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Note on Thermal Properties of Mars C https://ntrs.nasa.gov/search.jsp?R=19650016474 2020-03-17T01:44:24+00:00Z~~ CORE Metadata, citation and similar papers at core.ac.uk Provided by NASA Technical Reports Server NASr-21(07) MEMORANDUM RM-4551-NASA APRIL 1985 NOTE ON THERMAL PROPERTIES OF MARS C. Leovy This research is sponsored by the National Aeronautics and Space Administration under Contract No. NASr-21. This report does not necessarily represent the views of the National Aeronautics and Space Administration. 744 I700 MAIN I1 SANlA MONICA CALlfORNIA * *0101 c This Memorandum, using available data on Mars, helps to prepare the way for extensive numerical calculations of the general circula- tion to be conducted later by another RAND researcher. It supports other studies in finding that the Martian surface is finely powdered and demonstrates how radiometric measurements can be used for such purFoses. It was prepared for the National Aeronautics and Space Administration under Contract NASr-21(07). 'V 'V - ABSTRACT d&JV As measured by Sinton and Strong, the variation of infrared emission from the surface of Mars with local time on Mars is here interpreted in terms of { simplified theory of diurnal temperature variations, in which the effect of the atmosphere is included. The results suggest a very law thermal conductivity for the upper few centimeters of the Martian ground. Such law conductivities appear to be possible only if the material composing these layers is very fine powder having a characteristic size of not more than a few microns. If a linear relationship is assumed between convective heat transfer and surface temperature, the appropriate constant of 2 proportionality is on the order of cal per cm sec deg. dJ),&d -vii- CONTENTS PREFACE. ........................... iii ABSTRACT. o o o . V Section Io INTRODUCTION .. e . e . o 1 11. DETERMINATION OF THE THEW PARAMETERS. ....... 2 111. THEMARTIAN GROUND. ................. 9 IV. THE MARTIAN ATMOSPHERE ................ 13 17 -1- c I. INTRODUCTION In analyzing their observations of the,variationI with local time of Ithe apparent surface temperature on Mars6 Sinton and Strong (1960) find it impossible to match both the amplitude and the phase found in the observations with a theory that neglects conduction and convection of heat into the atmosphere.' They suggest that anianalysis that includes atmospheric processes could determine something about the meteorology of the planet. This paper is an attempt to carry out such an analysis, using a simple theory of the surface tempera- ture variation, developed by Lhnqvist (1962, 1963). \ -2 - 11. DETERMINATION OF THE THERMAL PARAMETERS Lldnnqvist assumes that a simple heat conduction law with thermal conductivity, k, describes the heat flow in the ground, while Newton’s law of cooling describes interaction among the surface, atmosphere, and space. Thus the heat balance boundary condition at the ground, z = 0, is given by where To is the temperature, S is the solar radiation flux, and h and T are parameters related to radiative processes as well as to h conduction and convection in the atmosphere. Their interpretation will be clarified in Sect. 4. Although Eq. (1) is perhaps the simplest boundary condition that can include the effect of atmospheric heat transfer, its applicability to the problem of the terrestrial diurnal temperature wave has been demonstrated by 11 Lonnqvist (1963) under a variety of conditions. The temperature in the ground and the solar radiation flux are represented by Fourier series in time: W T = Tm + C (pj cos jwt + q j sin jut) j=1 00 S = b -+ C (bj cos jwt + a sin jwt) , (3) O jsl j -3 - c and it is further assumed that S is proportional to the cosine of the angle of incidence of the solar radiation, so that S = C(sin (p sin 6 + cos cp cos 8 cos wt) (41 for tan cp tan 8 + cos wt > 0 , s=o < for tan cp tan 8 + cos Cot = 0 , where (p is latitude, 6 is solar declination, C the solar constant, and w the angular frequency of rotation of the planet. Eqs. (4), (4a) are valid if atmospheric attenuation of solar radiation is negligible. From the heat conduction equation, and the boundary condition Eq. (l), it follows that + (1+- B”,) cos 4} ’ -4 - 4 where 1/2 P = (1/2 pckru) , p and c are the density and specific heat of the ground, m = sin cp cos 6 n = cos cp sin S -1 -1 T = ru cos (-m/n) , and the mean temperature, Tm, is given by b = h(Tm - Th) 0 in the absence of any diurnally averaged