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Vol 5, No. 12                22 Dec 1995                    ISSN 1065-3597

Notes from the Editor
   by Brett A. Stroozas, ISO Manager

   Welcome to the electronic newsletter for NASA's Extreme Ultraviolet
Explorer (EUVE) satellite, compiled and published monthly by the
Integrated/Intelligent Science Operations (ISO) group at the Center for
EUV Astrophysics (CEA) at the University of California, Berkeley (UCB).
The contents of this issue of the EUVE electronic newsletter are as

 1. Science News
    1.1 Recent EUVE Science Highlights
    1.2 Two New Scientists Join CEA/EUVE Team
    1.3 CEA/EUVE Presentations for the Jan 1996 AAS Meeting
    1.4 Abstracts of Recently *Accepted* EUVE Papers
 2. Science Operations News
    2.1 Public Data Release for 1 Jan 1996
    2.2 New GO Data Products Guide
    2.3 1:0 Phase 1 Transition Implemented in the ESOC
    2.4 On-Line Access to EUVE
 3. Applied Research Technology Notes
 4. CEA Job Listings

To comment on or make suggestions for the EUVE electronic newsletter,
please send e-mail to (Internet).

		    *** CEA/EUVE WISHES YOU A ***
		    ***  MERRY CHRISTMAS AND  ***
		    ***    HAPPY NEW YEAR!    ***

   The EUVE observatory performed well throughout the month of Nov
1995, conducting observations of the following Guest Observer (GO)
targets (alternate name and spectral type information taken from the
SIMBAD or internal CEA databases; "NOIDs" are unidentified objects):

    Target          Alternate     Spectral       Observation
     Name             Name          Type         GMT Date(s)     Notes

   Feige 24         WD 0232+035     WD:DA   31 Oct - 01 Nov 1995  ---
   cma1928+73       --------        AGN     31 Oct - 01 Nov 1995  RAP
   EUVE J0540-015   --------        NOID    01 Nov - 05 Nov 1995  ---
   EUVE J0256+080   --------        NOID    05 Nov - 05 Nov 1995  ---
   EUVE J0738+098   --------        NOID    05 Nov - 06 Nov 1995  ---
   Comet 1995q1     --------        Comet   06 Nov - 07 Nov 1995  TOO
   MGC +11-13-018   --------        NOID    07 Nov - 07 Nov 1995  ---
   EUVE J0256+080   --------        NOID    07 Nov - 07 Nov 1995  RAP
   EUVE J0249+099   --------        NOID    07 Nov - 07 Nov 1995  RAP
   UX Ari           HD 21242        G5IV    07 Nov - 10 Nov 1995  ---
   EUVE J0002-495   --------        NOID    07 Nov - 10 Nov 1995  RAP
   IRAS Cloud       --------        BKGD    11 Nov - 19 Nov 1995  ---
   UX Ari           HD 21242        G5IV    19 Nov - 22 Nov 1995  ---
   GD 246           WD 2309+105     WD:DA   22 Nov - 22 Nov 1995  CAL
   UX Ari           HD 21242        G5IV    22 Nov - 25 Nov 1995  TOO
   MKN 110          --------        NOID    25 Nov - 26 Nov 1995  ---
   EUVE J0003+243   --------        NOID    26 Nov - 26 Nov 1995  ---
   beta CMa         HD 44743        B1II    26 Nov - 28 Nov 1995  ---
   beta CMa tunnel  --------        ISM     28 Nov - 29 Nov 1995  SCAN
   beta CMA tunnel  --------        ISM     29 Nov - 30 Nov 1995  SCAN
   Capella          alpha Aur       G5III   30 Nov - 02 Dec 1995  ---

   Key to Notes:
	RAP = simultaneous Right Angle Program imaging observation
	SCAN = scanner imaging GO observation
	TOO = Target of Opportunity
	CAL = calibration observation

1. Science News

1.1 Recent EUVE Science Highlights

	by Dr. Pierre Chayer, EUVE Scientist

      Upon re-observation of the RSCVn star UX Ari on 19-22 Nov, the
   star was discovered to be in a extreme flaring state, in which it
   had brightened by a factor of ten over the observations obtained
   just 10 days earlier.  This event was not only the brightest RSCVn
   flare seen by EUVE, but also the largest such relative increase in
   source brightness for a RSCVn star ever measured by EUVE.  In
   response to this flare the GO -- Dr. Andrea Dupree -- immediately
   contacted the Project Office to request a Target of Opportunity
   (TOO) extension.  This TOO was approved and EUVE continued to
   observe UX Ari for an additional three days.  The flare was so
   strong and continuous that the star had not returned to normal at
   the end of the extension, but the EUV flux levels were at least
   factor of 3 above their quiescent value.  Inspection of the
   quick-look spectra shows substantial increases in the strengths of
   the highest temperature species, Fe XXIII and Fe XXIV.

