© The Aerospace Corporation 2010 Radio Occultation Sensor Observations of Ionospheric Scintillation P. R. Straus 1, C. Carrano 2, R. Caton 3, K. Groves.

Slides:

Advertisements

Similar presentations

ESWW 5 Some ionospheric effects on ground based radar Y. Béniguel, J.-P. Adam.

Advertisements

B-spline Model of Ionospheric Scintillation

Using a DPS as a Coherent Scatter HF Radar Lindsay Magnus Lee-Anne McKinnell Hermanus Magnetic Observatory Hermanus, South Africa.

Calibration Scenarios for PICASSO-CENA J. A. REAGAN, X. WANG, H. FANG University of Arizona, ECE Dept., Bldg. 104, Tucson, AZ MARY T. OSBORN SAIC,

DETECTION OF UPPER LEVEL TURBULENCE VIA GPS OCCULTATION METHODS Larry Cornman National Center for Atmospheric Research USA.

Wave-critical layer interactions observed using GPS data Bill Randel, NCAR.

How can we get a vertical profile of the atmosphere?

1 UNCLASSIFIED – FOUO – Not for Public Release Operational Space Environment Network Display (OpSEND) & the Scintillation Network Decision Aid Dr. Keith.

GPS / RO for atmospheric studies Dept. of Physics and Astronomy GPS / RO for atmospheric studies Panagiotis Vergados Dept. of Physics and Astronomy.

ElectroScience Lab IGARSS 2011 Vancouver Jul 26th, 2011 Chun-Sik Chae and Joel T. Johnson ElectroScience Laboratory Department of Electrical and Computer.

1 Robert Schaefer and Joe Comberiate for the SSUSI Team Robert SchaeferJoe Comberiate (240) (240)

Radio Occultation From GPS/MET to COSMIC.

GPS Occultation Studies of the Lower Ionosphere: Current Investigations and Future Roles for C/NOFS & COSMIC Sensors R. Bishop.

Department of Computer Science and Electrical Engineering GNSS Research Group – EIS Laboratory GNSS Bistatic Radar September 14, 2006 Tore Lindgren, Dennis.

Sporadic E seasonal variability and descent derived from GPS- COSMIC Radio Occultation 1 Department of Physics, Chinese Culture University, Taipei, Taiwan,

New Satellite Capabilities and Existing Opportunities Bill Kuo 1 and Chris Velden 2 1 National Center for Atmospheric Research 2 University of Wisconsin.

Use of GPS RO in Operations at NCEP

Comparison of temperature data from HIPPO-1 flights using COSMIC profiles and Microwave Temperature Profiler. Kelly Schick 1,2,3 and Julie Haggerty, Ph.D.

Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)

ARL Applied Research Laboratories The University of Texas at Austin ARL Applied Research Laboratories The University of Texas at Austin Ionospheric Tomography.

COSMIC GPS Radio Occultation Temperature Profiles in Clouds L. LIN AND X. ZOU The Florida State University, Tallahassee, Florida R. ANTHES University Corporation.

Joint International GRACE Science Team Meeting and DFG SPP 1257 Symposium, Oct. 2007, GFZ Potsdam Folie 1 Retrieval of electron density profiles.

SI Traceability Applied to GPS RO October 22, 2008 CLARREO Workshop Oct 2008 AJM/JPL 1 SI Traceability Applied To GPS Radio Occultation A. J. Mannucci,

Charles S. Carrano, Cesar E. Valladares, Keith M. Groves

A New Bound on the Radar Cross-section of the Sun Bill Coles, UCSD Mike Sulzer and John Harmon, NAIC Jorge Chau and Ron Woodman, JRO We have not observed.

Vertical Wavenumber Spectra of Gravity Waves in the Venus and Mars Atmosphere *Hiroki Ando, Takeshi Imamura, Bernd Häusler, Martin Pätzold.

Vertical Structure of the Atmosphere within Clouds Revealed by COSMIC Data Xiaolei Zou, Li Lin Florida State University Rick Anthes, Bill Kuo, UCAR Fourth.

Use of GPS Radio Occultation Data for Climate Monitoring Y.-H. Kuo, C. Rocken, and R. A. Anthes University Corporation for Atmospheric Research.