temperature gradient in the ground. It follows that all the properties of the diurnal temperature wave depend on three parameters: h/P, m/n, and nC/rrP. Figure 1 shows the dependence of two of these properties on h/P: the phase lag of the maximum temperature after local noon, and the absolute diurnal temperature range in units of (nc/nP) for the case m = 0, corresponding to equatorial equinox conditions. We see that both phase lag and temperature range for a given value of (nC/rrg) decrease monotonically with increasing h/p; these two curves provide a guide for fitting observed ground temperature variations. Figure 2 illustrates an attempt to fit the observations of Sinton and Strong by adjusting (nC/nP) and (h/p) with (m/n) = 0. (Their observations were all within a few latitudinal degrees of the equator.) We see that a good fit to the data is obtained with (h/$) = 6, and (nC/nP) = 236.5, T = 226. A somewhat less satisfactory fit is m obtained with (h/P) = 10, and (nChP) = 379. The figure also shows -5 - 1 I I I I I I I I 0 8 .I4 rl 2 rl xo 0 v) xo U 4 d m . WO 2 u 0 h U v) aJaJ Fch a (da d (d nrn KaJ C Wd.. 0 M U E: d ma .d v) W 0 2- .n rd aJN U hN a 3 a u II 0 U n h rl d 0 aJE U h 3 0 W W 0 U rn h .d Fc W W" (d e U w (d I I I I I I 1 I I -u W 0 0 0 0 0 0 0 E U m cu 3 z N .a F N. bD .rl -7 - * data points from Sinton and Strong for observations mainly on dark areas, and some points from Gifford’s analysis (1956) of early Lowell Observatory observations by Coblentz and Lampland. Table 1 summarizes the values of h, (p~k)”~,and k if pc = .30 cals/cm3 OK corresponding to these data; the values for Gifford’s data and the dark area data are estimates based on Fig. 1. It has been assumed that the applic- 2 able solar constant, corrected for an albedo of .15, is 0.80 cal/cm min. Note that the values of (pck)’l2 from Sinton and Strong’s data lie between the values suggested by these authors when atmospheric effects are neglected [.001 < (pcl~)”~< .004]. These values are therefore not very sensitive to the assumed atmospheric exchange process. -8- Table 1 VALUES OF (h/p), (nC/np), h, and (pck)lI2 CORRESPONDING TO FOUR DIFFERENT MODELS OF THE DIURNAL TEMPERATURE VARIATION OF THE MARTIAN SURFACE 1/2 Units h and (pck) are cals cgs 0 The last row gives values of k in cals/cm sec K 3 under the assumption that p = 2 gms/cm , c = .15 cals/gm OK. Sinton and Strong Parameter Sinton and Strong (dark areas) Giff ord 6 10 16 1.3 236.5 379 389 50 h i.~ 1.0 1.6 x 1. o (pck)lj2 .0024 .0015 .0015 .Oll x k ,I .2 x I .8 x .8 -9- 111. THE MARTIAN GROUND The value pc .30 cal/cm3 OK used in deriving the values of k in Table 1 may be considered representative of powdery limonite, or of fine quartz sands. The low values of (pck)'j2 in Table 1 strongly support the hypothesis that the Martian surface consists of finely divided material. Measurements of polarization (Dolphus, 1961), albedo, and color (Sharonov, 1961) suggest some form of hydrated ferric oxide such as limonite as a primary constituent of the surface, although other materials cannot be ruled out. Little information is available on the thermal conductivities of dry, finely divided soils. Figure 3, based on Smoluchowski's data as given in International Critical Tables (National Research Council, 1926), shows the pressure variation of the thermal conductivity of six different powders. There is a strong suggestion of two distinct regimes, depending on the pressure: (a) at pressures greater than 50 mm Hg, k has a weak pressure dependence, and its magnitude depends primarily on the particular powder; (b) at pressures less than 30 mm Hg, k has a strong pressure dependence and depends primarily on particle size, while being almost independent of the particular pcwder. In the latter regime, over the particle-size range indicated, the approximate relation (where d is a characteristic particle dimension) appears to hold. Setting aside Gifford's temperature variation for the moment, the shaded ellipse in Fig. 3 appears to represent for Mars the most -10- 0 0 0 c aJ rl % P 0 Fc a 0 U d rn 0 a 0 Fc 0 .I4 g c a 3. rn rl aJ hl $4 $4 0 u (d aJ Fc (d a 10 0 a - (d -", CE .L I rn 9) E n N z E U 3 Fc 0 a' (d 7 W v 0 0 3 rn c a cn 7 \ \\ 0 Fc bo 0 Fc 0 I W rn A aJ M d (d Fc c aJ 0 N -I4 rn n aJ Ua aJt? E e .I4 aJ X 0 $4 a a I4 r( !? 6 X I P '13 i : 0 0 0 I .I4 c c c I bo I I rn Fc aJ J( n 5 z -11- I1 likely range of pressure (Kaplan, Munch and Spinrad, 1964) and thermal conductivity.
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