From P/Halley long slit spectroscopic exposures on 12 dates, extending from Oct. 1985 to May 1986, spatial profiles were obtained for emissions by C2, CN, NH2, and OI(1D). Haser model scale lengths were fitted to these data. The extended time coverage allowed the checking for consistency between the various dates. The time varying production rate of P/Halley severely affected the profiles after perihelion, which is shown in two profile sequences on adjacent dates. Because of the time varying production rate, it was not possible to obtain reliable Haser model scale lengths after perihelion. The pre-perihelion analysis yielded Haser model scale lengths of sufficient consistency that they can be used for production rate determinations, whenever it is necessary to extrapolate from observed column densities within finite observing apertures. Results of scale lengths reduced to 1 AU are given and discussed

Combi, Michael

Disanti, Michael A.

Fink, Uwe

English

NASA Technical Reports Server

66 A C.r"l
N91 "25 992 //
P/Halley: Spatial distribution and scale lengths for C_ CN, NH 2, and H20
Uwe Fink 1, Michael Combi 2 and Michael A. DiSantP
Lunar and Planetary Laboratory, University of Arizona
Abstract
From P/Halley long slit spectroscopic exposures on 12 dates, extending form 1985 Oct. to 1986 May,
spatial prot'des were obtained for emissions by C 2, CN, NH2, and Ol (1D). Haser model scale lengths were fitted
to these data. The extended time coverage allowed us to check for consistency between the various dates. Not
unexpectedly, the time varying production rate of P/Halley severely affected the pro[des after perihelion, which
is nicely demonstrated in two profile sequences on adjacent dates, March 01/02 and April 14/15. Because of
the time varying production rate, it was not possible to obtain reliable Haser model scale lengths after perihelion.
Our pre-perihelion analysis yielded Haser model scale lengths of sufficient consistency that they can be used for
production rate determinations, whenever it is necessary to extrapolate from observed column densities within
finite observing aperatures. Results of scale lengths reduced to 1 AU are as follows:
parent (10 3 kin) daughter (10 3 kin)
C 2 58_+20 58_+20
CN 28-+ 15 320 + 200/-100
NH 2 4.9- + 1.5 62-+20
H20 74-+60
For C 2 a slight flattening of the profile close to the nucleus could not be fitted with a two step Haser
model but can be accommodated with a CHON halo model (Combi and Fink 1991). If the inner region is
excluded from the fit, the daughter/parent scale length ratio changes from near one to about 6. However, when
production rates are sought using a two step Haser algorithm only an equal scale length model comes close to
providing an acceptable fit. Only three observations yielded a CN daughter scale lengths because our profiles
did not extend sufficiently far. The long daughter of CN also makes this emission very sensitive to production
rate variations causing greater scatter in the parent values. A curios asymmetry of the scale lengths for NH 2 was
found with the post-perihelion parent being about twice the pre-perihelion value, but the daughter being about
half the pre-perihelion number. We have as yet not found a ready explanation for this behavior. Most of the
OI 1D profiles, which effectively map out the comet's H20 distribution, deviated very little from a I/r fall off so
that it was not possible to obtain a reliable H20 parent scale length, although consistency with the nominal
lifetime of 80xl_ seconds is quite clearly demonstrated.
This research was supported by NASA grant NAGW 1549.
1 Uwe Fink: Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721
2 Michael R. Combi: Space Research Building, University of Michigan, Ann Arbor, MI 48109-2143
3 Michael A. DiSanti: Infrared & Radio Astronomy Branch, NASA-Goddard, Code 693, Greenbelt, MD 20771
https://ntrs.nasa.gov/search.jsp?R=19910016678 2020-03-19T16:51:26+00:00Z
ACM '91 67
LOW-RESOLUTION SPECTROSCOPY OF D-TYPE ASTEROIDS
A. Fitzsimmons, Queen's University Belfast
P. Magnusson and I.P. Williams, Queen Mary and Westfield College, London
M. Dahlgren and C.-I. Lagerkvist, Uppsala Observatory
We have obtained reflectance spectra of 19 D-type asteroids using the
4.2 m William Herschel Telescope on La Plama. The wavelength coverage of
370 nm to 950 nm has allowed us to measure accurate reflectance slopes for
