Engineering topics
Publications and source records attributed to Hoban, Susan.
Reuter's (1992) model of the IR fluorescence of methanol is used to retrieve a methanol production rate of 3 +/- 1 x 10 exp 26/s and an abundance relative to water of about 0.1 percent. It is argued that calibration is of paramount importance and that a near-simultaneous spectrum is necessary for achieving a reliable estimate of the continuum underlying the emission feature.
Models which assume either a parent or a distributed source for H2CO are presently used to retrieve 3-sigma upper limits to that species' production rate from a 3.55-3.64 micron search for cometary IR emission from the nu1 and nu5 bands of formaldehyde. A parent-source H2CO production rate relative to water of 0.15-0.80 percent is obtained, together with a distributed source production rate of 1.7-5.8 percent.
The IRTF's ProtoCAM has been used to observe the organic emission feature peaking near 3.36 microns in Comet Levy. 2D images of the spatial distribution of the 3.4-micron organic emission exhibit brightness profiles statistically indistinguishable from that of the dust continuum, within 1225 of the cometary nucleus; this suggests a progenitor for the emission feature which is not a photodissociation fragment of some other species.
Continuum emission has been detected during 3.44-3.64 micron spectral region observations of Comets P/Brorsen-Metcalf, Okazaki-Levy-Rudenko, and Levy. The spatial brightness profile of the 3.52-micron emission feature was measured and found to be consistent with uniform outflow from a central, unresolved source; the molecule generating the emission is either directly sublimated from the cometary surface or is a short-lived parent specie's dissociation product. The modeled IR spectrum of CH3OH implies the consistency of the observed spectra with a methanol origin for the 3.52 emission.
Near-infrared spectroscopic observations of the active star-forming region near NGC 7538 IRS 1 and IRS 2 were made. The relative intensities of the v = 1-0 Q(1), Q(3), and Q(5) lines of molecular hydrogen are used to calculate a rotational excitation temperature. Comparison of the measured intensity of the Q(2) transition relative to the intensity of Q(1) and Q(3) permitted the retrieval of the ratio of ortho-to-para hydrogen. It is found that an ortho-to-para ratio of between 1.6 and 2.35 is needed to explain the Q-branch line intensity ratios, depending on the excitation model used. This range in ortho-to-para ratios implies a range of molecular hydrogen formation temperature of approximately 105 K to 140 K.
A balanced view of the present generation of infrared instruments for cometary compositional studies is presented. Ground-based instruments are compared with airborne and spaceborne capabilities. An attempt to give examples of the unique science achievable with each is made, and particular emphasis is on the unique aspects of a dedicated Cometary Composition Telescope in earth orbit for investigating the chemical and structural heterogeneity of the cometary nucleus.
Significant spatial variations are noted in the color of the dust in Comet Halley's dust coma, out to 156,000 km from the optocenter, in the present March 1-6, 1986 narrowband CCD images. In particular, the envelope of intermediate-mass particles formed around the nucleus by solar radiation pressure is redder than the rest of the dust coma, and a strong jet noted in the March 1 images is redder than both the dust envelope and the remainder of the dust coma. A wavelength-dependence model of the Comet Halley dust's color is developed on the basis of Mie theory.
The presently reported VLA search for icy-grain 2-cm continuum emission in the halo surrounding Comet Halley in mid-November, 1985, notes the 3-sigma upper limit for flux density at this wavelength to be consistent with the detections at 1.3 and 3.5 mm by Altenhoff et al. (1986) only in the case where the sources of the emission are inefficiently radiating particles. These particles are surmised to be either icy or small refractory grains; in either case, they would be sub-mm-sized and slightly dirty.
Emission-band and continuum data were obtained of Comet Halley with a CCD camera system at the Perth Observatory during the post-perihelion phase. The image processing techniques which were applied and which revealed jets in the CN band are described. The jets had a spiral shape due to nucleus rotation at a rate which was not precisely determined. Estimates are made of the FWHM and half-width half-maximum spatial extent of the jets. Possible parent molecules of the CN jets are discussed.
Properties of the gas jets in P/Halley reported to exist in images taken in the light of CN are described. The jets also exist in the light of other radicals, specifically C2. The jets do not exist in the continuum images although it appears that one of the jets seen may come from the same area on the nucleus that produces much of the dust. The jets are seen to persist, although with varying geometry, for 2 months or more, from the time of the spacecraft encounters in March to the beginning of May. The strength of the jets is well correlated with fluctuations in the overall production rate of radicals by the comet.
Comet Halley CCD images taken in the light of CO(+) and H2O(+) were analyzed. Most of the ionic emission originates in a diffuse component on which the ion ray structure appears to be superimposed. On average, the peak enhancement in the CO(+) rays is 20% over the adjacent minima, where the emission is due to the underlying component. The H2O(+):CO(+) ratio varies by as much as 30% from ray to ray.