Introduction
With the creation of AMANDA (the Antarctic Muon and Neutrino Detector Array), we hope to open a new astronomical window, using neutrinos instead of light (Reference LowderLowder and others, 1991; Reference BarwickBarwick and others, 1992). The goal is to image the trajectories of ultra-high-energy neutrinos created throughout the Universe in very energetic processes such as take place in quasars and other Active Galactic Nuclei. Because the conversion rate of neutrinos into detectable particles is extremely small, the observatory must be huge, eventually of order 1 km3 in volume. All designs share the same idea: a three-dimensional array of large phototubes embedded in a transparent medium will look down at the cone of Cherenkov light emitted by an upward-moving muon into which a high-energy neutrino is transformed in passing upward through the Earth. Measurement of arrival times of Cherenkov photons at various phototubes enables the direction of the neutrino to be reconstructed. In contrast to other techniques, which propose to build an observatory in a deep lake or the deep ocean, all of the electronics in the present version of AMANDA sit on the surface of South Pole ice above cables that simply carry signals from the phototubes, and the imaging medium is essentially free of background light such as that due to radioactivity or bioluminescence.
To minimize cost, the strings of phototubes should he far apart and the spacing of phototubes on each string should be large, To reduce background due to downward-directed muons created in the Earth’s atmosphere, the array should be buried deeply and the phototube spacing should be large in order to give a long enough lever arm to determine trajectories very accurately. Our results from the first four strings, which were deployed during the 1993—94 drilling season, showed that Cherenkov light from downward muons propagated diffusively due to scattering from residual air bubbles at the depth interval 800-1000 m where the phototubes were located (Reference AskebjerAskebjer and others, 1995). Using a laser to send pulses of light (510 nm) down optical fibers to various depths, we measured the distribution of arrival times at phototubes at various distances from the emitter. From the excellent fits to a model of random walk with absorption, we were able to determine separately the absorption length (the e-folding distance for loss of photons at a particular wavelength) and the scattering length (the mean free path between scatterers). The result for the absorption length at 510 nm, λabs = 59 ± 3 m, is larger than that of the clearest ocean water and far larger than the values estimated for laboratory ice and for Lake Baikal. This large value of Aabs will permit us ultimately to construct a neutrino observatory at lower cost than we originally expected. The geometrical scattering length on bubbles, λbub, was found to be 11 cm at 800 m and to increase to 26 cm at 1000 m. In order to take maximum advantage of the information from Cherenkov wave-front arrival times, we plan to implant all future strings of AMANDA phototubes at depths sufficiently great that λbub is greater than about 20 m.
Figure 1 is a sketch showing the location of the first four AMANDA strings and the proposed location of the remaining six strings. In this paper we discuss the factors that must be considered in deciding how deep to implant the remaining six strings. Future plans to proceed to construction of a 1 km3 size neutrino observatory will depend on success in deploying these six strings and on results of measurements with them.
Fig. 1. The AMANDA high-energy neutrino observatory. The top four strings are frozen into the ice at the South Pole and are working. The lower six strings will be deployed at a greater depth to be discussed in this paper.
Time-Scale Model (Age Vs Depth)
To estimate the dust concentration as a function of depth, we require a model of age as a function of depth for South Pole ice. The most important ingredient of such a model is the accumulation rate as a function of time and distance upstream from the site Since almost no information on accumulation rate upstream from the South Pole has been published, there is little point in developing a sophisticated flowline model. We start with the information in Table 1 on deep cores in ice and on drilling sites. The first four rows are for Greenland sites and the last four are for Antarctic sites. The last row includes information about the South Pole site. No core deeper than 349 m has been obtained at this site.
Figure 2 displays age vs depth obtained from references at the bottom of Table 1. Wherever possible, we selected data based on absolute determination of age using stratigraphy (annual layers of high and low δ 18O values, of electrical conductivity, of dust or of dissolved impurities due, for example, to identifiable volcanic eruptions). In other cases, we followed the authors in associating patterns of δ 18O, 10Be and dust concentrations from core to core with dated events such as the Last Glacial Maximum. To complete the picture, we selectively used ages based on ice-flow models reported by the various authors. In case of any discrepancies from one author to another, we used the most recent work or the one least dependent on flow models. For the Camp Century core, ages estimated from Fourier spectral analyses of δ 18O profiles and comparisons with features in the deep-sea record differ by a factor ∼2 far times greater than ∼10kyear. Various reasons have been given for the irregularities in the Camp Century time-scale near the bottom of the core (Reference DansgaardDansgaard and others, 1982). We decided to include only the data for depths more than 280 m above bedrock, for which stratigraphy is said to be accurate to ±30% (Reference Hammer, Clausen, Dansgaard, Gundestrup, Johnsen and ReehHammer and others, 1978).
Fig. 2. Depth as a function of age for various deep cores. Curves are meant to guide the eye. Points are a sampling of more extensive data from the references in Table 1.
