Studies of Radiation-Driven and Buoyancy-Driven Fluid
Flows and Transport
(supported by NASA Grant No.
NAG3-1653)
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ABSTRACT
It is well known that
radiative heat transport influences many types of buoyant flows due to its effect
on the temperature and thus density field in the fluid medium. It is of
interest to study gaseous flows driven solely by radiation in the absence of
buoyancy, particularly because of its application to astrophysical flows that
are well known from astronomical observations and numerical simulation.
However, no laboratory-scale experiments of this phenomenon have ever been
conducted. To study the possibility of obtaining such flows in the laboratory,
an apparatus was built to produce large temperature differences (T) up to 300K in a gas confined between flat parallel plates.
SF6 was used as the radiatively-active gas
because its Planck absorption length is much shorter than that of any other
common non-reactive gas. The NASA-Lewis 2.2 second drop tower was used to
obtain reduced gravity in order to suppress buoyancy effects. To image the
resulting flows, a laser shearing interferometer was employed. Initial results
indicate the presence of flow that does not appear to be attributable to the
residual flow resulting from buoyancy influences before the drop. For T > 70K, slight deformations in the interferometer fringes
seen at lower T became large unsteady swirls. Such behavior did not occur
for radiatively-inactive gases, suggesting that a flow
driven solely by radiation was obtained in SF6 and to a lesser
extent in CO2. This was more pronounced at higher pressures and
plate spacings, consistent with our scaling
predictions.
INTRODUCTION
Radiation-driven flows
occur in many gases and liquids that are neither completely transparent nor
completely opaque to electromagnetic radiation. This effect of importance to
many practical problems including glass and semiconductor processing;
oceanographic or atmospheric flows with application to global climatic change;
astrophysical flows; plasma physics; combustion systems; solar energy
collection; nuclear explosions and heat transfer in inhabited enclosures.
We have proposed that
flow driven solely by radiative effects without imposed hydrodynamic or
hydrostatic pressure gradients may be possible for the following reason. If a
parcel of gas receives slightly more heating than the surrounding gas, its
temperature increases. In gases with a strongly temperature-dependent Planck
absorption length (lp) such as SF6,
this temperature increase results in a significant decrease in the
absorptivity, which in turn causes an increase in the radiative conductivity.
For SF6 the radiative conductivity is roughly proportional to T5.
The local increase in temperature would encourage further heat transfer
throughout the gas and upon coupling with thermal expansion effects, may
produce a flow. Evidence of this instability has been found in _g combustion
experiments (ref. 1). In combustible CH4-O2 and H2-O2
mixtures diluted with SF6, a flame structure characterized by the
sudden fingering of an evolving front has been observed, particularly at high
pressures. The fingering occurred in SF6-diluted mixtures but not N2-,
Ar- or CO2-diluted mixtures, which is to
be expected if the proposed instability mechanism is present because lp/T is much larger for SF6 and because at the
conditions tested only SF6 is optically thick. For the current
study, we examined radiative flow instability in a non-reacting gas at µg
with an imposed heat source of known character, rather than a chemical reaction
whose heat release characteristics are intimately coupled to the thermal field.
Many theoretical and
computational studies of radiation-driven flows appear in the astrophysical
literature (refs. 2 - 4) because of its relevance to solar flares, the
formation of galaxies, etc., yet no experimental studies of analogous flows
have been conducted in a laboratory setting. Scaling analyses indicate that at
earth gravity, this flow would be overwhelmed by buoyant convection even in a
highly radiatively-active gas such as SF6.
Depending on the orientation, buoyancy would either suppress the instability or
would be overshadowed by Rayleigh-Benard convection.
Consequently, microgravity conditions are needed for an experiment test for the
existence of this type of flow. The intent of the current experimental study is
to explore aspects of radiation-dominated fluid flows which
cannot be studied at earth gravity.
EXPERIMENTAL APPARATUS AND PROCEDURES
Experimental
Background
A modified Rayleigh-Benard type of apparatus was utilized for these
experiments. It consisted of two parallel flat plates with a gap between them
varying from 2 to 5 cm (see Fig. 1.) The upper hot plate was resistively heated
and the lower cold plate was thermoelectrically or water
cooled. 1-cm thick plates were used to ensure uniform temperature across
the plate and to ensure that their thermal response time was very large
compared to the low-gravity test duration. A large temperature difference (up
to 300K) could be maintained between the two plates. Locating the hot plate on
top of the cold plate minimized the buoyant flow in the test section before the
drop, however, some buoyant flow within the test
section was unavoidable because of the flow off of the top of the hot plate.
This flow is undesirable because a finite amount of time is required for it to
decay once buoyancy is removed, i.e., when the drop begins. This makes
it more difficult to determine whether flow observed during _g conditions is a
result of radiative effects or decaying buoyant flow. A set of baffles and
blocks of insulation was used to minimize this flow. Also, comparisons were
made between tests conducted at similar earth-gravity Grashof
numbers with radiative and non-radiative gases (see below). The plates and
their supporting structure are housed in a well-insulated,
sealed aluminum chamber. The NASA-Lewis 2.2 second
drop tower facility was employed to obtain low-gravity conditions.
