Engineering topics

Lien, David J.

Publications and source records attributed to Lien, David J..

8 records

NASA NTRS1998

"CHON" particles: The interstellar component of cometary dust

Interstellar dust is characterized by strong absorption in the ultraviolet and the mid-IR. Current models of interstellar dust are based on three chemically distinct components: a form of carbon (usually graphite), a silicate, and a blend of polycyclic aromatic hydrocarbons or other carbonaceous material. Previous work using effective medium theories to understand the optical properties of cometary dust suggested that an amalgam of materials could reproduce the observed interstellar and cometary dust features. Recently, Lawler and Brownlee (1992) re-analyzed the PIA and PUMA-1 data sets from the Giotto flyby of P/Halley and discovered that the so-called "CHON" particles were actually composed of a blend of carbon-bearing and silicon-bearing materials. Based on effective medium theories, the absorption spectrum of such a material would display the spectral features of each of the components - strong UV absorption from the carbonaceous component and strong absorption in the IR from the silicate component. To test this idea, vapor-deposited samples were created using two different deposition techniques: sputtering with an argon RF magnetron and deposition from an argon plasma torch. Two different compositions were tested: a blend of graphite and silica in a 7:1 ratio and an amalgam of materials whose approximate composition matches the "CHON"-silicate abundances for the uncompressed PIA data set of Lawler and Brownlee: graphite, iron oxide, magnesium oxide, ammonium sulfate, calcium carbonate, and silica in mass ratios of 6:4.3:4:2.2:1:9. The samples were finely ground and pressed into 2" diameter disks using a 40 ton press. In all, four different experiments were performed: one with each of the compositions (C:SiO and "CHON") in both the RF magnetron and the plasma torch chambers. The RF magnetron created a uniform dark thin film on the substrate surface, and the plasma torch created a coating of small (<100 micron) diameter grey particles. The spectra of all four samples show a strong, broad absorption feature at around 220 nm as well as a strong but narrower absorption peak near 10 microns. The RF magnetron sputtered samples showed some sub-structure in the UV, and the peak of the absorption was shifted toward longer wavelengths. The UV absorption in the plasma torch deposited samples have no sub-structure, and the peak absorption is very near 220 nm. Strong absorption near 9 microns is seen in the spectra from both sample preparation techniques, and is consistent with the IR spectra of some terrestrial silicates. Other features, particularly at 6.2 and 8.6 microns, are seen in the interstellar medium. A strong feature near 2 microns is due to absorbed water in the sample. Based on the results of these experiments, there is evidence that a material with a composition similar to that detected in "CHON" particles in the coma of P/Halley have a spectral signature which reproduces the main absorption features of interstellar dust. This suggests that the "CHON" particles could be the interstellar component of cometary dust.

Lien, David J.↗

NASA NTRS1992

Numerical simulations of cometary dust

Most observations of comets are done photometrically or spectrophotometrically. The interpretation of the aperture-averaged flux is relatively simple for an isotropic, radially expanding coma of infinite extent - the canonical model. However, the interpretation of the observations is not so clear when the motion of the dust is affected by radiation pressure, or when the emission is time-varying and anisotropic. For example, in a sample of CCD images of 10 comets, Jewitt and Meech (1987, Ap.J. 317, 992) found that the photometric profiles of only three comets were consistent, within the observational errors, with the profiles predicted form the canonical model. Photometric observations with large apertures, however, seem to suggest that the canonical model may be quite adequate (c.f. Osip, Schleicher, and Millis, 1992, Icarus 98, 115). The dust itself is characterized by a size distribution, with size dependencies on the expansion velocity, the scattered and thermal radiation, the response to radiation pressure, and probably the density. How good then are the approximations normally used in determining the production rates of the dust when these effects are present? As part of a program to better understand the dynamics of cometary dust and gas, a computer program has been developed which numerically simulates the emission of both dust and gas from a tilted rotating nucleus.