	by Dr. Mark Hurwitz, EUVE Scientist

      EUVE spectrometer observations of the eclipsing DQ Her star EX
   Hya will be presented by Mark Hurwitz, Martin Sirk, and Stuart
   Bowyer at the Jan 1996 meeting of the American Astronomical Society
   (AAS) in San Antonio, TX.  This system shows strong flux modulation
   at both the binary period (5895 sec) and the white dwarf (WD) spin
   period (4022 sec).  A deep eclipse lasting 0.15 of the binary
   orbital period occurs just prior to phase 0.0 and indicates the
   presence of a bulge in the accretion disk with an optical depth
   about 1.8 at 100 Angstroms, or a column density (assuming neutral
   material) of about 1.3E+20 cm^(-2).  The flux during the eclipse
   from the secondary star is consistent with zero.  This eclipse is
   very short (~40 sec) and confines the EUV bright region to within a
   few WD radii of the primary.  The eclipse profile and centroid do
   not vary with the WD spin phase, indicating that most of the EUV
   emission arises on, or very close to, the WD surface as opposed to
   the inner regions of the accretion disk.

      The EUV flux varies as a function of WD spin phase by a factor
   3.7.  We attribute this to absorption by an accretion curtain that
   intercepts EUV light most strongly when both the EUV accretion
   region and the curtain face are most nearly in line with the
   observer.  The EUV modulation at the WD spin period can be
   successfully reproduced with a simple model of sinusoidally varying
   optical depth in the curtain.  When the source is bright, the EUV
   spectrum shows about ten narrow emission lines, primarily from
   highly ionized Iron.  The EUV spectrum is very similar to that of
   HR 1099, suggesting a peak temperature of a few times 10^7 K.

1.2 Two New Scientists Join CEA/EUVE Team

   Two new scientists --Drs. Pierre Chayer and Brian Flynn -- have
recently joined the EUVE team at CEA.  Please join us in welcoming
them both to CEA and to the EUVE Project!

   Dr. Pierre Chayer obtained his PhD in 1995 at the Universite de
Montreal where, under the supervision of Professor Gilles Fontaine, he
studied diffusion processes in the photospheres of hot white dwarf
stars.  His thesis dissertation (entitled "Theorie de la levitation
radiative dans les etoiles naines blanches chaudes") represents the
most up to date and comprehensive calculations of selective radiative
acceleration on a large group of atomic species for white dwarf stars.
Hired as a post-doctoral researcher by Dr. Stephane Vennes and
Professor Stuart Bowyer, Dr. Chayer arrived at CEA in Jan 1995.  His
principal research activities then consisted of analyzing the far and
extreme ultraviolet spectra acquired by EUVE, ORFEUS, and IUE for an
important sample of white dwarfs.  His abundance determinations will
constitute a critical test of the diffusion theory in white dwarfs.
   In Nov Dr. Chayer accepted an Assistant Research Astronomer
position at CEA, where he will continue to actively pursue his
research on white dwarf stars.  His service duties consist of
providing science/technical support to the EUVE GO community and of
informing the public of exciting EUVE results through the monthly
highlights and the Science Bulletin.
   Dr. Chayer is also an accomplished educator; for several years He
has taught introductory level astronomy for science majors at the
Universite du Quebec in Montreal.  In his spare time he enjoys good
wine, blues guitar, and ice hockey.