all of these low-albedo objects. A simultaneous search for absorption and
emission features has been performed. An initial result is that we have
been unable to confirm the existance of absorption bands in 279 Thule as
reported by us previously. Preliminary results will be presented and
discussed.
68 ACN _91
LARGE MICROMETEORITES: ATMOSPHERIC ENTRY SURVIVAL, RELATION
TO MAIN-BELT ASTEROIDS, AND IMPLICATIONS FOR THE COMETARY DUST
FLUX. G. J. Flynn, SUNY-Plattsburgh, Plattsburgh, NY 12901.
Micrometeors and micrometeorites 50 pm to 1 mm in diameter
constitute 80% of all the meteoritic mass (excluding rare, large
impactors > 1014 grams) accreting onto the Earth [Hughes 1978].
Although small micrometeorites (_< 50 _m in diameter) have been
collected from the Earth's stratosphere since the early-1970's,
micrometeorites larger than 100 _m were expected to vaporize on
atmospheric entry. Large micrometeorites (>100 _m), partially
melted and unmelted, have recently been recovered from the sea
floor [Brownlee 1981] and polar ices [Maurette et al. 1986].
IDENTIFICATION AS MICROMETEORITES: High Ne concentrations in
several large micrometeorites confirm their extraterrestrial
origin, and establish they were individually irradiated by the
solar wind as small objects, thus they are not ablation debris or
interior parts of a much laruer body [Olinger et al. 1989].
Cosmogenic nuclei, lOBe and 26A1, in large micrometeorites also
indicate small body or surface exposure [Nishiizumi et al. 1991].
ENTRY HEATING SOURCE IMPLICATIONS: Computer simulations of the
atmospheric entry of large micrometeorites show only those with
very low geocentric velocities survive without vaporization,
indicating the large micrometeorites arrive at Earth by Poynting-
Robertson (P-R) orbital evolution from main-belt asteroids [Flynn
1990, 1991; Love and Brownlee 1991] or comets in low inclination,
near-circular orbits, like Schwassman-Wachmann 1 [Flynn 1989].
RELATIONSHIPS TO METEORITES AND ASTEROIDS: The most common large
micrometeorites are partially melted spheres consisting of olivine
grains with minor amounts of magnetite. They have "chondritic" (or
solar) abundances of Mg, AI, Si, Mn, and Fe [Maurette et al.
1986]. Sutton et al. [1988] suggest the elemental abundance
patterns observed in 3 of 9 melted spheres are more consistent
with ordinary chondrite than carbonaceous chondrite composition.
Thus S and C type asteroids seem the most likely parent bodies.
But high carbon abundances, >10% in 1/3rd of particles examined
[Maurette et al. 1987], leave open P or D asteroid parent bodies.
IMPLICATIONS FOR FLUX OF COMETARY DUST: The contribution of main-
belt asteroids to the flux of large micrometeorites at Earth has
previously been assumed to be small [eg, Flynn 1989] because the
calc9lated gatastrophic collision lifetimes of these particles
(~10 _ to 10 D years) were substantially shorter than the times
required for P-R orbital evolution from the main-belt to Earth
(-10 ° yearsl[eg , Dohanyi 1978]. The space exposure ages of large
micrometeor_tes (105 to 107 years) measured by Nishiizumi et al.
[1991] are consistent with the calculated P-R lifetimes,
suggesting the true collisional lifetimes are much longer than
those calculated by Dohanyi [Flynn 1990; Nishiizumi et al. 1991].
Since the collisional lifetimes are calculated to be dominated by
smaller cometary particles, suggesting the cometary contribution
to the interplanetary dust cloud in the 1 _m to 20 _m diameter
range (responsible for the fragmentation of the larger particles)
is significantly less than previously assumed, consistent with the
conclusion that much of the 10 to 20 _m cosmic dust collected at
earth is asteroidal [Flynn 1989; Sandford and Bradley 199_
REFERENCES: Brownlee, D. E. (1981) in _he Sea, vol. Wiley, 733-762. Dohanyi, J.S. (1978) Dust (ed.
J.A.M. McDonnell) Wiley, 527-605. Flynn, G.J. (198g) 7caru,, 77, 287-310. Fllmn , G. J. (1990) M_t_nr_tln,, 25,
365. Flynn, G. J. (1991) Lunar • P1an,_, Sol. _YTT, 393-394. Hughes, D.W. {1978) in _ (ed. J.A.M.
McDonnell), Wilay, 123-185. Love, S.G. and Bruwnlee, D.E. (1991) Icar_, 8g, 25-43. Maurette, M. et al. (1986)
Sclsncs, 2_1, 869-872. Maurett_, M. et al. (1987) Natura, 328, 599-702. Rishlizuml, K. et al. (1991) Exposure
History of Individual Cosmic Particles, Earth _ _ Left. (in press). Ollnger et al. (1989) _,
