Presentation is loading. Please wait.

Presentation is loading. Please wait.

Rosetta_CD\PR\what_is_RS.ppt, 04.09.2015 18:39AM, 1 Mars Express Radio Science Experiment MaRS MaRS Radio Science Data: Level 3 & 4 The retrieval S.Tellmann,

Published byBrice Hampton Modified over 8 years ago

Similar presentations

Presentation on theme: "Rosetta_CD\PR\what_is_RS.ppt, 04.09.2015 18:39AM, 1 Mars Express Radio Science Experiment MaRS MaRS Radio Science Data: Level 3 & 4 The retrieval S.Tellmann,"— Presentation transcript:

1 Rosetta_CD\PR\what_is_RS.ppt, 04.09.2015 18:39AM, 1 Mars Express Radio Science Experiment MaRS MaRS Radio Science Data: Level 3 & 4 The retrieval S.Tellmann, M.Pätzold ESAC June 2008

2 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 2 Overview LEVEL 3: The data preparation Calculation of bending angle and rayparameter The Abel Transformation LEVEL 4: The Neutral Atmosphere Calculation of Density Temperature Pressure The Ionosphere Calculation of the electron density

3 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 3 Level 3 Retrieval of the Refractivity and the Radius

4 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 4 Level 3 Data Processing Flow Chart Input: Level 2 residual

5 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 5 Level 3 Data Processing Flow Chart Input: Level 2 residual Baseline fit correction

6 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 6 Starting Point: Residual Starting point: Level 2 residual Offset Offset (and/or trend): Reason Uncertainties in Orbit

7 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 7 Baseline Fit Correction Starting point: Level 2 residual Offset range for baseline fit radius: ~ 4000 km

8 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 8 Residual after Correction

9 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 9 Level 3 Data Processing Flow Chart Input: Level 2 residual Baseline fit correction Calculation of Measurement Geometry Occultation Plane

10 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 10 Next Goal: Calculation of Bending angle & Rayparameter  : bending angle a: rayparameter

11 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 11 Next Goal: Calculation of Bending angle & Rayparameter  : bending angle a: rayparameter Measurement geometry must be known: Occultation Plane containing Groundstation Planet Spacecraft given by: z: vector from groundstation to planet r: vector perpendicular to z and in this OCC plane

12 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 12 Occultation (OCC) plane Radio Link MEX orbit OCC plane at time t m Earth direction Calculation of state vectors for every measurement sample P MEX,V MEX P G/S,V G/S

13 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 13 Level 3 Data Processing Flow Chart Input: Level 2 residual Baseline fit correction Calculation of Bending Angle & Rayparameter Calculation of Measurement Geometry Occultation Plane

14 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 14 Next Goal: Calculation of Bending angle & Rayparameter  : bending angle a: rayparameter Solve equations from [Fjeldbo et al., 1971]: B · ( ) = ( ) where b 11 = -v rs sin(  e –  r ) + v zs cos(  e –  r ) b 12 = -v rt cos(  s –  r ) + v zt sin(  s –  r ) b 21 = (r s + z s ) 1/2 sin(b e –  –  r ) b 22 = z t cos(  s –  r ) k 1 = c  f/f s + v rs [cos(  e –  r ) – cos  e ] + v zs [sin(  e –  r ) – sin  e ] - v rt [sin(  s –  r ) – sin  s ] – v zt [cos(  s –  r ) – cos  s ] k 2 = z t sin(  s –  r ) + (r s 2 -z s 2 ) 1/2 sin(  e –  –  r )  r  r k1k1 k2k2

15 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 15 bending angle  =  r +  r rayparameter a = (r s 2 + z s 2 ) 1/2 sin(  e –  r –  ) Calculation of Bending angle & Rayparameter

16 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 16 Level 3 Data Processing Flow Chart Input: Level 2 residual Baseline fit correction Calculation of Bending Angle & Rayparameter Abel Transformation Calculation of Refractivity & Radius Calculation of Measurement Geometry Occultation Plane

17 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 17 Calculation of Refractivity & Radius Refractive index n n Refractivity  Radius r

18 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 18 Algorithm for the calculation of the refractive index via an Abel transform Initialise a vector of dimension ‚i‘ To store the row integrals Current rayparameter of layer ‚i‘ Upper and lower boundary of the current row integral Bending angle of the current layer Call of the integration function and storing of the integral output Summing up of the array Zintegral

19 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 19 Algorithm for the calculation of the refractive index via an Abel transform Initialise a vector of dimension ‚i‘ To store the row integrals Current rayparameter of layer ‚i‘ Upper and lower boundary of the current row integral Bending angle of the current layer Call of the integration function and storing of the integral output Summing up of the array Zintegral INTEGRAL: Integration routine able to handle the pole

