using speed of sound measurements to constrain the huygens probe descent profile

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

1

ILEWG

Using speed of sound measurements to constrain the Huygens Probe descent profile

H. Svedhem, J-P. LebretonESA/RSSD, NL

J. Zarnecki, B. HatiOpen University, UK

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

2

ILEWGJohn Tyndall’s atmospheric

experiment 1875

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

3

ILEWG

About 100 years later Jean-Pierre Lebreton proposes to fly an acoustic sensor to Titan

• We now talk about miniaturisation…..

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

4

ILEWG

The Acoustic Properties Investigation (API) of the Surface Science Package on Huygens

• API has two sets of sensors and one card of electronics incorporated in to the SSP Top Hat and electronics box– API-S, (sounder) is a monostatic SODAR for detection of

atmospheric precipitation during the descent, surface characterisation during the last phase of the descent and detection of sea depth in case of landing in a liquid.

– API-V, (velocity) will measure the speed of sound across a 15 cm long path during the descent from an altitude of about 50 km down to the surface, and in the liquid in case of landing in a liquid.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

5

ILEWG

API-S

• The API-S in principle works as a conventional SODAR.• The return signal is proportional to the number density of

the scattering particles in the scattering volume and to the particle diameter to the 6th power. (Rayleigh scattering)

• For both volume scattering and surface scattering the signal is inversely proportional to the square of the distance.

• The similarities to Radars are striking. By coincidence the wavelength of the API-S and the probe altimeter are both about 2 cm. Comparisons will be useful.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

6

ILEWG

API-S Modes 1/2

• Atmospheric sounding mode, >7km. Search for hydrometeors and turbulence. Pulse length 10 ms. Binned samples for the closes 50 m are stored each 2 seconds.

• Surface proximity mode,7km>h>1km. Pulse length 10 ms. Search for surface return AND hydrometeors. Binned samples at higher resolution around the surface bin each 3 seconds.

• Near surface mode. h<1km. Pulse length 2 ms. Search for surface structure and topography. Binned samples at highest resolution around the surface bin each second.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

7

ILEWG

API-S Modes 2/2

• Surface mode. After impact, search for depth of liquid. Pulse length 10 ms. Send one pulse, listen for 10 s. Binned data around the maximum return.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

8

ILEWG

API-V mode

• One mode only at h<60 km. Sensor A transmits a pulse and start a 4 Mhz counter, sensor B receives the pulse and stops the counter. Immediately afterwards the sequence is repeated in the reverse direction. Both data are stored. Frequency of measurement is 1 s.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

9

ILEWG

API-S reflectivity factors, Z

Hydrometeor condition Precipitation rate Z[mm/h] [mm6m-3]

Cloud 0.001 to 1Fog 0.01 to 1Drizzle 1 10Light Rain 1 200Heavy Rain 25 33000Light Snow 1 1000Heavy Snow 10 40000

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

10

ILEWG

API-S Performance

-40

-30

-20

-10

0

10

20

30

0 0.5 1 1.5 2 2.5 3 3.5 4 4.5

log Z [mm6m-3]

Echo

leve

l [dB

, ref

20

uPa]

d=50 md=10 mNoise level

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

11

ILEWG

Performance API-S

• Reflectivity factors on earth are known, (previous graph). Titan situation is hard to estimate.

• Garry (1996)estimated, based on data from Toon et al (1988) that the reflectivity factors at Titan are too low to be detected by API-S. The method for these calculations was however unconventional and seem to give too pessimistic results.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

12

ILEWG

API-V pressure sensitivity

0.01

0.1

1

10

100

0 200 400 600 800 1000 1200 1400

Pressure [mBar]

Rec

eive

r out

put [

mV]

N=10N=1

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

13

ILEWG

Error analysis

• M = ·R · T · c-2

M/M=((T/T)2+ (2c/c)2)1/2

• For the gasses at the temperatures we have c is about 200 m/s, we get with 250 ns resolution and 15 cm path, 2c/c 7 ·10-4. T 0.1 K which at 100 K gives T/T = 10-3. The contributions are thus of the same order of magnitude.

M/M 1.2 ·10-3 .

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

14

ILEWG

Empirical approach, gas

• In stead of calculating the mean molecular weigh one may go directly to find mixing ratios from calibrated measurements.

• The mixing ratio will be accurate to better than 1 % for binary gasses. The number is dependent on which species are involved.

• This will work well for binary mixtures but is difficult for mixtures of three or more gasses (or liquids)

• For mixtures of three or more components a test of the expected sound speed can give useful constraints to measurements by other instruments.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

15

ILEWG

Empirical approach, liquid

• For the liquids the sound speeds are typically ten times higher while the resolution remains 250 ns. Hence the c/c is the dominating error.

• The spread in sound speed is larger and therefore a precision in the mixing ratio similar to that of gasses will be achieved, i.e. about 1% for binary mixtures.

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

16

ILEWG

API-V in Nitrogen gas

150

170

190

210

230

250

270

290

310

-190 -170 -150 -130 -110 -90 -70 -50Temperature [deg C]

Soun

d sp

eed

[m/s

]

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

17

ILEWG

API-V in 100% Methane gas

200

250

300

350

400

450

500

-200 -150 -100 -50 0 50Temperature [deg C]

Soun

d sp

eed

[m/s

]

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

18

ILEWG

API-V in 100% Ethane gas

245

250

255

260

265

270

275

280

285

290

-100 -80 -60 -40 -20 0Temperature [deg C]

Soun

d sp

eed

[m/s

]

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

19

ILEWG

API-V in 100% Ethane liquid

1100

1300

1500

1700

1900

2100

-190 -170 -150 -130 -110 -90 -70 -50Temperature [deg C]

Soun

d sp

eed

[m/s

]

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

20

ILEWG

API-V in 100% Methane liquid

1320

1340

1360

1380

1400

1420

1440

1460

1480

1500

-180 -175 -170 -165 -160Temperature [deg C]

Soud

spe

ed [m

/s]

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

21

ILEWG

What about the miniaturisation, did it work

out?

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

22

ILEWG

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

23

ILEWG

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

24

ILEWG

Planetary Probe Atmospheric Entry Workshop, Lisbon, 6-9 October 2003

25

ILEWG