The light produced by the atoms and ions of Jupiter's luminous, heavy particle environment was studied. High resolution spectrophotometry is discussed

Brown, R. A.

English

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Produced by the NASA Center for Aerospace Information (CASI) 
https://ntrs.nasa.gov/search.jsp?R=19830010357 2020-03-21T05:39:46+00:00Z
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RM Grant moo MM-7634
Final Nq?ort
s
Period of Grant: 1979 October 1 - 1983 September 30
1
Submitted to: Dr. William Brunk	
4"
Discipline Scientist	 FE+i In".	 ;a
Code EL-4 (—: RECEIYEO
NASA Headquarters SSA F600 Independence Avenue, SW	 M ^
Washington, DC 20546
s
Principal Investigator: Dr. Robert A. B^o►.n*
Lunar & Planetary Lab.
University of Arizona
Tucson, AZ 85721
Submission Date: 1983 February 15
*Current address:
Space Telescope Science Inst.
Homewood Campus
Baltimore, MD	 21218
}
I. Introduction
This grant has supported research into Jupiter ' s luminous, heavy-particle
environment. The strategy has been to collect and analyse the light produced
by these atoms and ions, and to construct models using basic principles of
atonic, plasma and planetary physics. Our particu^ar coals have been: (1)
improved characterization of this region ' s physical state and composition as a
basis for interpreting Galileo in situ findings; (2) identification of the
governing physical processes which sustain this unique geophysical phenomenon;
and (3) improved fundamental capability in emission line liagnoetic sensi:-lg of
other planetary or astrophysical plasmas, with particular attention to
cemetary problems.
our program has stressed high resolution spectrophotometry with special
capabilities: ( 1) Doppler shifts measuring thermal and bulk motions; (2)
detections to the i Rayleigh emission level; and (3) photometric acccuracy
limited only by photon statistics. our instrumentation has included: (a)
high dispersion Cassegrain spectrographs; ( b) an array of state-of-the-art
photon-counting detectors; and (c) a special telescope facility optimized to
reduce scattered light.
Cn 1982 .lily 1, the Principal Investigator changed his affiliation to the
Space Telescope Science Institute. With a changed budgetary profile now
supporting mainly UA graduate students and observing runs, the program
continues with the same PI and NASA grant NAGW-383 to ST ScI.
In the NSG-7634 grant period we made scientific advances and completed
two technical projects (which found dominant support under other grants but
have been crucial to this research effort). The current report summarizes
these achievements.
l
1
II. Scientific Research
Neutral oxygen was discovered in the lo torus and was shown to imply a
major energy path from neutrals to ions to electrons (3). Extensive neutral
clouds were discussed as possi')Iy a dominant particle and power source for the
torus (4).
Neutral sodium very far from To was shown to imply atom-ice momentum
transfer collisions are important for neutral cloud morphology 173.
The [SII) line profiles at 5.9 RJ
 indicate non-equilibrium and much
higher average ion energy than implied by a simplistic interpretation of the
half-width 18).
The non-relationship between [SII) brightness ane electron density at 5.9
RJ indicates the importance of change-exchange collisions in determining toms
ionization balance (12), as does the anomalous absence of OIII (13).
Tne failure of torus corotation at Io's orbit was discoveredt it probably
indicates the transfer of angular momentum from Jupiter to newly-created ions
[15).
Two reviews of torus physics were published (2, 111, plus a conference
review 141.
Other planetary studies published during this period included VLA
observations of To indicating no non-thermal sources (10); and continued work
on `Aenus thermal emission (1].
A technical paper vas published on the performance of 76" blaze angle
grating used in our new Cassegrain echelle spectrograph [9]. Also, a report
appeared on our clean telescope dust precipitator technique (21).
Seven abstracts for papers delivered at DPS/AAS meetings are listed in
the Bibliography.
2
tM. Technical Projects
(1) R4 Spectrograph (NSF Grant AST-7916476). This new instrument has 	 3
operated at the Whipple Observatory 61 ca telescope during all the bright
periods January-June 1982 and February 1982. Figure 1 is a cut-away sketch of
the unusual, quasi-Littrow echelle gratinq mount that allows all wavelengths
to be observed at the blaze peak. The flexure is relatively low (Fig. 2), the
optical performance is as designed: reciprocal dispersion - 1.5A mm-1 at
5800A and usable resolving power >10 5 . The low resolution mode (185A mm- 1 ) is
also operational.
Figures 3 and 4 are representative planetary spectra obtained in Spring
1982.
(2) Detectors. We :lave used a variety of etectors on the spectrograph this
Spring - the SAO CCD, the SAO intensified Reticon, our bare Reticon, and our