Lien, David J.↗

NASA NTRS1991

Optical properties of cometary dust

The application of measured optical constants to the interaction of electromagnetic radiation with small cometary dust particles is discussed, with emphasis on the interpretation of cometary observations. It is found that in some spectral regions optical constants vary greatly with wavelength. The optical constants may be incorrect. Because of errors in measurement, or the application of the Kramers-Kronig relationship over too small a spectral region, or an improperly prepared sample, the derived optical constants may be in error. It is suggested that a full Kramers-Kronig analysis and application of the more important sum rules should be performed on any set of optical constants whose accuracy is important. Optical constants derived from the measurement of inhomogeneous materials, where the inhomogeneities are of comparable size to that of the beam of radiation used in the experiment, should not be used to predict the optical properties of small particles.

Lien, David J.↗

NASA NTRS1990

Ground-based thermal IR images of Comet Tempel 2

The 10.8-micron images of Comet Tempel 2 obtained on the four days from September 21 to 24, 1988, indicate that the dust coma contributed about half of the nuclear pixel brightness. The nuclear condensation brightness exhibited a temporal variability slightly larger than observational uncertainty. The structure of the observed extended dust emission is interpretable as (1) a large grain tail primarily generated by cm-scaled particles, (2) the result of an outburst near 2.5-3.0 AU perihelion, and (3) a sunward emission of dust in a fanlike pattern.

Campins, Humberto↗

NASA NTRS1990

The Tempel 2 dust trail

The IAS satellite's extensive observations of Comet Tempel 2 dust trail suggest that it is composed of particles of greater-than-1 mm diameter, whose velocities relative to the comet (assuming isotropic emission) are in the range of several m/sec. Excess color temperatures obtained relative to a blackbody indicate that either (1) the particles are large enough to support a temperature gradient over their surfaces, or (2) a small-particle population exists whose diameters are smaller than 100 A. If these small particles had not originated from the large particles, their acceleration to km/sec velocities by the gas outflow would have prevented their ejection into trail orbits.

Sykes, Mark V.↗

NASA NTRS1990

Comparison of P/Brorsen-Metcalf and P/Halley in the thermal infrared

Of the periodic comets, only comets Halley and Brorsen-Metcalf have periods of the order of 75 years and are bright enough to study spectroscopically in the infrared. Thermal IR spectroscopy of comet P/Brorsen-Metcalf near perihelion are presented and the results are compared to comet P/Halley.

Lynch, David K.↗

NASA NTRS1989

Infrared imaging of the coma of Comet Wilson

The brightness of the nuclear condensation noted in March 13-15, 1987 thermal IR images of Comet Wilson did not vary, in contrast to Comet Halley's behavior; a dynamical analysis of the dust coma/tail structure establishes that the particle size distribution in this comet, while different from that of Comet Giacobini-Zinner, is nevertheless more similar to that in Comet Halley. The nonisotropic character of the dust ejection is taken to be evidence for prograde rotation of the nucleus, and it is speculated that Comet Wilson is too young to have developed a dust mantle; this would account for the lack of short time scale variability.

Campins, Humberto↗

NASA NTRS1988

Thermal properties of heterogeneous grains

Cometary dust is not spherical nor homogeneous, yet these are the assumptions used to model its thermal, optical, and dynamical properties. To better understand the effects of heterogeneity on the thermal and optical properties of dust grains, the effective dielectric constant for an admixture of magnetite and a silicate were calculated using two different effective medium theories: the Maxwell-Garnett theory and the Bruggeman theory. In concept, the MG theory describes the effective dielectric constant of a matrix material into which is embedded a large number of very small inclusions of a second material. The Bruggeman theory describes the dielectric constant of a well mixed aggregate of two or more types of materials. Both theories assume that the individual particles are much smaller than the wavelength of the incident radiation. The refractivity for a heterogeneous grain using the MG theory is very similar to the refractivity of the matrix material, even for large volume fractions of the inclusion. The equilibrium grain temperature for spherical particles sized from .001 to 100 microns in radius at 1 astronomical unit from the sun was calculated. Further explanation is given.

Lien, David J.↗