20 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 20 Calculation of Refractivity radius [km]   Bending Angle Refractivity Abeltransform Bending angle [deg * 10 6 ] Refraktivität [deg * 10 6 ]

21 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 21 The Occultation Footpoints x Occultation footpoint Moving over the surface of Mars Spacecraft Earth direction

22 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 22 The Occultation Footpoints Calculation of intersection point of ray asymptotes using spherical symmetry Transformation of this vector into planetary coordinates (lat, lon) for every measurement value

23 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 23 Level 3 Data Processing Flow Chart Input: Level 2 residual Baseline fit correction Calculation of Bending Angle & Rayparameter Abel Transformation Calculation of Refractivity & Radius Calculation of Measurement Geometry Occultation Plane Main Output: Refractivity, Radius & OCC Footpoints Calculation of Occultation Footpoints

24 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 24 Level 4 The Neutral Atmosphere

25 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 25 Starting Point: Refractivity Ionosphere: Negative Refraktivity higher than ~ 80 km altitude approx. 3480 km radius Transition Region: no significant bending approx. 60 km – 80 km altitude approx. 3450 km – 3480 km Neutral Atmosphere: positive Refractivity up to approx. 50 km altitude up to approx. 3450 km radius Neutral Atmosphere Ionosphere Ionopause Transition Region

26 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 26 The Neutral Number Density  : refractivity C 1 : atmospheric constant k : Boltzman constant n : neutral number density C 1 is based on the atmospheric composition (CO 2, N 2, Ar) C 1 = 1.3063 10 -6 K·m·s 2 /kg known from laboratory measurements [Hinson et al., 1999].

27 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 27 Ideal gas law relates Pressure, Temperature and Density Hydrostatic equilibrium in well-mixed atmosphere: temperature can be derived directly from neutral number density Calculation of Pressure and Temperature

28 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 28 Ideal gas law relates Pressure, Temperature and Density Hydrostatic equilibrium in well-mixed atmosphere: temperature can be derived directly from neutral number density Calculation of Pressure and Temperature upper boundary condition

29 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 29 Upper boundary condition of temperature T up = 150 K T up = 160 K T up = 170 K

30 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 30 Level 4 Neutral Atmosphere Data Processing Flow Chart Input: Refractivity Profile Calculation of Neutral Number Density Calculation of Temperature and Pressure Main Output: Profiles of Temperature, Pressure and Density

31 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 31 Level 4 The Ionosphere

32 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 32 The Electron Density f 0 : Radio link frequency N e : electron density C 3 = 40.31

33 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 33 The Electron Density

34 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 34 2007 Autumn 2005 Autumn 2005 Spring Temperature Profiles Northern Hemisphere 35.0°N

35 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 35 2007 Autumn 2005 Autumn 2005 Spring Temperature Profiles Northern Hemisphere Typical daytime profile middle latitude 35.0°N

36 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 36 2007 Autumn 2005 Autumn 2005 Spring Temperature Profiles Northern Hemisphere morning profile inversion in boundary layer 35.0°N

37 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 37 2007 Autumn 2005 Autumn 2005 Spring Temperature Profiles Northern Hemisphere Stationary wave structures 35.0°N

38 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 38 Comparison with Model: middle latitudes MaRS GCM low dust GCM med. dust GCM high dust

39 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 39 Comparison with Model: 60° N MaRS GCM low dust GCM med. dust GCM high dust

40 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 40 Comparison with Model: 63° N MaRS GCM low dust GCM med. dust GCM high dust

41 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 41 Comparison with Model: Winter Night MaRS GCM (LMD) Temperature [K] altitude [km] planetary latitude [deg]

42 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 42 Autumn profiles L s = 250° – 265° L s = 227° – 235° 2005 2007

43 Rosetta_CD\PR\what_is_RS_v4.ppt, 04.09.2015 18:39AM, 43 Autumn & Winter profiles L s = 250° – 265° L s = 227° – 235° L s = 345° – 15°

Download ppt "Rosetta_CD\PR\what_is_RS.ppt, 04.09.2015 18:39AM, 1 Mars Express Radio Science Experiment MaRS MaRS Radio Science Data: Level 3 & 4 The retrieval S.Tellmann,"

Similar presentations

Rosetta_CD\PR\what_is_RS_v4.ppt, 09.02.2014 22:45AM, 1 Mars Data Workshop Mars Express Radio Science MaRS Data Products, Part II Martin Pätzold, Silvia.

Rosetta_CD\PR\what_is_RS_v4.ppt, :45AM, 1 Mars Data Workshop Mars Express Radio Science MaRS Data Products, Part II Martin Pätzold, Silvia.
Eyk Bösche et al. BBC2 Workshop, Oktober 2004: Eyk Bösche et al. BBC2 Workshop, Oktober 2004: Simulation of skylight polarization with the DAK model and.

