ATMOSPHERIC TURBULENCE IN ASTRONOMY
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Transcript of ATMOSPHERIC TURBULENCE IN ASTRONOMY
2Zanjan, July 2001
List of Themes
How to find the ideal site...and keep it good?
Optical Propagation through Turbulence
– Mechanical and Thermal
– Index of Refraction
– Signature on ground based observations
– Correction methods Integral Monitoring Techniques
– Seeing Monitoring
– Scintillation Monitoring Profiling Techniques
– Microthermal Sensors
– Scintillation Ranging Modelling Techniques
7Zanjan, July 2001
Atmospheric Turbulence
Big whorls have little whorls, Which feed on their velocity;
Little whorls have smaller whorls,And so on unto viscosity.
L. F. Richardson (1881-1953)
Vertical gradients of potential temperature and velocity determine the conditions for the production of turbulent
kinetic energy
25.02
dzdu
dzd
T
gRi
8Zanjan, July 2001
= dissipation rate of turbulent kinetic energy (~u^3/L, m^2s^-3)
= kinetic viscosity (in air, 15E-6 m^2 s^-1)
4
13
l
Atmospheric Turbulence
Inner (dissipation) scale:(l~0.1mm in a flow of velocity u=10m/s)
In a turbulent flow, the kinetic energy decreases as the -5/3rd power of the spatial frequency (Kolmogorov, 1941)
within the inertial domain ]l, L[
Outer (injection) Scale: L(L= 100m or more in the free atmosphere, less if pure convection)
9Zanjan, July 2001
Structure function of the temperature fluctuations
(Tatarskii, 1961)
3D Spectrum (Tatarskii, 1971)
3/112033.0)( fCf TT
3
222()( rCrrTrTrD TT
Atmospheric Turbulence
within the inertial domain ]2/L,2 /l[ but L is now the size of the thermal eddies
10Zanjan, July 2001
Index of refraction of air
Assuming constant pressure and humidity, n varies only due to temperature fluctuations, with the same structure function
matCT
PC Tn 5.01080 2
2
262
T
eP
Tn 48101052.71
106.771 23
6
Atmospheric Turbulence
P,e (water vapor pressure) in mB, T in K, Cn2 in m-2/3
11Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric Turbulence
The Long Exposure Parameters
12Zanjan, July 2001
Fried parameter: ( meter, ^6/5)
Seeing: (radian, ^-0.2) 0
98.0)(r
FWHM
53
0
22
0 )()sec(2
423.0)(
dhhCr n
Optical Propagation
The Signature of Atmospheric Turbulence
Easy to remember: r0=10cmFWHM=1” in the visible (0.5m)
13Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric TurbulenceS= 0.7 à 2.2 um FWHM=0.056 “
S=0.3 à 2.2 um FWHM=0.065 “
0I
IS
0rFWHM
Seeing = FWHM
Strehl Ratio
14Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric Turbulence
The Short Exposure Parameters
15Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric Turbulence
Shorter exposures allow to freeze some atmospheric effects
and reveal the spatial structure of the wavefront corrugation
Sequential 5s exposure images in the K band on the ESO 3.6m telescope
16Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric TurbulenceA Speckle structure appears when the exposure is
shorter than the atmosphere coherence time 0
1ms exposure at the focus of a 4m diameter telescope
V
r00 31.0
53
0
2
0
352
)(
)()(
dhhC
dhhVhC
V
n
n
17Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric TurbulenceHow large is the outer scale?
A dedicated instrument, the Generalized Seeing Monitor
(GSM, built by the Dept. of Astrophysics, Nice University)
18Zanjan, July 2001
Optical Propagation
The Signature of Atmospheric TurbulenceHow large is the outer
scale?
Overall Statistics for the Wavefront Outer Scale
At Paranal: a median
value of 22m was found. Ref: F. Martin, R. Conan, A. Tokovinin, A. Ziad, H. Trinquet, J. Borgnino, A. Agabi and M. Sarazin; Astron. Astrophys. Supplement, v.144, p.39-44; June 2000
http://www-astro.unice.fr/GSM/Missions.html
19Zanjan, July 2001
Structure function for the phase fluctuations:
3
5
0
88.6
r
ffD
The number of speckles in a pupil of diameter D is (D/r0)^2
Optical Propagation
The Signature of Atmospheric Turbulence
20Zanjan, July 2001
Why looking for the best seeing if turbulence can be corrected?
Adaptive optics techniques are more complex (ND/r0^2),
less efficient (Strehlexp(r0/D^2))
and more expensive to implement
for bad seeing conditions
Optical Propagation
The Signature of Atmospheric Turbulence
22Zanjan, July 2001
Local Seeing
Flow Pattern Around a BuildingIncoming neutral flow
should enter the building to contribute to flushing, the height
of the turbulent ground layer
determines the minimum height of
the apertures. Thermal exchanges
with the ground by re-circulation inside the
cavity zone is the main source of
thermal turbulence in the wake.
23Zanjan, July 2001
Mirror Seeing
When a mirror is warmer that the air in an undisturbed enclosure, a convective equilibrium (full cascade) is reached after 10-15mn. The limit on the convective cell size is set by the mirror diameter
24Zanjan, July 2001
LOCAL TURBULENCE
Mirror Seeing
The warm mirror seeing varies slowly with the thickness of the convective layer: reduce height by 3 orders of magnitude to divide mirror seeing by 4, from 0.5 to 0.12 arcsec/K
The contribution to seeing due to turbulence over the mirror is given by:
25Zanjan, July 2001
Mirror Seeing
When a mirror is warmer that the air in a flushed enclosure, the convective cells cannot reach equilibrium. The flushing velocity must be large enough so as to decrease significantly (down to 10-30cm) the thickness turbulence over the whole diameter of the mirror.
The thickness of the boundary layer over a flat plate increases with the distance to the edge in the and
with the flow velocity.
26Zanjan, July 2001
Thermal Emission Analysis
VLT East Landscape
Access Asphalt Road 19 Feb. 1999 0h56 Local Time Wind summit:
ENE, 7m/s Air Temp summit:
13.5C
*>14.9°C
*<-1.3°C
0.0
2.0
4.0
6.0
8.0
10.0
12.0
14.0
27Zanjan, July 2001
Thermal Emission Analysis
VLT Unit Telescope
UT3 Enclosure 19 Feb. 1999 0h34 Local Time Wind summit:
ENE, 4m/s Air Temp summit:
13.8C
*>15.0°C
*<1.8°C
2.0
4.0
6.0
8.0
10.0
12.0
14.0
28Zanjan, July 2001
Thermal Emission Analysis
VLT South Telescope Area
Heat Exchanger 10 Oct. 1998 11h34 Local Time Wind summit: North,
3m/s Air Temp summit:
12.8C
*>25.1°C
*<-1.6°C
0.0
5.0
10.0
15.0
20.0
25.0