The Mesoscale Ionospheric Simulation Testbed (MIST) Regional Data Assimilation Model Joseph Comberiate Michael Kelly Ethan Miller June 24, 2013.

Simulations of Radio Imaging in the Earth’s Magnetosphere J. L. Green, S. Boardsen, W. W. L. Taylor, S. F. Fung, R. F. Benson, B. Reinisch, and D. L. Gallagher.

Comparison of Temperature Data from HIPPO-1 Flight Using COSMIC and Microwave Temperature Profiler Kelly Schick 1,2,3 and Julie Haggerty 4 1 Monarch High.

Key RO Advances Observation –Lower tropospheric penetration (open loop / demodulation) –Larger number of profiles (rising & setting) –Detailed precision.

The Thermosphere/Ionosphere Response to Solar Activity During the October/November 2003 Storms P. R. Straus 1, G. Crowley 2, R. R. Meier 3, L. J. Paxton.

AGU Fall MeetingDec 11-15, 2006San Francisco, CA Estimates of the precision of GPS radio occultations from the FORMOSAT-3/COSMIC mission Bill Schreiner,

1 Module One: Measurements and Uncertainties No measurement can perfectly determine the value of the quantity being measured. The uncertainty of a measurement.

Deep Occultations With GRAS C. Marquardt, A.von Engeln and Y. Andres.

Aerosol distribution and physical properties in the Titan atmosphere D. E. Shemansky 1, X. Zhang 2, M-C. Liang 3, and Y. L. Yung 2 1 SET/PSSD, California,

Improved Radio Occultation Observations for a COSMIC Follow-on Mission C. Rocken, S. Sokolovskiy, B. Schreiner UCAR / COSMIC D. Ector NOAA.

-1- Solar wind turbulence from radio occultation data Chashei, I.V. Lebedev Physical Institute, Moscow, Russia Efimov, A.I., Institute of Radio Engineering.

Principles of the Global Positioning System Lecture 09 Prof. Thomas Herring Room A;

Predicting Ionospheric Densities and Scintillation with the Communication / Navigation Outage Forecasting System (C/NOFS) Mission Chin S. Lin 1, O. de.

Formosat3/COSMIC Workshop, Taipei, Oct. 1-3, 2008 The Ionosphere as Signal and Noise in Radio Occultation Christian Rocken, Sergey Sokolovskiy, Bill Schreiner,

0 Earth Observation with COSMIC. 1 COSMIC at a Glance l Constellation Observing System for Meteorology Ionosphere and Climate (ROCSAT-3) l 6 Satellites.

The identification of the fluctuation effects related to the turbulence and “permanent” layers in the atmosphere of Venus from radio occultation data V.N.Gubenko.

Electron density profile retrieval from RO data Xin’an Yue, Bill Schreiner  Abel inversion error of Ne  Data Assimilation test.

LIGO- G Z AJW, Caltech, LIGO Project1 A Coherence Function Statistic to Identify Coincident Bursts Surjeet Rajendran, Caltech SURF Alan Weinstein,

0 7th ESWW, Bruges, Ionospheric Scintillations Propagation Model Y. Béniguel, J-P Adam IEEA, Courbevoie, France.

COSMIC Ionospheric measurements Jiuhou Lei NCAR ASP/HAO Research review, Boulder, March 8, 2007.

GPS Radio-Occultation data (COSMIC mission) Lidia Cucurull NOAA Joint Center for Satellite Data Assimilation.

1 AIR FORCE RESEARCH LABORATORY Dr. Keith Groves Space Weather Center of Excellence AFRL/VSBXI 29 Randolph Rd Hanscom AFB, MA voice

Formosat-3/COSMIC WorkshopNov 28 - Dec 1, 2006Taipei, Taiwan Estimates of the precision of LEO orbit determination and GPS radio occultations from the.

Comparison of Temperature Data from HIPPO-1 Flights Using COSMIC and Microwave Temperature Profiler Kelly Schick 1,2,3 and Julie Haggerty 4 1 Monarch High.

Project presentation - Significant parameters for satellite communication.

The impact of wind turbines on fixed radio links Börje Asp, Gunnar Eriksson, Peter Holm Information and Aeronautical Systems FOI, Swedish Defence Research.