   Dr. Brian Flynn graduated from the University of California,
Berkeley, in 1986, where he majored in astronomy and in applied
mathematics.  He then worked for two years as a research assistant at
NASA Ames Research Center.  From 1988-93 he attended graduate school
at Boston University, where he studied sodium emission around Jupiter
and the Moon.  After graduate school Dr. Flynn spent two years as a
post-doctoral researcher at Southwest Research Institute in San
Antonio, TX, and Boulder, CO, where he studied the Moon's atmosphere
and the properties of icy moons in the outer solar system.
   Dr. Flynn began his employment at CEA in Dec 1995 as an Assistant
Research Astronomer.  He looks forward to analyzing EUVE's vast
background data set in order to learn more about such phenomena as the
Earth's magnetosphere and extended atmosphere, and the local
interstellar medium.  His service duties will include acting as a Duty
Scientist for the science payload instruments.
   Dr. Flynn and his wife, Lori, enjoy outdoor activities such as
gardening, hiking, and skiing.  They also like to spend time with
family and friends, and both enjoy cooking and dining out.  They look
forward in the coming years to taking advantage of the many activities
that the Bay Area has to offer, and to visiting the beautiful north
coast and Sierras.

1.3 CEA/EUVE Presentations for the Jan 1996 AAS Meeting

   The following is a list of the CEA/EUVE presentations for the 187th
meeting of the American Astronomical Society (AAS) that will be held
14-18 Jan 1996 in San Antonio, TX.

   Bowyer, M.M. Sirk, and M. Hurwitz
   Christian, M. Mathioudakis, and J.J. Drake
   TAURI, J. Dupuis, S.L. Cully, T. Rogriguez-Bell, and O.H.W.
   S.B. Howell, M.M. Sirk, and R.F. Malina.
   SECONDARIES (III, IV, V; A, F, G, K), S. Vennes, J.R. Thorstensen,
   and D. Christian
   Hawkins, N. Levandovsky, L. Wong, V. Arellano, P. Ford, K. Nguyen,
   and R.F. Malina
   Bevan, D. Christian, N. Craig, E. Olson, and J. Sommers
 o THE EUVE SPECTRAL ATLAS, H. Jessop, K. Anderson, N. Craig, J.
   Sommers, and B. Stroozas
   X. Wu, and S. Bowyer
   Stroozas, J. Sommers, D. Christian, and R.F. Malina

1.4 Abstracts of Recently *Accepted* EUVE Papers

   Included below are abstracts of EUVE-related papers recently
*accepted* for publication.  For those papers authored by CEA
personnel, the CEA publication numbers are indicated.  Unless
otherwise noted, researchers may obtain preprints of the CEA papers by
sending an e-mail request containing the publication number(s) of
interest to
   Researchers are encouraged to contribute *accepted* EUVE-related
abstracts for inclusion in future editions of this newsletter;
abstracts or preprints will also be posted under the CEA WWW Home
Page.  Please send all abstracts or preprints to


N. Craig, S.B. Howell, M.M. Sirk, and R.F. Malina
To appear in Astrophysical Journal Letters.  [CEA publication #704]

   The source EUVE_J1429-38.0 was discovered serendipitously by the
Extreme Ultraviolet Explorer (EUVE) satellite on 1993 March 5.
Optical spectroscopy confirms a cataclysmic-variable-type optical
counterpart for the source, showing Balmer, He I and Ca emission, as
well as strong He II emission.  The optical spectrum, the apparent
high/low state behavior, and possible weak cyclotron humps visible in
the spectrum indicate that this star is likely to be an AM Herculis
system, but the possibility of being a DQ Her, or an unlocked AM Her
system can not be excluded.  Analysis of the highly modulated EUVE
photometry yields a period of 2 hr 22 min, which we conclude is the
binary orbital period.  In addition, a 57 min period is also present.
An orbital period of 2.5 hr would make EUVE_J1429-38.0 only the third
known AM Her system within the cataclysmic variable period gap, all
three of which were discovered through EUV observations.


R. Lieu, J.P.D. Mittaz, S. Bowyer, F.J. Lockman, C.-Y. Hwang, and
   J.H.M.M. Schmitt
To appear in Astrophysical Journal Letters.  [CEA publication #705]

   An observation of M87, the central galaxy of the Virgo cluster, was
performed by the Deep Survey (DS) telescope aboard EUVE, in the
0.065-0.245 keV energy band.  A central source and an extended
emission halo of radius ~20 arcmin are clearly visible in the data,
and represent the first detection of cluster gas emission in the EUV.
The emission cannot be explained by the well-known cluster gas
(Fabricant & Gorenstein 1983; Forman, Jones, & DeFaccio 1985; Stewart
et al. 1984a; Bohringer et al. 1994) at X-ray temperatures.  Instead,
it is necessary to introduce a second gas component, with temperature
between 5E+5 K and 1E+6 K.  The rapid cooling of plasmas at such
temperatures implies a mass accretion rate of > 300 M_solar per year.
It is unlikely that the phenomenon is directly related to a cooling
flow, which involves a much lower accretion rate of ~10 M_solar per


