Radar astronomy and radioastronomy using the over-the-horizon radar NOSTRADAMUS. ONERA, Département Electromagnétisme et Radar
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1 Radar astronomy and radioastronomy using the over-the-horizon radar NOSTRADAMUS J-F. Degurse 1,2, J-Ph. Molinié 1, V. Rannou 1,S. Marcos 2 1 ONERA, Département Electromagnétisme et Radar 2 L2S Supéléc, CNRS UMR 8506, Université Paris-Sud Conférence Elbereth 2013, Institut d Astrophysique de Paris
2 Introduction Jean-François DEGURSE PhD Funding DGA Thesis defense: 15/01/2014 «Space-time adaptive processing in heterogeneous environment. Application to radar detection and implementation on GPU.» Other works: Use an over-the-horizon radar developped by ONERA to do astronomy 2
3 OUTLINE The NOSTRADAMUS over-the-horizon radar Radar astronomy (radar mode) Radioastronomy (passive mode) 3
4 Skywave over-the-horizon radar interests IONOSPHERE Classical radar Blind zone LOS detection Over the horizon radar OTH detection Earth Earth Long range detection All altitude detection (including very low) No stealth target in HF band F 1, j F 2, j 2 4 Mission of OTH radar: Monitoring sector at long range for early warning 4
5 Detection below ionospheric layers: Oceanography 5 Wind direction Oceanic waves height Interest: Weather studies (sea state over large area) Cyclone tracking Drifting objects tracking and forecasts 5
6 Frequency (MHz) Elevation (degrees) Ionosphere sounding with Nostradamus 6 Backscatter sounding with scanning in : Frequency Elevation Azimuth Group range Group range Sunrise Ionospheric forecasts average conditions No external sounders radar mode alternated with sounding mode 6
7 Applications in Astronomy Why? : Source: JPL Diversification of the applications of the NOSTRADAMUS radar Few radiotelescopes operate in HF band (RDN Nancay, UTR-2) but renewed interest with new projects (LOFAR, LWA) Have Fun!! 7
8 Applications in Astronomy: radar mode Transmit and reception: radar principles for one antenna Te Tr Te Tr Te Tr Te Tr Te Tr «slow-time» Doppler frequency «fast-time» dimension or range Range-Doppler image 8
9 Detection of the Moon The moon is completely within the receiving beam Fixed beam (azimuth/elevation) Detection of the Moon when entering into the beam Radar frequency: 20,5 MHz (crossing the ionosphere and low bias at night) Ambiguous range measurement Te= 3ms B=20kHz, implying a range resolution of 7,5km TRecu= 30ms, hence Form Factor is FF=1/10 Coherent integration of 256 récurrences, Tint= 7,68s Start scanning gate Deb_num= 3,5ms, -> 525km End scanning gate Fin_num= 29,5ms, -> 3975km 9
10 Detection of the Moon /2 Nostradamus R L Good Signal-to-Noise Radio (SNR) expected Moon dimensions greater than signal wavelength Radial extension of the backscattered echo (about 1700km) Variation of echos amplitude depending on the range 10
11 Detection of the Moon Range-Doppler image (radial) for the beam steered towards the Moon Low Doppler shift 11
12 Range and Doppler profile Detection of the Moon Coupe suivant les distances Coupe suivant les Doppler Applications: Radar calibration (localization) Ionospheric bias study Moon imagery using ISAR methods Moon reflectivity study (penetration of HF waves into the regolith) 12
13 Range (km) Radial acceleration (m/s2) Detection inside or beyond ionospheric layers: 13 Line of sight propagation (high frequency) Ionospheric bias due to electronic content (angular deviation, range and Doppler bias) Bias corrections Range Radial acceleration Time (s) Interest: Tracking objects through the ionosphere Satellite detection Calibration for radiotelescopes Time (s)