HSAF Soil Moisture Training

Munetoshi Tokumaru （ISEE, Nagoya University）

Joe Comberiate Larry Paxton JHU/APL June 28, 2007

Formosat3 / COSMIC The Ionosphere as Signal and Noise

Study of the sporadic E (Es) layer by GPS radio occultation (RO)

Ionospheric Effect on the GNSS Radio Occultation Climate Data Record

Hiromu Seko (MRI) , Toshitaka Tsuda and Naoto Yoshida (Kyoto Univ.)

Formosat3 / COSMIC The Ionosphere as Signal and Noise

Application of Aeolus Winds

Results and Discussions Data Used and Methodology

Can radio occultation be used to discern long-term tropopause trends?

SSAEM Sensors Paul R Straus October 14, 2011.

Effects and magnitudes of some specific errors

Floor Movement Measurement at ATF Ring

Challenges of Radio Occultation Data Processing

Presentation transcript:

© The Aerospace Corporation 2010 Radio Occultation Sensor Observations of Ionospheric Scintillation P. R. Straus 1, C. Carrano 2, R. Caton 3, K. Groves 3, and R.L. Bishop 1 The Aerospace Corporation 2 Boston College 3 Air Force Research Laboratory

2 Overview CORISS-Radar-Theory evaluation of RO scintillation observation Calculation of S4 “Proxy” S4 indices Ground UHF/RO scintillation comparison

Tangent Point Track Apex Altitude km C/NOFS Orbital Track 21 Apr :09 UT CORISS/ALTAIR Geometry

Coherent Returns from ALTAIR & CORISS SNR ALTAIR indicates location of small-scale (40cm) irregularities relative to the CORISS tangent point track. CORISS detects ionospheric irregularities only within F region, while high sensitivity of ALTAIR reveals structure at slightly lower altitudes. Mean scattering location is slightly westward of the CORISS tangent point track. CORISS occultation tangent points CORISS SNR Bottomside Max Height 10

Assume weak scattering: Break frequency Fresnel null frequencies Given propagation orthogonal to B, then Yields d s ~ 630 km (t.p. is ~500 km) Determine irregularity strength, region size, spectral slope, & BG density profile from ALTAIR, SCINDA & CORISS measurements where d is C/NOFS-GPS distance PRN 16 CORISS Observations & Simulation CORISS Multiple Phase Screen Simulation

15 MPS Simulation CORISS Multiple Phase Screen Simulation of CORISS Data

Proper Calculation of the S4 Index What sample rate should be employed? How long a data segment should be analyzed? The answer depends on the Fresnel frequency –Optimally, one should observe at a frequency substantially above f Fresnel and calculate S4 over a sample interval 10  longer than 1/f Fresnel –For occultation data 50 Hz observations are adequate with a 10 second sample interval RO data does not support calculation of S4 over a 1-second interval Data must also be detrended prior to calculating S4 where P i is the receiver power

“Proxies” for S4: S RO (1s) Calculated from MR (1 Hz) C/A SNR observations 1 Hz Data 50 Hz Data 05:10:00 S RO(1s) (31 s) S4 (10 s) C/A SNR S RO(1s) S4 (10 s) All profiles with max(S RO(1s) ) > 0.5

Summary of CORISS (L-Band)/SCINDA (UHF) Comparisons

“Proxies” for S4: UCAR S4 (COSMIC) Calculated from on-board 50 Hz SNR variance collected at 1 s cadence S4 (1s) UCAR S4 (10s) C/A SNR S4 (1 s) 05:10:00 S4 (10 s) S4 (10s) UCAR S4 (10s) All profiles with max(S RO(1s) ) > 0.5

11 Summary CORISS high rate observations of scintillation are in the process of being validated through ground/theory comparisons S RO(1s) calculated from 1 Hz SNRs generally under-predicts S4, but is fairly representative of S4 characteristics most of the time –The lower noise floor is useful for certain types of analysis UCAR (COSMIC) 1-second S4 index is not valid, but the UCAR approach to S4 determination can be made to work quite well if calculations are extend over a larger time interval (10 s)

12 Simulation of Scintillation in a Limb Viewing Geometry

13 Single Bubble Simulation

14 Multi-Bubble Simulation