Figure 1. Test apparatus block diagram (expanded in
vertical direction for clarity).
Measurement
Techniques
Two types of
measurements were made: thermal properties and imaging. The thermal properties
are used to verify the 1-d transport equations, to quantify spatial and
temporal deviations from steady and/or 1-d profiles (i.e., to identify
instabilities) and to quantify the amplitude and spectrum of the disturbances.
Thermal properties were measured by thermocouples and radiometers. Imaging
provided qualitative information on the overall flow. Temperatures were
measured with fine-wire thermocouples (50 µm) were placed at several locations
within the gas. Since their size was much smaller than the scales under
consideration, their influence on heat transport can be considered negligible.
To measure fluctuations in radiant energy flux, two thermopile-type
narrow-angle shielded radiometers were placed in the gap between the plates.
They were oriented parallel to each other, but separated by a horizontal
distance of 8 cm, in order to obtain a relative measurement of fluctuations in
radiant energy present at any given time during the drop test.
A
shearing interferometer (Fig. 2) was developed for flow imaging in the drop
tower, since the gases tested are transparent at visible wavelengths. A great
deal of attention was given to its sensitivity as well as its ruggedness so
that quantitative measurements as well as qualitative information may be
obtained.
Figure 2. Interferometer and drop frame block diagram.
Radiative Media
The test gases were
chosen based on their radiative properties. SF6 and CO2
were used in the bulk of the tests to represent strongly radiating gases.
Although SF6 has the smallest lp
and the most rapid decrease in lp as T
increases, initial drop tests performed with CO2 also showed
considerable radiatively-driven flow. N2, a nonradiating
medium, was utilized to determine if any flow would be encountered in the
absence of radiative effects.
RESULTS AND DISCUSSION
At higher pressures and
temperatures, flows were observed in SF6 that did not appear to be a
residual of the buoyancy-induced flow present prior to the drop tests. Drop
tests performed with high pressure CO2 also
produced significant flow. The tests with N2 did not produce any
visual indication of the presence of fluid motion other than the decay of the
buoyant flow present before the drop. Since N2 is not a radiating
gas, this is in accordance with the proposal outlined above.
Figure 3 shows an
interferometer image of the flow in SF6 at 2 atm
taken near the end of the drop test. The large deformation of
the fringes in the right half of the frame denote a sharp density
gradient and the presence of flow. This is the most likely time frame for a radiatively-driven flow to materialize, since the estimated
time scale for the onset of radiation at microgravity ranges from .5-5 seconds.
Figure 3. Interferometer image of radiation-driven flow at µg taken near end of drop period. Gas: SF6; pressure: 2 atm; plate spacing: 2 cm; T=105K. Note strong fringe deformation in fringes in upper right of image indicating density gradient. Fringes are parallel lines when no flow is present.
Although the CO2
did not exhibit as much flow as SF6, tests conducted at pressures
above 2 atm. revealed a significant amount of fluid motion. In fact, CO2
tests and N2 tests performed at the same Grashof
number were noticeably different. Figures 4 and 5 show interferometer images
from CO2 and N2 drop tests, respectively, taken near the
end of the drop. The CO2 image shows several regions where fringe
deformation is significant, while in the N2 test only minimal fringe
deformation is observed. It is significant that even though the earth-gravity Grashof numbers are nearly the same for these two cases, in
the CO2 case the flow persists throughout the drop whereas in N2
the flow is steadily decaying, indicating that in the CO2,
radiatively-induced flow dominates.
Figure 4. Interferometer image of radiation-driven flow at µg taken near end of drop period. Gas: CO2; pressure: 3.2 atm; plate spacing: 2 cm; Grashof number at earth gravity: 1.4 x 106.
Figure 5. Interferometer image of decaying buoyant flow at µg taken near end of drop period. Gas: N2; pressure: 4.6 atm; plate spacing: 2 cm. Grashof number at earth gravity: 9.2 x 105.
CONCLUDING REMARKS
Additional drop tests
will be used to further isolate and eventually quantify the flows. In
particular, the spectra of the temperature and radiative flux fluctuations will
be measured and compared these to theoretical predictions from the
astrophysical literature. The NASA-Lewis drop tower only provides 2.2 seconds
of microgravity, so the long-term behavior of these radiatively-driven
flows is unknown. The short time duration also prohibits the complete decay of
the residual effects of buoyant flow at one-g. The interferometer images
indicate that more microgravity time is needed to fully characterize and
understand the phenomena of radiation-driven flows.
ACKNOWLEDGMENTS
We gratefully
acknowledge the support of the staff at the 2.2 second
drop tower at NASA-Lewis Research Center.
REFERENCES
1. Lozinski,
D., Buckmaster, J. D., Ronney, P.
D.: Absolute flammability limits and flame balls in optically thick mixtures. Combustion and Flame 97, 301 (1994).
2. Field, G. B.: Thermal
instability. Astrophys. J. 142, 531
(1965).
3. Balbus,
S. A.: Local dynamic thermal instability. Astrophys.
J. 303, L79 (1986).
4. Karpen,
J. T., Picone, J. M., Dahlberg, R. B.: Nonlinear
thermal instability in the solar transition region. Astrophys.
J. 324, 590 (1988).