Table 1. Data on ice cores and drilling sites
Figure 3 casts the data in Figure 2 as a universal function in which depth as a function of age is shown in dimensionless coordinates. The dimensionless time is defined as t* = ta(t)/H, where t is the time in years, a is the accumulation rate in meters of ice (at density 0.92 Mg m−3) per year and Η is the ice thickness (m) to bedrock. The dimensionless depth is defined as if d*=d/H. Following the practice of most authors, for times t < 15 kyear BP we took a(t)to be its average value during the Holocene, and for 15 ≤ t≤ 110 kyear BP we took a(t)to be a constant fraction of its Holocene value. For Antarctic sites, the fraction is taken to be 0.75; for Greenland sites the fraction is taken to be 0.5. Our adapted values of a(t) are given in columns 7 and 8 of Table 1. The rationale for assigning a smaller value to a(t) during the period 15-110 kyear BP is that large parts of the time-scales given in the references are based on ice-flow models for which the authors (with justification) assumed a smaller value of a(t) during that period. This approach should be most successful for sites near ice divides, for which the horizontal flow rate is small. Recently, more sophisticated models have been used, in which the accumulation rate has been taken as continuously varying in a way that can be inferred from the δ 18O record or the 10Be record less the spikes. Since such data are not available far South Pale ice, we have contented ourselves with the simpler approach using step-function values as described above. For the South Pole site, with its large horizontal flow rate, the accumulation rate for upstream from which the deep ice originated is somewhat smaller than assumed in our simple model (personal communication from E. Mosley-Thompson, 1994). To convey an idea of the uncertainty, we will present three age vs depth curves for the South Pole, one of which (Reference McInnes and RadokMcInnes and Radok, 1984) is based on unrealistically low upstream accumulation rates.
Fig. 3. Universal curve of dimensionless depth vs dimensionless age, with a(t) = step function, reduced at 15-100 kyear BP (see text).
Analytical ice-flow models of age vs depth have evolved from work by Reference NyeNye (1963), Reference WeertmanWeertman (1968) and Reference Dansgaard and JohnsenDansgaard and Johnsen (1969). On the assumption of a constant vertical strain rate with depth, Reference NyeNye (1963) found the simple dependence of depth on age
where a =constant. In the dimensionless version
More refined models take into account the variation of horizontal flow rate, vertical strain rate and temperature with depth; the dependence of ice plasticity on temperature and crystal texture; the temperature at the ice-bedrock interface; the flow paths of ice from the surface at various times in the past to its present depth, which depends on factors such as the distance of the core From an ice divide; the variation of accumulation rate upstream as a function of time and of the position from which the ice originated; the slope of the bedrock; and the slope at the surface. Little of this information is available for the South Pole site.
The universal curve in Figure 3 is for Equation (2). One sees that for values of reduced depth d * greater than about 0.5 the scatter becomes large. With the universal curve as input, the solid curve in Figure 4 shows our prediction of the age vs depth for the South Pole. The best direct measurements give quite consistent values of accumulation rate for recent times: a =0:074 m year−1 from annual dust layers extending back to AD 1590 (personal communication from E. Mosley-Thompson, 1994), a = 0.072 m year−1 based on visible stratigraphy in an inclined snow mine for the period AD 1950-1770 (Reference GiovinettoGiovinetto, 1964), and 0.0073 m year−1 based on a stake network and beta-activity measurements over much of Antarctica (Reference Young, Pourchet, Kotlyakov, Korolev and DyugerovYoung and others, 1982). The curve in Figure 4 labeled “AMANDA model” is for a(t) =0.073 m year−5 back to 15 kyear BP and 0.055 m year−1 before 15 kyear BP.
Fig. 4. Models of depth as a function of age for South Pole ice. The AMANDA models is for a = 0.073 m year−1 since 15 kyear BP and a = 0.055 m year−1 before 15 kyear BP. Lowest curve is the flowline model of Reference McInnes and RadokMcInnes and Radok (1984). Intermediate curve is based on values of a(t) from Giovinetto. Irregular curue is dust flux at Vostok after smoothing by a cubic spline function (Reference Petit, Mounier, Jouzel, Korotkevich, Kotlyakov and LoriusPetit and others, 1990). The scale for dust is linear, with the largest peak corresponding to 7.3 × 10−7 cm year−1 (which can be converted into units of g cm−2 year−1 by multiplying by density).
One attempt to predict age vs depth for ice at the South Pole has been published (Reference McInnes and RadokMcInnes and Radok, 1984). The lower curve in Figure 4 shows their model, which agrees with ours at depths down to ∼ 1300 m, corresponding to an age of ∼33 kyear BP. For greater depths they inferred a much more rapid increase in age with depth than we do, because they assumed anabrupt decrease in accumulation rate from ∼0.088 m year−1 at the South Pole to a constant value of for ice more than ∼100 km upstream, which reaches the South Pole at times greater than ∼30 kyear BP. Mosley-Thompson’s recent measurements of accumulation rate at Plateau Remote, near the Pole of Relative Inaccessibility, gave values about twice as large as assumed by Reference McInnes and RadokMcInnes and Radok (1984). Giovinetto (personal communication, 1995) has recently estimated upstream values that are about 1.6-2 times as large as those of McInnes and Radok. The middle curve in Figure 4 gives Giovinetto’s estimates, which we adopt.