D.J. Christian, J. Drake, and M. Mathioudakis
To appear in Proceedings of the 9th Cambridge Workshop, Cool Stars,
   Stellar Systems, and the Sun, ed. R. Pallavicini and A. K. Dupree,
   PASP Conference Series (San Francisco: ASP), 1996.  [CEA
   publication #706]

[No abstract.  This paper discusses a variability analysis on a sample
of cool late-type stars from the EUVE Right Angle Program.]   


N. Craig
To appear in Proceedings of the 9th Cambridge Workshop, Cool Stars,
   Stellar Systems, and the Sun, ed. R. Pallavicini and A. K. Dupree,
   PASP Conference Series (San Francisco: ASP), 1996.  [CEA
   publication #707]

[No abstract.  This paper discusses results from the EUVE Optical
Identification program.]


G.F. Bignami, P. A. Caraveo, R. Mignani, J. Edelstein, and S. Bowyer
Astrophysical Journal Letters, 456, L111, 1996.  [CEA publication

   A new set of ground-based optical, HST UV and EUVE data on Geminga
are presented.  The object, identified with a high proper motion
isolated neutron star (INS), is seen to emit thermal radiation with a
temperature between (2.2-2.8)E+5 K.  This is compatible with the
global thermal emission from the surface of a standard neutron star of
Geminga's spindown age located at the distance of about 160 pc,
recently measured through its annual parallax.  However, in the
"optical" (3400-8000 A) range, combined ground based and HST data
suggest the presence of a spectral feature (either in emission or
possibly in absorption) superimposed to the Rayleigh-Jeans continuum.
Its simplest interpretation could be related to an ion (H or He)
cyclotron frequency for the object's canonical magnetic field of
1.5E+12 G.  This is the first observational evidence for an optical
spectral feature in an INS. A search for a similar effect should be
feasible also for PSR0656+14, the only other INS possibly showing
optical thermal emission from its surface.


M. Abbott
To appear in Proceeding of the Fifth Annual Conference on Astronomical
   Data Analysis Software and Systems (ADASS '95), Oct. 22-25, 1995,
   Tucson, AZ.  [CEA publication #711]

   The EUVE Knowledge Base (KB) will be an online repository of the
expertise of the developers and users of the Extreme Ultraviolet
Explorer (EUVE) satellite and data analysis software.  It will help to
address the issue of maintaining adequate support for Guest
Investigators after the project has entered a purely archival stage
with few or no personnel available to answer questions.  It will also
help to preserve knowledge about EUVE as particular people may leave
the project.  The KB will be accessible as a hypertext document in the
CEA WWW site.  Information will be stored internally in small "units,"
and cross-references will be created between individual units
on-the-fly as they are delivered to users.  This will enable us to
tailor the documents to allow each user to explore the KB as
efficiently as possible.


M. Abbott, T. Kilsdonk, C. Christian, E. Olson, M. Conroy, R.
   Brissenden, D. Van Stone, and J. Herrero
To appear in Proceeding of the Fifth Annual Conference on Astronomical
   Data Analysis Software and Systems (ADASS '95), Oct. 22-25, 1995,
   Tucson, AZ.  [CEA publication #712]

   ETOOLS is a software development project working to produce a
package of general purpose tools for reducing event data.  The package
is intended for use with event data from any observatory.  In addition
to applications for basic analysis, ETOOLS will contain software
libraries for extending the package to specific needs.


L. Wong, F. Kronberg, A. Hopkins, F. Machi, and P. Eastham
To appear in Proceeding of the Fifth Annual Conference on Astronomical
   Data Analysis Software and Systems (ADASS '95), Oct. 22-25, 1995,
   Tucson, AZ.  [CEA publication #713]

   In compliance with NASA administrator Daniel Goldin's call for
faster, cheaper, better NASA projects, the Center for EUV Astrophysics
has developed and deployed a partially autonomous, satellite-telemetry
monitoring system to monitor the health of the Extreme Ultraviolet
Explorer (EUVE) satellite payload.  Originally, the telemetry was
monitored on a 24-hour basis by human operators.  Using RTworks, a
software package from Talarian Corporation, the EUVE project has
developed a rule-based expert system capable of detecting critical
EUVE payload anomalies and notifying experts.  This paper discusses
the process of capturing and codifying the operations knowledge into
rules and how this rule-based system is applied in our mission