3-stage image tube. These detectors have offered different advantages for
different situations.	 Bare silicon gives high signal-to-noise, but has
difficulty with low light levels. The IRET is good for low light levels, but
it is one dimensional, and the current version has large-amplitude fixed
pattern noise.	 The image tube turns a photometric plate black at low
illumination, but it is not photometric. None of these systems nor the
weather were entirely satisfactory last spring, but we have been able to
demonstrate our method as Figures 3 and 4 show.
Our main-line detector for emission studies is the intensified CCD ai.=ay
from Dr. Lyle Broadfoot's laboratory. It has been operated at the telescope
in February 1983. This records single photoelectrons plus provide the two-
dimensional format needed to use the spectrograph's stigmatic optics for
imaging along the slit.
3
(3) Clean telescope (NASA Grant NAGw-262). We have developed a CM imaging
protocol to _document the condition of the mirror as manifested in stellar
scattered light profiles.
	 Figure 5 is such a recently-obtained profiles
synthesized from greatly-varying exposures, the longest of which saturate in
the inner region. The CCD was operated with no optical filter, and the
expected aperture-only diffraction profiled is drawn in for different
wavelengths spanning the band-pass. The approximately 1-2 orders of magnitude
increase in scattered light is due to dust superposed on the mirror, which was
decreased by a factor two when the primary was cleaned.
Our documentation technique is able to record a stellar profile over
about seven orders of magnitude in surface brightness in the distance range 1-
300 arc-seconds from the central object.
The mirror has not been protected by the dust precipator in the last
months, since that unit is being refurbished for operation without any
contaminating sticky surfaces. Reference (21) is a technical description of
the preciptator unit, which is being developed by Dr. Stuart Hoenig.
4
NSG-7634 Bibliography
1. J. Apt, R.A. Brown, and R.M. Goody (1980), "The character of thermal
emission from menus", J. Gaophys. Res. 85:7934-7940.
2. R.A. Brown (1981), "Heavy ions in Jupiter's environment", Planetary
Aeronomy and Astronomy (ad., S.K. Atreya and J.J. Caldwell), Adv.
Space Res. 1:75-82. Pergamon Press.
3. R.A. Brown (1981), "The Jupiter hot plasma torus:	 observed electron
temperature and energy flows", Astrophys. J., 244:1072-1080.
4. R.A. Brown and W. H. Ip (1981), "Atomic clouds as distributed sources for
the Io plasma torus", Science, 213:1493-1495.
S. N.M. Schneider, and R.A. Brown (1981), "Sodium remote from Io", Bull.
Amer. Astron. Soc., 13:730 (Abstract).
6. I. de Pater, R.A. Brown, at al. (1981), "Radio emission from Io", Bull.
Amer. Astron. Soc., 13:730 (Abstract).
7. R.A. Brown and N.M. Schneider (1981), "Sodium remote from lo', Icarus,
48:519-535.
S. R.A. Brown (1982), "The probability distribution of S + gyrospeeds in the
Ic ", J. Geophys. Res., 87:230-234.
9. R.A. Brown, R. Hilliard, and A. Phillips (1982), "The actual blaze angle
of the Bausch and Lomb R4 echelle grating", Applied Optics, 21:167-
168.
10. I. de Pater, W.J. Jaffe, R.A. Brown, and G.L. Berge (1982), "Radio
emission from lo", Astrophys. J. (Part 1), 261: 396-401.
11. R.A. Brown, C.B. Pilcher, and D.F. Strobel (1983), "Spectroscopic studies
of the Io torus", Physics of the Jovian Magnetosphere, (A. Dessler,
ad.), in press.
12. R.A. Brown and D.E. Shemansky, (1982). "On the nature of (SII) emission
from the lo plasma torus", Astrophys. J. (Part 1), 263: 433-442.
13. R.A. Brown, D.E. Shemansky and R.E. Johnson (1983), "A deficiency of 0111
in the lo plasma torus", Astrophys, J. (Part 1), 264: 309-323.
14. M.H. Acuna, R.A. Brown, et al., (1983), "Physics of the Jovian and
Saturnian Magnetospheres", Space Sci. Rev., in press.
5
NSG-7634 Bibliography (Continued)
15. R.A. Brown (1983), "Observed departure of the Io plasma torus from rigid
corotation with Jupiter`, Astzophys. J. (Part 2), in press.
16. N.M. Schneider, D.M. Hunten, and R.A. Brown (1982), "A spectroscopic
search for water vapour on VentAs", Bull. Am. Astron. Soc., 14:742
(Abstract).
17. C.C. Cunningham, D.M. Hunten, and R.A. Brown, "Ortho and para molecular
hydrogen in Jupiter's belts and zones", Bull Am. Astron. Soc., 14:730
(Abstract).
18. D.E. Shemansky, R.A. Brown, and R.E. Johnson, "A deficiency of OIII in
the Io plasma torus", Bull. Am. Astron. Soc., 14:763 (Abstract).
19. R.A. Brown and D.E. Shemansky, "On the nature of SII emission from
Jupiter's hot plasma torus", Bull. Am. Astron. Soc., 14:763
(Abstract).
20. R.A. Brown, The Io plasma torus does not corotate with Jupiter", Bull.
Am. Astron. Soc., 14:762 (Abstract).
6
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Studies of planetary extended atmospheres

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