The irregular curve along the abscissa gives the dust flux at the South Pole in arbitrary units as a function of time, inferred from measurements made on an ice core at Vostok Station (see later section for discussion).
Depth-Dependence of Scattering From Bubbles
A quantity of vital concern to the AMANDA project is the depth-dependence of λbub, the mean free path for scattering of the visible component of Cherenkov radiation off of air bubbles. For smooth spherical bubbles of r.m.s. radius rand number concentration n, λbub = (nπr 2)–1. For purposes of discussion, the polar ice can be divided into three depth regimes: at depths shallower than the close-off depth (typically ∼60 m), the firn is porous to air. At intermediate depths, bubbles exist at an constant number concentration and with bubble volume that decreases as hydrostatic pressure increases. At great depths, bubbles transform into a more stable phase consisting of air-hydrate crystals.
Bubbles are formed at the “close-off ” depth at which the firn changes into ice. The volume fraction of air trapped in the ice at pore close-off, Vc , is given experimentally (Reference Raynaud and LebelRaynaud and Lebel, 1979) by
Vc depends on atmospheric pressure and thus on altitude at the time of close-off, and depends weakly on temperature. For Vostok Station, Vc = 0.084cm3 g–1, whereas for Byrd Station, at an altitude nearly 2000 m lower than Vostok Station, Vc = 0.114cm3 g–1. The South Pole, with an altitude intermediate between Vostok and Byrd Stations, would have an intermediate value of Vc .
At zc the ice-equivalent depth for pore close-off, ρV c/n = 4πr 3/3, if all the gas is in bubbles(where ρ= mass density). The number concentration at pore close-off depends on temperature, dust concentration and other climatic factors, but is roughly similar for Vostok and Byrd Stations, the two cores on which detailed studies have been made of bubbles. Since the ice density is roughly constant below the firn layer and the ice temperature does not change much in the first 1000 m, the perfect gas law leads to expressions for the depth-dependence of the r.m.s. bubble radius
and of 1/λbub
The latter is shown by the solid curve in Figure 5. The figure also shows data for 1/λbub at Byrd Station, Vostok Station and the South Pole, derived from measurements by Reference Gow and WilliamsonGow and Williamson (1975) on a Byrd Station core, by Reference Barkov and LipenkovBarkov and Lipenkov (1984) on a Vostok Station core and on laser calibration data in situ by the AMANDA collaboration (Reference AskebjerAskebjer and others, 1995). The two sets of triangular symbols for the AMANDA measurements are put in to remind the reader that the scattering length inferred from the data depends on the angular distribution of scattered light: the lower triangles correspond to the assumption of isotropic scattering from bubbles with rough surfaces (which might come about, for example, if air-hydrate crystals were nucleating at various points on the surfaces) and the upper triangles correspond to the assumption of forward-peaked scattering from smooth spherical bubbles. (The true values should lie somewhere in between.) The curve in Figure 5 is normalized to the data at depths less than 700 m by choosing zc = 60 m, a typical depth for pore close-off,and adjusting the bubble concentration at that depth.
Fig. 5. Inverse scattering length as a function of depth for air bubbles. The data for Byrd Station and Vostok Station were taken from microscopic measurements of bubbles in caes. The AMANDA data for the South Pote were based on light scattering of laser pulses in situ. The solid curve shows the effect of hydrostatic pressure on bubble sizes, assuming all of the air is trapped in bubbles. The dashed curve shows the calculated dependence on depth due to conversion of bubbles into air-hydrate crystals (Reference PricePrice, 1995).
At depths from 100 m to nearly 700 m, the data for Byrd and Vostok Stations follow the hydro static-pressure curve rather well. At greater depths, the inverse scattering length decreases very rapidly with depth, due to a decrease in n brought about by a phase transition. A quantitative diffusion-growth model for the conversion of bubbles into air-hydrate crystals (Reference PricePrice, 1995) both fits the data for 1/λbub as a function of depth at Vostok and Byrd Stations and predicts the effective disappearance of bubbles at a depth of ∼1450 m in South Pole ice. The dotted curves in Figure 5 shew the results of that calculation for Vostok and Byrd Stations and the dashed curve shows the prediction for the South Pole. In the next section, we discuss further the phase transition from the two-phase system (ice + bubbles) into the two-phase system (ice + air hydrate).