24, 312. Sand(oral, S. and Bradley, J.f1990} Inarns, 82, 146-165. Sutton, 8.R. otal. (1988) M_te_rltlc,, 23, 304.
:\CH ' 9 1 69
Bulk abundances of the main rock-forming element in the P/Halley dust component
Fomenkova M.N., Evlanov E.N., Mukhin L.M., Prilutsky O.F. (Space Research
Insitute, Profsoyuznaya 84/32, Moscow 117810, USSR)
The main data on the chemical composition of P/Halley dust component
were obtained after Vega missions from PUMA-l,2 dust-impact mass-spectro-
meters. Ion ratios of a "compound bulk comet" obtained by different authors
(1-3) as the average of the individual grins spectra differ greatly from elemental
abundances in carbonaceous chondrites of type CI even for the main rock-forming
elements.However, taking into account mass of dust particles brings about a quite
satisfactory coincidence of the average ionic composition of comet dust with the solar
abundances of these elements.
The procedure of averaging was as follows. First, the sum of all the ions of
the main elements in an individual spectrum was assumed to be 100% and the
percentage of every element in this spectrum was calculated. The next step was
to average the obtained values in all spectra with weighting factors equalling the
independently derived mass of dust particles (4). This procedure enables to eliminate
u ncertainities due to the variations of the ion signal in the spectra of particles of similar mass.
To determine abundances of minor elements as AI, K, Ca, Ti, Cr, Ni we
used selected spectra of higher quality, where these elements are surely
identified. It is necessary, because noise pulses caused by impacts of very small dust grains
can be confused with peaks of minor elements. Results are given in
the table for both instruments and for different modes of functioning. Errors have been
estimated assuming that individual error of every peak is a square root of its amplitude.
PUMA1, wide PUMA1, narrow PUMA2, wide PUMA2, narrow
Na 40.8 + 17.2 29.3 _+ 1.7 69.7 + 5,7 48.2 ± 3.7
Mg 107.7 +39.6 168.4 + 5.9 138.7 + 8.6 177.0 ± 10.8
AI 18.9 + 6.3 9.0 + 0.8 23.6 ± 1.6 23.3 ± 1.6
Si 100 100 100 100
S 67.3 + 23.5 50.3_+ 2.5 74.7 _+ 5.3 85.6 ± 5.9
Cl 34.9 + 10.2 22.1 ± 1.2 3.6 + 0.2 0.2 ± 0.01
K 0.4 ± 0.2 1.2 + 0.3 2..6 ± 0.3 2..3 ± 0.2
Ca 7.4± 3.0 5.3± 0.6 11.6+ 1.2 12.5± 1.1
Ti 0.3 _+0.15 0.9 + 0.2 1.1 ± 0.1 0.9 ± 0.1
Or 1.3 ± 0.6 1.7 ± 0.4 3.0 + 0.2 3.8 ± 0.3
Fe 92.7 ± 33.4 54.7 + 3.0 70.9 ± 5.1 49.9 + 3.2
Ni 4.8 ± 1.5 2..5 + 0.4 0.6 + 0.1 < 0.1
REFERENCES
1. Sagdeev, R.Z. et al. Space Research 25, 840-848 (1987).
2. I_angevin, Y. et al. Astron. Astrophys. 187, 761-766 (1987).
3. Jessberger, E.K. et al. Nature 332, 691-695 (1988).
4. Fomenkova M.N. et al. Lunar Planet Sci. Conf. 22, 397-398 (1991).
70 ACM '91
Synthetic mapping for long range integration of
Hamiltonian system
Cl. Froeschl_ and J.M. Petit
Different types of interpolation are proposed and tested for transforming a non linear
differential system, and more particulary Hamitonians one with 2 and three degrees of
freedom into maps without having to integrate the whole orbit as in the well known
Poincar6 return map technique. We construct piecewise polynomial maps by coarse-
graining the phase surface of section into parallelograms using values of the Poincar6
maps at the vertices to define a polynomial approximation within each cell. The numeri-
cal experiments are in good agreement with both the real symplectic and Poincar6 maps.
The agreement is better when the number of vertices and the order of the polynomial
fit increase.
The effect of secular resonances in the asteroid
region between 2.1 and 2.4 AU
Ch. Froeschl6, H.Scholl
Observatoire de la CSte d'Azur, Nice, France
The asteroid region between 2.1 and 2.4 AU at inclinations between 10 ° and
20 ° is anormally depopulated. This region is surrounded by the principal secular
resonances Us, u6 and u16 and it is crossed by higher order secular resonances. Our
aim is to investigate the effect of secular resonances on the orbital evolutions of
asteroids in this region. We integrate in the frame of the four-body problem Sun-
Jupiter-Saturn-asteroid the orbits of twenty fictitious asteroids with the same initial
eccentricity of e = 0.14, initial semimajor axes in the range 2.1 <_ a <_ 2.4AU, and
initial inclinations between 12 ° < i < 20 °.


The P/Halley: Spatial distribution and scale lengths for C2, CN, NH2, and H2O

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