1. Modern Status LUNAR ОRBITAL RADIO DETEKTOR
V. A. Chechin, G.A. Gusev, B. N. Lomonosov,
K. M. Pichkhadze, N.G. Poluhina, V. A. Ryabov, V. K. Sysoev, V. A. Tsarev
ARENA JUNE 25-27, G.Gusev
Russia: LPI, Lavochkin association

2. Method: detection of radio emission; the Moon as a target
Scientific problems:
The prime goal: detection of UHECR & UHEN with energy E > 1020 eV
Additional goals: study of the Moon and its vicinity (EM environment, plasma, lunar seismic activity, etc.)‏
Method: detection of radio emission; the Moon as a target
Realization: within the LUNA-GLOB mission
Collaboration: LPI, Lavochkin Association, MSU;
Expected results : measurements of the CR flux near and above the GZK cut-off, detection of ultra-high energy neutrinos.
ARENA JUNE 25-27, G.Gusev

3. ?
ARENA JUNE 25-27, G.Gusev

4. Optimization of the concept and configuration of the experiment
Theoretical calculations and simulation of the generation and registration of radio emission in the different media
Optimization of the concept and configuration of the experiment
Simulation of the experiment (taking into account the scattering and reflection of the signal due to subregolith layer)‏
Adjusting to the space platform, ballistics etc.
Expected by-product results (lunar seismic activity, impacts of meteorites)‏
ARENA JUNE 25-27, G.Gusev

5. The Moon as a target Rmoon = 1740 km Regolith: density   1.7 g / cm3
depth ÷12 m,
dielectric permitivity ε≈3
attenuation length  ~ 15 m/ f (GHz);
effective volume for Veff ~ 2105 (km.w.e.)3;
neutrino detection
Average surface temperature: from 107 C to C
ARENA JUNE 25-27, G.Gusev

6. CONCEPTUAL MODELING of the EXPERIMENT
ARENA JUNE 25-27, G.Gusev

7. 0.4·106 km2sr Full aperture, km2·sr Energy eV
Full aperture for UHECR events
0.4·106 km2sr
Full aperture, km2·sr
Energy eV
ARENA JUNE 25-27, G.Gusev

8. LORD limits on  flux
1 year
Eth =
0.01V/m MHz;
f = 0.5; GHz
18/06/08

9. CONCEPTUAL DESIGN OF THE RADIO DETECTOR
ARENA JUNE 25-27, G.Gusev

10. ARENA JUNE 25-27, G.Gusev

11. Monte Carlo Modeling of the Experiment
Simulation of the event (Cherenkov emission) registration in t-representation taking into account models of antenna system (diagram, polarization), noises (thermal and galactic), digital system parameters
ARENA JUNE 25-27, G.Gusev

12. Number of simulations)
Experimental parameters
Determination of threshold tension and transfer function
Start of selection cycle
Selection of event candidates with condition
Addition of the signal with noise
Number of simulations)
Selection of events with trigger
Primary parameters
Candidates? no
Useful event
Forming of array of primary parameters with dimension [1 x NI]
Secondary parameters
With dimension [1 х Nin]:
Digitizing of signals
Forming of array of secondary parameters with dimension[1 x NI]:
End of selection? no
Algorithm
ARENA JUNE 25-27, G.Gusev
Exit

13. + +
ARENA JUNE 25-27, G.Gusev

14. Model study of the basic characteristics of the LORD experiment.
f, MHz
f, МHz
Distribution in signal duration
t, ns
t, ns
ARENA JUNE 25-27, G.Gusev

15. ARENA JUNE 25-27, G.Gusev

16. ARENA JUNE 25-27, G.Gusev

17. Taking into account the subregolith layer Retarded reflected signal
vacuum
Retarded reflected signal
T = 2hcosθn/c
Direct signal 1 CR 2 3
regolith ν h h θ
ε≈3
ε≈6÷8
subregolith
ARENA JUNE 25-27, G.Gusev

18. reflected
direct
The first example of the statistics for direct(blue) and reflected(red) signals (CR cascade) for the regolith depth is 1 m (without scattering on two interfaces)‏
ARENA JUNE 25-27, G.Gusev

19. reflected
direct
Second example of the statistics for direct and reflected signals. Regolith depth is 10 m. For this regolith depth the statistics for reflected signal is two times smaller.
ARENA JUNE 25-27, G.Gusev

20. A2 B2
direct
reflected A1 B1
Registration of a signal in t-representation by 4 antennas with two orthogonal polarizations.
ARENA JUNE 25-27, G.Gusev

21. Amplitude, μV
Amplitude of the direct and reflected signals as a function of cascade energy.
ARENA JUNE 25-27, G.Gusev

22. Currently a new platform is under construction.
Universal platform for small-sized space vehicles
LAVOCHKIN ASSOCIATION
Currently a new platform is under construction.
ARENA JUNE 25-27, G.Gusev

23. CONCLUSIONS
1. For CR spectrum E-3 statistics per year in the LORD experiment :
for CR – one hundred events;
for GZK neutrino (maximum flux model) – several units events.
2. Conception of radio detector (first generation) is developed and optimized.
3. There are principle possibilities for selection of the events from the radio pulse background and separation between CR and neutrino cascades.
4.The LORD experiment is included in LUNA-GLOB mission, to be launched at about 2012 year.
ARENA JUNE 25-27, G.Gusev

24. THE END
THANK YOU
ARENA JUNE 25-27, G.Gusev

25. Some examples of lunar relief (from Apollo mission )‏
STUDY of the INFLUENCE of the MOON SURFACE RELIEF and FINITE DEPTH of the REGOLITH on DETECTION of RADIO EMISSION
Some examples of lunar relief (from Apollo mission )‏
On the left photo one can see relatively flattish lunar surface and hills, for which the diffusion by small irregularities is not strong . On the other hand on the right photo one sees irregular stone big enough to destroy significantly mirror component of radio emission from cascade.
ARENA JUNE 25-27, G.Gusev

26. 1. In the case of small diffusion, duration of the signal is virtually the same as for ideally flat plane surface, amplitude decrease does not exceed 10%.
2. In the case of strong diffusion incident from below beam transforms into many quasi-mirror ray beams and diffusion component. Although the diffusion diminishes the signal amplitude (increasing threshold), but it increases angular aperture so that positive integral effect in statistics may be more, due to relatively small angular aperture and small penetration coefficient from regolith to vacuum for Cherenkov mechanism used in simulations.
3. We must take into account that in the case of more large angular aperture we have more large registration surface and more favourable conditions for the concordance with LORD antenna (effective distance, diagram and polarization).
Also the scattering diminishes from below the range of registering primary particle energy, consequently the imprecision of energy measurements also diminishes.
ARENA JUNE 25-27, G.Gusev

27. Lebedev short message on physics #10, 1984, p. 41.
The schema of phase interferometer for EAS registration with effective area 1000 km^2.
It consists of 5 transmitters and 20 receivers. For CR with spectrum E^-3 statistics per year about 1 event for energies E>5·10^20 eV
Lebedev short message on physics #10, 1984, p. 41.
18/06/08

28. Background Processes for Radio Antarctic Muon
and Neutrino Detector (RAMAND)
A.F. Bogomolov, V.V. Bogorodsky, et al.
Proc. 20 ICRC, v. 6, p.472
The curve 1 corresponds to radio pulse background spectrum at the Russian Vostok station, the curve 2 – at the Mirnii station (20 km from the cost) during good whether, the curve 3 – at the Mirnii during storm (23 m/sec). Here the σ is thermal noise rms for temperature about 3000ºC.
18/06/08