Conversion of Bubbles to Air-Hydrate Crystals
Reference MillerMiller (1969) first showed that, at sufficiently high pressure, the system (air bubbles + ice) becomes unstable against the transformation into a two-phase system consisting of normal ice + crystals of the cubic clathrate ice structure in which O2 and N2 molecules occupy a fraction of the clathrate cages (experimentally, about 80%). In Figure 6, the dashed curves (Reference MillerMiller, 1969) give the dissociation pressures as a function of ice temperature for nitrogen hydrate and “air hydrate”. Within the hatched region between the two curves, both bubbles and hydrate crystals should coexist. On the same graph, we show the temperature as a function of depth for some cores for which either measurements or calculations exist. The profile at the South Pole is based on a model with Τ fixed at −50°C at the surface and at the pressure-melting temperature at bedrock. Seven months after completion of hot-water drilling, temperatures measured at 800-1000 m with thermistors imbedded during the AMANDA operation had dropped to within ∼0.3°C of the model temperatures.
Fig. 6. Temperature profiles for several sites in Greenland and Antarctica, compared with pressure-dissociation equilibria (converted to depths) for nitrogen clathrales and air (N2 + O2) hydrates. In the hatched region, both bubbles and hydrate crystals should coexist. The solid triangles indicate depths at which air-hydrate crystals are first observed to appear; the solid squares indicate depths at which air bubbles have completely disappeared. Arrows at solid squares for Dome C and Camp Centry indicate lower limits on depths for disappearance of bubbles.
With polarized light, air-hydrate crystals have been observed in a number of core sections. (Reference Shoji and LangwayShoji and Langway 1982, Reference Shoji and Langway1987) studied air-hydrate crystals in cores from Dye 3, Camp Century and Byrd Station. Reference Uchida, Hondoh, Mae, Lipenkov and DuvalUchida and others (1994a) recently made quantitative measurements of size, shape and concentration of such crystals as a function of depth in Vostok Stationcores. In Figure 6 we have indicated on the depth vs temperature curves the depths at which air-hydrate crystals first appear, as well as the depths at which air bubbles are no longer present. Reference Shoji and LangwayShoji and Langway (1987) pointed out that the depth at which air-hydrate crystals first appear agrees reasonably well with the depths corresponding to the dissociation pressures calculated for air hydrate by Reference MillerMiller (1969). To explain why air-hydrate crystals are found at depths about 100 m above the depth corressponding to the equilibrium-phase boundary at Byrd Station (see our Figure 6), Reference Craig, Shoji and LangwayCraig and others (1993) pointed out that the hydrate crystals had probably formed at a greater depth just upstream of Byrd Station and had remained metastable following vertical advection of ice through the local phase-boundary depth on the way to their present location at Byrd Station. The advection is attributed to large-scale irregularities in the topography of the bedrock. Since the bedrock topography upstream of the South Pole would not give rise to such upwelling, we predict that air hydrates will appear in increasing concentration at depths exceeding ∼500 m at the South Pole.
Reference PricePrice (1995) showed that the broad transition zone in depth for coexistence of both bubbles and air-hydrate: crystals in ice cores was not due to a nucleation barrier but rather to the slowness of diffusion of water molecules through a spherical shell of air-hydrate crystal forming on bubble walls. His model exploited the fact that, whereas the activation energy for diffusion through normal ice is only 0.57 eV, the activation energy for diffusion through air hydrate is much higher, 0.9 eV (Reference Uchida, Hondoh, Mae, Duval and LipenkovUchida and others, 1994b), which is able to account for the very slow growth rate of air-hydrate crystals.
In Table 1, column 9 gives the depths at which air bubbles in various cores are no longer seen. The same data are displayed in Figure 6. For the South Pole site, we adopt the diffusion model that predicts essentially conversion of bobbles into air-hydrate crystals at depths greater than 1450 m.
Particle-Scattering Centers as a Function of Depth
Insoluble impurities
In the absence of bubbles, insoluble dust particles with diameters ∼0.l-∼10 µm probably make the most important contribution to scattering of visible light in the ice. The concentration of dust and soluble impurities in the ice has been shown to be directly related to the of atmospheric aerosols. For insoluble the size distribution is log normal, with typical modal diameter ranging from 0.5 (in Dome C; Reference Royer, Angelis and PetitRoyer and others, 1983) to 0.6 µm (in Vostok Station; Reference De Angelis, Legrand, Petit, Barkov, Korotkevich and KotlyakovDe Angelis and others, 1984). The dust concentration in ice cores shows both an annual variation and a long-term anti-correlation with the temperature inferred from δ 18O measurements. For example, as seen in Table 2, all deep cores show an increase in dust concentration at depths corresponding to the Last Glacial Maximum (LGM) — by one order of magnitude for Antarctica and by two orders of magnitude for Greenland. The vertical dust flux increases as global temperature decreases, both because of increased continental aridity and because of higher wind velocity. (The flux is roughly proportional to the desert area of nearby continents and to the cube of wind velocity.) For a given annual dust flux, the concentration deposited in ice is inversely proportional to snow-accumulation rate and is roughly constant for the entire Antarctic continent (Reference Petit, Mounier, Jouzel, Korotkevich, Kotlyakov and LoriusPetit and others, 1990).
