galactic and solar cosmic rays
It will provide measurements outside the Earth’s magnetosphere of:1. the cosmic ray intensity time variability 2. the cosmic ray anisotropy time variability 3. Earth directed strong solar wind shocks and hence 4. space weather predictions complementary to other methods 5. time and directional variations of the spectrum, possibly variations of the composition and
temperature of cosmic rays can also be measured6. Magnetar activity studies will also benefit from such an observatory
The study of cosmic rays both galactic and solar continues to be of great importance to space sciences (origin, propagation, exotic objects)
The cosmic ray spectral (not only the higher end) time and directional variability is of importance to cosmic sciences
• The SunThe Sun the 11 (or 22) year solar the 11 (or 22) year solar activity cycle & Cosmic Rays activity cycle & Cosmic Rays
time variations of the Heliospheretime variations of the Heliosphere::temperature, density, magnetic filed, velocity of the termination shock and radiustemperature, density, magnetic filed, velocity of the termination shock and radius
Cosmic ray 1D shell model (red), also for 400 MeV, > 5 GeV compared with Climax Neutron MonitorCosmic ray 1D shell model (red), also for 400 MeV, > 5 GeV compared with Climax Neutron Monitor
whenever we have directional flux n=a00 (1) measurments of a population of particles (e.g. solar energetic particles, cosmic rays, solar wind plasma) of well-defined energy resolution are available, new macroscopic fluid-like quantities can be rigorously estimated, thus describing the sub-flux referring to that energy range in fluid terms. We have derived analytically, exact closed relations for these quantities as functions of lower order spherical harmonics coefficients. Equation (1) gives the differential number density of the energetic particles. Equations (2), (3) give the components and the magnitude respectively of the mean velocity. Equation (4) states that first order anisotropy vector, A1 is parallel and proportional in magnitude to the differential mean particle velocity. Thermal pressure tensor vector components are written as in equations (5)-(10). Equation (11) gives the kinetic temperature of cosmc rays.
Also the direction of heat flux
Cosmic ray fluxes, heat flux, anisotropies and temperature, density etc
Cosmic ray fluxes, anisotropies and temperature, density etc
Cosmic ray fluxes, anisotropies and temperature, density etc
The global neutron monitor network is used as a large CR 3D detectorThis permits the prediction of the arrival of an interplanetary shock (CME)using the anisotropies of “galactic” cosmic rays (see also Dorman, Belov and colleagues). Anisotropies of CR can be measured using detectors on the Moon without the masking and dstortion of the magnetic filed of he Earth
See Cosmic Rays and Space WeatherBy Lev I. DORMAN
Cosmic rays are used for forecasting of major geomagnetic storms accompanied by Forbush-effects.
NM network, asymptotic directions of cosmic ray stations
(asymptotic directions)
Scheme of mechanisms of possible precursor effects in CR (Dorman et al 2003)
Observations of a precursor effect in CR (from Dorman et al 2003) : Galactic cosmic ray pre-increase (white circles) and pre-decrease (grey circles) effects before the Sudden Storm Commencement (SSC) of great magnetic storm in September 1992, accompanied with Forbush-decrease
A 3D cosmic ray detector on the MoonA 3D cosmic ray detector on the Moon
3D cosmic ray time dependent distributions can be obtained using properly positioned cosmic ray detectors on the Moon.
This system can give new insight to the study of the modulation of both galactic and solar cosmic rays
It will provide measurements outside the Earth’s magnetosphere of:1. the cosmic ray intensity time variability 2. the cosmic ray anisotropy time variability 3. Earth directed strong solar wind shocks and hence 4. space weather predictions complementary to other methods 5. time and directional variations of the spectrum, possibly variations of the
composition and temperature of cosmic rays can also be measured6. Magnetar activity studies will also benefit from such an observatory