Eyk Bösche et al. BBC2 Workshop, Oktober 2004: Eyk Bösche et al. BBC2 Workshop, Oktober 2004: Simulation of skylight polarization with the DAK model and.
Basics & Motivation Technique & Observations Fits & Measurements Summary & Outlook Atmospheric Wave Workshop ESTEC 11/10/2011 Tobias Stangier I st Physics.

Basics & Motivation Technique & Observations Fits & Measurements Summary & Outlook Atmospheric Wave Workshop ESTEC 11/10/2011 Tobias Stangier I st Physics.
1 Ionospheres of the Terrestrial Planets Stan Solomon High Altitude Observatory National Center for Atmospheric Research

1 Ionospheres of the Terrestrial Planets Stan Solomon High Altitude Observatory National Center for Atmospheric Research
Chapter Fifteen: Radio-Wave Propagation

Chapter Fifteen: Radio-Wave Propagation
Air Pressure and Winds III

Air Pressure and Winds III
Atmospheric Refraction

Atmospheric Refraction
Session 2, Unit 3 Atmospheric Thermodynamics

Session 2, Unit 3 Atmospheric Thermodynamics
Stellar Interior. Solar Facts Radius: –R  = 7  10 5 km = 109 R E Mass : –M  = 2  10 30 kg –M  = 333,000 M E Density: –   = 1.4 g/cm 3 –(water is.

Stellar Interior. Solar Facts Radius: –R  = 7  10 5 km = 109 R E Mass : –M  = 2  kg –M  = 333,000 M E Density: –   = 1.4 g/cm 3 –(water is.
METO 621 Lesson 5. Natural broadening The line width (full width at half maximum) of the Lorentz profile is the damping parameter, . For an isolated.

METO 621 Lesson 5. Natural broadening The line width (full width at half maximum) of the Lorentz profile is the damping parameter, . For an isolated.
Lesson 2 AOSC 621. Radiative equilibrium Where S is the solar constant. The earth reflects some of this radiation. Let the albedo be ρ, then the energy.

Lesson 2 AOSC 621. Radiative equilibrium Where S is the solar constant. The earth reflects some of this radiation. Let the albedo be ρ, then the energy.
Temperature, pressure, and winds. Review of last lecture Earth’s energy balance at the top of the atmosphere and at the surface. What percentage of solar.

Temperature, pressure, and winds. Review of last lecture Earth’s energy balance at the top of the atmosphere and at the surface. What percentage of solar.
Determination of upper atmospheric properties on Mars and other bodies using satellite drag/aerobraking measurements Paul Withers Boston University, USA.

Determination of upper atmospheric properties on Mars and other bodies using satellite drag/aerobraking measurements Paul Withers Boston University, USA.
IPPW- 9 Royal Observatory of Belgium 20 June 2012 0 Von Karman Institute for Fluid Dynamics Obtaining atmospheric profiles during Mars entry Bart Van Hove.

IPPW- 9 Royal Observatory of Belgium 20 June Von Karman Institute for Fluid Dynamics Obtaining atmospheric profiles during Mars entry Bart Van Hove.
2 nd GRAS SAF User Workshop 1 Radio Occultation and Multipath Behavior Kent Bækgaard Lauritsen Danish Meteorological Institute (DMI), Denmark 2 nd GRAS.

2 nd GRAS SAF User Workshop 1 Radio Occultation and Multipath Behavior Kent Bækgaard Lauritsen Danish Meteorological Institute (DMI), Denmark 2 nd GRAS.
GPS / RO for atmospheric studies Dept. of Physics and Astronomy GPS / RO for atmospheric studies Panagiotis Vergados Dept. of Physics and Astronomy.

GPS / RO for atmospheric studies Dept. of Physics and Astronomy GPS / RO for atmospheric studies Panagiotis Vergados Dept. of Physics and Astronomy.
Solar System Physics I Dr Martin Hendry 5 lectures, beginning Autumn 2007 Department of Physics and Astronomy Astronomy 1X Session 2007-08.

Solar System Physics I Dr Martin Hendry 5 lectures, beginning Autumn 2007 Department of Physics and Astronomy Astronomy 1X Session
the Ionosphere as a Plasma

the Ionosphere as a Plasma
GPS radio occultation Sean Healy DA lecture, 28th April, 2008.

GPS radio occultation Sean Healy DA lecture, 28th April, 2008.
Chapter 17 Notes: The Atmosphere. What is the Atmosphere? The atmosphere can be defined as the portion of planet earth that contains gas. Weather can.

Chapter 17 Notes: The Atmosphere. What is the Atmosphere? The atmosphere can be defined as the portion of planet earth that contains gas. Weather can.

Similar presentations

Ads by Google