Table 2. Dust concentration in cores at depths for Holocene, LGM and 40 kyear BP (units are particles ml 1 with 0.65 ≤ diam. ≤ 0.82 μm)
In Figure 4, the irregular curve shows the dust flux as a function of time at Vostok Station inferred from measurements on an ice core (Reference Petit, Mounier, Jouzel, Korotkevich, Kotlyakov and LoriusPetit and others, 1990). By comparing this curve with the models of age vs depth on the same graph, we obtain estimates of the depths at the South Pole at which maxima and minima in the dust concentration occur. (To convert from flux to concentration, divide, by accumulation rate.) For example, each of the models predicts that the largest peak, corresponding to the Last Glacial Maximum, will be found at a depth of ∼1000 m. The next maximum, at ∼60 kyear BP, is predicted to occur at ∼1700 m with the Giovinetto model.
Taking together the requirements that all bubbles must have converted into air-hydrate crystals (which dictates that the detectors be deeper than 1450 m), that depths with high dust concentration be avoided and that depths of large horizontal shear (>2100 m) be avoided, the Giovinetto model leads to the following constraints:
Strings instrumented over a vertical distance of 200 m could be deployed in the depth interval ∼1400 to 1600 m between the 18 and 60 k year dust peaks, or
strings instrumented over a vertical distance of 300 m could be deployed in the depth interval ∼1800 to ∼2100 m between the 60 and 160 kyear dust peaks.
We must, however, allow for an uncertainty of at least 100-200 m in the location of the 60 kyear dust peak. When we drill the holes for the six deeper AMANDA strings, we intend to use the pulsed laser technique to measure the scattering mean free path λscat as a function of depth throughout the region of interest from 1450 to 2100 m. In order to optimize the vertical location of the phototubes on the six strings, we must determine the depth of the 60 kyear BP dust peak while drilling the first hole. As the AMANDA observatory expands beyond the set of ten strings envisaged in Figure 1, additional strings will be implanted so as to avoid the dust peak.
We next estimate the mean free path for light scattering from dust at the South Pole for the maximum and minimum values of the dust concentration. We use data collected in Table 2, which gives our estimates of the dust concentrations in various cores at depths corresponding to three times: the Holocene (from the present back to ∼13 kyear BP), for which the dust concentration has been roughly constant and quite low; the Last Glacial Maximum, at ∼18 kyear BP; and a time ∼40 kyear BP, typical of the region of minimal dust concentration. Data at the South Pole exist only for a depth of 100-349 m (personal communication from E. Mosley-Thompson, 1994). To predict the concentration at 40 kyear BP at the South Pole, we note that the ratio of the concentration at 40 kyear BP and during the Holocene is ∼1.5 for Byrd Station, 2.6 for Dome C and 2.9 for Vostok Station. We assume that the average of these three values, a factor 2.3, holds at the South Pole. Noting that the ratio of concentrations at the LGM and during the Holocene is 10, 17 and 12 for Byrd Station, Dome C and Vostok Station, respectively, we adopt a factor ∼13 for the South Pole. Our predictions appear in row 6 of Table 2.
We estimate the mean free path for light scattering from dust in two ways. The more direct approach uses the data in Table 3 on the diameter distribution of dust measured in an ice care in the depth interval 100-349 m at the South Pole. (No deeper core has yet been obtained.) Column 2 gives the numbers of particles per ml and column 3 gives the total cross-sectional area per ml assuming πr2 per particle. Summing the entries gives 7 × 104 particles with diameter >0.1 μm and total cross-sectional area ml−1 of 7 × 10−5 cm−1. (For a log-normal size distribution peaked at 0,5 μm, the area ml−1 below 0.1 μm (Reference Gayley and RamGayley and Ram, 1985) is negligible and the area ml−1 above 2 μm (personal communication from E. Mosley-Thompson, 1994) is as given in Table 3.) The reciprocal of the latter quantity is λscat, which is seen to be ∼140 m. Assuming that the relative concentrations in the different diameter intervals do not change with depth, we can scale the mean free path to different times, leading to the prediction that λscat ≈ 11 m at the Last Glacial Maximum and λscat ≈ 60 m at a depth corresponding to 40 k year BP.
Table 3. Size distribution of dust in a South Pole core at depth of 100-349 m
The second approach is based on the study of light scattering and absorption by dust suspended in a Dome C core. Reference Royer, Angelis and PetitRoyer and others (1983) used a gonionephelometer to measure the intensity of light at 546 nm scattered at angles from 15° to 150° in freshly melted ice. Using Mie theory to fit the angular distribution of scattered light, they derived average values of the scattering coefficient b = 3.46 ± 0.2 × 10–2m–1 for Holocene samples, b = 10 ± 2.5 × 10–2m–1 for LGM samples and ~5 × 10–2m–1 for samples, near the bottom of the core (corresponding to ∼30 kyear Β P). From these results, we infer a mean free path λscat = 20 m for dust near the bottom of the care at Dome C. Scaling with accumulation rate, we infer λscat = 40 m for dust at 1500 m at the South Pole. Comparison of this result with that obtained by the first approach provides an indication of the uncertainty in the value of λscat.