14 Meteor detection Fast particles passing through the ionosphere Create an ionized channel Detection in radar mode Ionospheric plasma density & frequency determine if echos are "overdense" or "underdense" Image range-slow time (no ground echos) Typical reflexion on an underdense meteor trail 14 Applications: Detection of Extensive Air Shower caused by cosmic rays
15 Coronal Mass Ejection (CME) measurement Low SNR Ratio: requires long integration but wavefront is moving fast! Huge Doppler shift (~5-40kHz) Interest: Estimate the density and the speed of CME 15
16 Astronomy applications: passive mode Passive mode: principle for one antenna Te Tr Te Tr Te Tr Te Tr Te Tr «Slow-time» dimension «fast-time» dimension Receiver bandwidth Time-Frequency image 16
17 Sun radio observation Measurement of noise generated by the Sun Passive mode at 25,6MHz (trans-ionospheric) The sun is entirely within a receiving beam Looking direction is fixed (azimuth/elevation) Detecting of the Sun when it enters the beam Experimentation: 14/10/2011 from 11h 10 to 12h 20 TU No increase of the background noise during the transit of the Sun into the beam Presence of bursts caused by solar flares This bursts were located in the Corona 17
18 Sun radio observation 25,6 MHz 14 oct 2011 Entry of the solar disk into the beam Solar disc is at the center of the beam Solar disk leaves the beam 18
19 Sun radio observation 25,6 MHz 14 oct
20 Sun radio observation 25,6 MHz 14 oct 2011 RDN Nançay - WIND Source : secchirh.obspm.fr/ NOSTRADAMUS 20
21 Digital beamforming Sun imagery 25,6 MHz 14 oct 2011 Main lobe 1 azimuth 2 elevation S 21
22 Frequency (khz) Observation of radio emissions from Jupiter Fixed beam, frequency = 21,437 MHz 14 december 2012, 21h15 23h00 TU Tracking mode 22 Time (s)
23 Frequency (khz) Observation of radio emissions from Jupiter Fixed beam, frequency = 21,437 MHz 14 december 2012, 21h15 23h00 TU Tracking mode 23 Time (s)
24 Observation of radio emissions from Jupiter Faisceaux fixe: 21,437 MHz 14 décembre 2012, 21h15 23h00 TU Mode poursuite 24
25 Observation of radio emissions from Jupiter Imagery Digital beamforming 25
26 Pulsar observation at long wavelength Observation of pulsar PSR avril 2013 Frequency: 25,6 MHz Processing is more complex: Very low SNR Ratio Frequency dispersionof the signal Temporal integration is difficult In processing 26
27 Observation of Orbital Angular Momentum in radio An electromagnetic wave passing near a massive body (black hole) can acquire an orbital angluar momentum The structure of NOSTRADAMUS is adapted to OAM detection Goal: detect OAM rays coming from HF radio sources OAM paramater 27
28 Observation of Orbital Angular Momentum in radio 25MHz simulations Reception pattern of Nostradamus at f=25 MHz for a plane wave with l=0. Reception pattern of Nostradamus at at F=25 MHz for an OAM with l=1. To detect an OAM: compensate the phase due to the spatial spin Limitation to l=2 due to the 3 arms configuration Need for HF OAM with sufficient SNR 28
29 STAP processing for radioastronomy Data: LOFAR Nançay (R. Weber) 29 Clear environment Jammed environment radio frequency intereference
30 STAP processing for radioastronomy Use multidimensionnal adapative processing to remove RFI 30 Clear environment Jammed environment after STAP processing
31 Conclusion Application in radara astronomy and radioastronomy of NOSTRADAMUS: Moon radar detection, Detection of a Solar Coronal Mass Ejection (CME) Sun radio observations (bursts), Jovian radio observations, Observation of OAM in radio band, Pulsar observation, Cosmic rays detection,... Radar signal processing applied to radioastronomy Potential collaboration for the use of NOSTRADAMUS Was very fun and exciting 31
32 Thank you for your attention Contact: 32
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