Soluble impurities
Studies of the paleochemistry of deep Antarctic cores have shown that the mass in soluble impurities was comparable to or even greater than the mass in insoluble impurities (Reference Royer, Angelis and PetitRoyer and others, 1983; Reference De Angelis, Legrand, Petit, Barkov, Korotkevich and KotlyakovDe Angelis and others, 1984; Reference Legrand,, Lorius, Barkov and PetrovLegrand and others, 1988). Since the soluble impurities might have remained intact until chemistry was done on melted core samples, we discuss to what extent they would contribute to light scattering in deep ice. The concentration of soluble impurities in recent ice at Vostok Station (Reference Legrand,, Lorius, Barkov and PetrovLegrand and others, 1988) is about twice as great as in recent ice taken from a 130 m South Pole core (Reference Kirchner and DelmasKirchner and Delmas, 1988). We use this factor 2 to scale concentrations of various soluble impurities from Vostok Station to the South Pole at 40 kyear BP. We group soluble impurities in two classes — those that remain liquid at a temperature ∼-45° to -50°C pertinent to South Pole ice (comprising sulfuric, nitric and hydrochloric acid) and those (mainly NaCl) that are solid at those temperatures.
The acids are transported to the South Pole mainly as hydrated sub-micron droplets. During compaction and grain growth, ice-crystal boundaries sweep up ions such as SO4 2−, leading to a concentration of acids in three-crystal boundaries called veins (Reference Wolff, Mulvaney and OatesWolff and others, 1988). As a worst-case estimate of λscat, we assume that all acid (∼100ng g−1) reaches veins. For a crystal size of ∼4mm, the same as measured in the Vostok Station core at a depth of 1500 m (Reference Lipenkov, Barkov, Duval and PimientaLipenkov and others, 1989), the vein diameter would be 2 μm, the refractive index due to the acid would be ∼1.37 (sulfuric acid, at 3.7 Ml–1) and λscat ≈ 10m. For a more optimistic estimate, assume that the acid is uniformly spread out in two-crystal boundaries. Then, the thickness of the acid layer would be only ∼0.1 nm and light would be unaffected by its presence.
The salts, sprayed into the atmosphere during sea storms, diffuse as aerosols, a small fraction reaching the South Pole. 20% of snowflakes and ice particles collected from the air by filters near South Pole Station have NaCl at their centers (Reference KumaiKumai, 1976). We estimate that the concentration of salt grains is ∼50 ng g-1 at 1500 m depth in South Pole ice, To make a worst-case estimate, we assume that no salt particles dissolve in surrounding water or ice either in the atmosphere, in snow near the surface or in deep ice. We also assume that during grain growth, crystal boundaries will pass through the salt grains, leaving them unaltered. The contribution to λscat depends on the size distribution of salt grains, which is poorly known for aerosols and unknown for deep ice. We estimate that λscat(m) ≈ 26 r r.m.s. (μm). If r r.m.s. = 0.4μm, the scattering mean free path becomes ∼10 m. We think it very unlikely, however, that salt grains will survive intact for 40 kyear. It is much more likely that sub-micron salt grains will react or dissolve as crystal boundaries pass through them. Reference Wolff, Mulvaney and OatesWolff and others (1988) estimated that ∼10% or more of the sulfuric acid could be in crystal boundaries. Then, NaCl would react at boundaries to form Na2SO4 + HCL. The solubility of Na2SO4 in water is ∼40 g 100 ml-1, so that some or all of the salt would end up dissolved in liquid films at crystal boundaries. Even partial dissolution would facilitate diffusion of Na+ and Cl- ions through the lattice. Either of the two effects would increase λscat.
Refraction by Air-Hydrate Crystals
In the last section, we concluded that in the depth interval 1600-1850 m at the South Pole all bubbles will have transformed into air-hydrate crystals and λscat will be of order 40-60 m, independent of the age vs depth model. Because the air-hydrate crystals have dimensions very large relative to the wavelength of light, Cherenkov light will undergo refraction rather than scattering at interfaces between air-hydrate and hexagonal ice crystals. The quantitative effect of the hydrate crystals on light transmission will depend on their size, shape, concentration and refractive index relative to that of the normal ice in which they are imbedded. Using X-ray diffraction, Reference Hondoh, Anzai, Goto, Mae, Higashi and LangwayHondoh and others (1990) verified the cubic clathrate nature of natural air-hydrate crystals in a Dye 3 deep core. From the Raman intensities of the stretching modes of N2 and O2, Reference Nakahara, Shigesato, Higashi, Hondoh and LangwayNakahara and others (1988) inferred a composition ratio of N2:O2 to be 1.6–1.9 in the clathrate structure of these same hydrate crystals. (Reference Shoji and LangwayShoji and Langway 1982, Reference Shoji and Langway1987) made optical studies and did laboratory experiments on air-hydrate crystals in ice cores from Dye 3, Camp Century and Byrd Station. Uchida (personal communication, 1994) determined that the ratio of the refractive index of natural air hydrate in ice-core samples relative to the refractive index of hexagonal ice is 1.004. Reference Uchida, Hondoh, Mae, Lipenkov and DuvalUchida and others (1994a) recently made an extensive study of the depth profiles of the shape, volume concentration, number concentration and mean volume per crystal of air-hydrate crystals in Vostok Station ice-core samples. They found a typical concentration of air-hydrate crystals of ∼500 cm-3, a typical diameter of 100 μm and a predominance of spherical shapes, from which we infer a typical mean path of ∼15 cm for encounter of a light ray with such crystals. To reach a phototube at a distance of, say, 25 m requires ∼170 traversals of such crystals. Integrating over impact parameters gives an r.m.s. refraction angle δrms = 1° for one encouter. Although the distribution of single refractions is strongly non-Gaussian, after ∼170 refractions the distribution is very closely Gaussian, with σ δ = δrms(L/λrefr)1/2 ≈ 13°. The distribution of transverse displacements is also nearly Gaussian, with σ d = δrms(L/λrefr)3/2λrefr e –1/2 ≈ 3.3 m.
We calculated the timing dispersion due to photons that are emitted from all points along a muon’s trajectory and that refract into a pholomultiplied tube. Absorption prevents the integral from diverging. The distribution of arrival times has a sharp peak due to photons emitted from the part of the muon track near the Cherenkov angle and a weak but very broad component due to photons coming from the muon track far upstream. For a muon passing close to one of the PMTs, we find that the angular error is ∆α ≈ (tan θ C)/(tan2 θ C + 1) ∆tn/cL 0, where L 0 is the distance along the Cherenkov angle to the muon track. For λabs = 300 m, which is the case for light at a wavelength of ∼400 nm, we find that even for a long distance like L 0= 50 m, the fraction of photons refracted more than 1° is only ∼6%, and the associated tine delay is 8 ns. The conclusion is that air-hydrate crystals cause far less serious problems for AMANDA than does scattering by dust. From the Fresnel equations for reflection, we conclude that the fractional reduction in intensity of transmitted light after 102 encounters is only ∼103. Thus, because of the nearly perfect match of refractive index to that of hexagonal ice, air-hydrate crystals have virtually no effect on the imaging of muon trajectories.
Refraction at Ice-Crystal Boundaries
With its hexagonal crystal structure, ice has a refractive index along the c axis that is larger than that in the basal plane by a factor of 1.001. Again, assuming a mean crystal size of 4 mm, a light ray in South Pole ice would refract ∼6000 times in traversing a distance af 25 m. As a simple estimate, we assume a random distribution of c axes with a typical angle of 45° between caxes in adjacent crystals. We estimate an r.m.s. deflection angle σδ = 0.1°, a net deflection of 12°, a transverse displacement σδ ≈ 5 m and a fractional loss of intensity of transmitted light ∼ few 10−3. In a more detailed analysis, to be published elsewhere, we conclude that large-angle scattering from dust causes greater degradation of trajectory information than does a series of small-angle refractions at ice-crystal boundaries and air-hydrate crystal boundaries.
Conclusions
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1. The AMANDA age vs depth model in Figure 4 probably underestimates ages at great depths because the choice of a(t) =0.055 m year−1 during the interval 15–110 kyear BP is higher than recent values estimated by Mosley-Thompson (personal communication, 1994) and Giovinetto (personal communication, 1995). The flowline model of McInnes-Radok overestimates the ages at depths greater than ∼1300 m because of the very small (and incorrect) value a(t) =0.0.2 m year−1 at distances more than ∼180 km upstream. We adopt a model based on estimates of a(t) by Giovinetto and shown in Figure 4.
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2. A diffusion-growth model that fits Vostok and Byrd Stations core data predicts that the transformation of bubbles into air-hydrate crystals at the South Pole will be complete at depths below ∼1450 m.
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3. Using data on the size distribution of dust in a shallow South Pole core (100–349 m), together with systematics of depth profiles of dust concentrations at other sites, we estimate a mean free path of ∼40–∼60 m for scattering of Light from dust in the depth intervals 1400–1600 m and 1800–2100 m at which AMANDA detectors might be deployed. At a depth of ∼1700 m corresponding to the peak in the dust concentration at ∼60 kyear BP, the scattering mean free path is estimated to drop to ∼13–20 m. Such a short mean free path is confined to a vertical layer a few tens of meters thick.
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4. The main water-soluble impurities are liquid acids and salt grains. For an acid concentration of 100 ng g−1 the fraction of the acid (f ≈ 0.4–0.9) that segregates to µm sized veins at three-crystal boundaries is estimated to scatter light with λscat ≈ 10 m f –1, the exact value depending on crystal size and shape. The ∼50 ng g−1 of salt grains will interact with moving crystal boundaries, where they will at least partially dissolve in concentrated acid films in the boundaries. The contribution to λscat will depend on the r.m.s. radius (in µm) of surviving grains and on the fraction of survivors as λscat(m) ≈ 26r r.m.s./f. To determine more quantitatively the contributions of soluble impurities to scattering must await measurements to be made with the six future strings.
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5. Taking into account the age vs depth relationship, the depth profile of the dust concentration for the deep Station core, the expected depth for bubble disappearance (1450 m) and the depth (∼2500 m) at which the horizontal ice-flow rate is thought to change rapidly with depth (personal communication from B, Koci, 1994), we conclude that
the safest depth interval in which to deploy AMANDA phototubes is between 1800 and 2100 m. If drilling capabilities limit us to shallower depths, the interval 1400–1600 m is our second choice. The pulsed-laser technique can be used to locate the 60 kyear BP peak in dust concentration and to optimize the choice of depth interval for a second-generation version of AMANDA.
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6. Due to the small difference in refractive index between air-hydrate and normal hexagonal ice crystals, refraction at the interfaces between the two types of crystal will have a small effect on the trajectories of Cherenkov light rays emitted by muons in the ice and loss of light due to at the boundaries will be negligibly small.
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7. Similar reasoning leads to the conclusion that, due to the small difference in refractive index parallel to and perpendicular to the c axis in normal hexagonal ice, refraction at the interfaces between randomly distributed ice crystals will have a small effect on the trajectories of Cherenkov light rays emitted by muons and loss of light due to reflections at the boundaries will be negligibly small.
Acknowledgements
We are indebted to B, Koci and the entire PICO organization for their excellent support with the ice drilling. This work was supported in part by the U.S. National Science Foundation, the K. A. Wallenberg Foundation, the Swedish Natural Science Research Council, the G. Gustafsson Foundation, Swedish Polar Research and the Graduate School of the University of Wisconsin, Madison. We thank R. B. Alley, S. P. Davis, P. Duval, J. Fitzpatrick, A.J. Gow, T. Hondoh, B. Koci, V.Ya. Lipenkov, S. L. Miller, E. Mosley-Thompson, R. G. Pain, J. M. Palais, J. R. Petit, M. Ram, C.F. Raymond and T. Uchida for helpful discussion.
Appendix The Amanda Collaboration
Members of the AMANDA Collaboration arD: P. Askebjer (Physics Department, Stockholm University, Stockholm S-106 91, Sweden), S. Barwick (Physics Department, University of California, Irvine, California 92717, U.S.A.), L. Bergström and A. Bouchta (Physics Department, Stockholm University, Stockholm S-106 91, Sweden), S. Carius (Physics Department, Uppsala University, Uppsala S-752 20, Sweden), A. Coulthard and K. Engel (Physics Department, University of Wisconsin-Madison. Madison, Wisconsin 53706, U.S.A.), B. Erlandsson and A. Goobar (Physics Department, Stockholm University, Stockholm S-106 91, Sweden), L. Gray (Physics Department, University of Wisconsin-Madison, Madison, Wisconsin 53706, U.S.A.), A. Hallgren (Physics Department, Uppsala University, Uppsala S-752 20, Sweden), F. Halzen (Physics Department, University of Wisconsin, Madison, Madison, Wisconsin 53706, U.S.A.), P.O.Hulth (Physics Department, Stockholm University, Stockholm S-106 91, Sweden), J. Jacobsen (Physics Department, University of Wisconsin-Madison, Madison, Wisconsin 53706, U.S.A.), S, Johansson (Physics Department, Stockholm University, Stockholm S-106 91, Sweden; currently at Physics Department, Jönköping University, Jönköping, Sweden), V. Kandhadai and I. Liubarsky (Physics Department, University of Wisconsin-Madison, Madi¬son, Wisconsin 53706, U.S.A.), D. Lowder and T. Miller (Physics Department, University of California, Berkeley, California 94720-7300, U.S.A.; currently at Bartol Research Institute, Newark, Delaware 19716, U.S.A.), P. Mock (Physics Department, University of California, Irvine, California 92717, U.S.A.), R. Morse (Physics Department, University of Wisconsin-Madison, Madison, Wisconsin 53706, U.S.A.), R. Porrata (Physics Department, University of California, Irvine, California 92717, U.S.A.), P.B. Price and A. Richards (Physics Department, University of California, Berkeley, California 94720-7300, U.S.A)H. Rubenstein (Physics Department, Uppsala University, Uppsala S-752 20, Sweden), J. C. Spang (Physics Department, University of Wisconsin-Madison, Madison, Wisconsin 53706, U.S.A.), Q. Sun (Physics Department, Stockholm University, Stockholm S-106 91, Sweden), S. Tilav (Physics Department, University of Wisconsin-Madison, Madison, Wisconsin 53706, U.S.A.), C. Walek (Physics Department, Stockholm University, Stockholm S-106 91, Sweden) and G. Yodh (Physics Department, University of California, Irvine, California 92717, U.S.A.)