E. Olson, F. Girouard, and A. Hopkins
To appear in Proceedings of the Fifth Annual Conference on
   Astronomical Data Analysis Software and Systems (ADASS '95), Oct.
   22-25, 1995, Tucson, AZ.  [CEA publication #714]

   The ability to store and access mission data is a critical element
of mission operations.  The Center for EUV Astrophysics, which
operates the Extreme Ultraviolet Explorer (EUVE) Science Operations
Center for Goddard Space Flight Center, is currently developing the
Tomographic Experiment using Radiative Recombinative Ionospheric EUV
and Radio Sources (TERRIERS) ground system in collaboration with Ames
Research Center and AeroAstro for Boston University.  CEA is designing
a general-purpose data archive for storing, indexing, and accessing
spacecraft telemetry.  A specification file will describe the
mission-specific information about telemetry formats.  By reusing
software components, as might be possible with the Multi-Mission
Archive, new missions will be able to focus their efforts on
instrumentation and analysis.


2. Science Operations News

2.1 Public Data Release for 1 Jan 1996
        by Dr. Nahide Craig, Archive Scientist, ISO Science Support Team

   The table below lists the GO observations that become public on 1
Jan 1996.  For each entry is given the target name, the approximate
exposure time in ksec, the GMT start and end date(s) for the
observation, the spectral type of the target, and the data
identification code.  All public data sets can be ordered from the
archive via WWW and electronic or postal mail (see addresses below).
Please be sure to include in your order the DataID(s) of interest.
Processed data sets are shipped on 8mm tape (or, if requested, on
CD-ROM) via postal mail.
   The data rights policy for GO observations states that GOs have
proprietary rights to the data for one year from the date (s)he
receives it.  It is often the case that long observations are broken
up over many months; e.g., an observation approved for 60 ksec may
actually be observed for 10 ksec one month, 20 ksec the next and 30
ksec three months later.  In such cases the one-year proprietary
period begins after the GO is sent the final piece of the completed

      Target        ~Exp     Observation Date(s)     SpT      DataID
       Name        (ksec)    Start           End

     Data Sets Available 1 Jan 1996:

     AB Dor          100     12 Nov - 15 Nov 1994    K1IIIp   go0248
     AB Dor           42     15 Nov - 17 Nov 1994    K1IIIp   go0249 
     Beta Cet        100     30 Sep - 04 Oct 1994    K0III    go0250 
     Beta Cet         75     04 Oct - 06 Oct 1994    K0III    go0251 
     RE 0029-632     100     07 Sep - 11 Sep 1994    WD:DA    go0252
     RE 0029-632      11     11 Sep - 11 Sep 1994    WD:DA    go0253 
     RE 0506-213      73     17 Nov - 20 Nov 1994    dM2e     go0254 
     FK Aqr          100     11 Sep - 15 Sep 1994    M0Vpe    go0255 
     FK Aqr           21     15 Sep - 16 Sep 1994    M0Vpe    go0256 
     HD 220657       100     16 Sep - 19 Sep 1994    F8IV     go0257 
     HD 220657       100     19 Sep - 23 Sep 1994    F8IV     go0258 
     HD 220657        17     23 Sep - 23 Sep 1994    F8IV     go0259 
     Moon              1     12 Nov - 12 Nov 1994    SolSys   go0260 
     P/Borrelly       53     20 Nov - 22 Nov 1994    Comet    go0261 
     UX Ari           80     19 Oct - 22 Oct 1994    G5IV     go0262 
     VY Ari          100     06 Oct - 10 Oct 1994    K0       go0263 
     VY Ari           52     10 Oct - 12 Oct 1994    K0       go0264 
     V471 Tau        100     28 Nov - 01 Dec 1994    K2+DA2   go0265 
     V471 Tau         18     01 Dec - 02 Dec 1994    K2+DA2   go0266 
     V711 Tau          2     30 Sep - 30 Sep 1994    G9V      go0267 *

     Notes:  "*" is a calibration observation

2.2 New GO Data Products Guide
	by Anne Miller, EGO Center Technical Writer

   Version 1.6 of EUVE Guest Observer Data Products Guide has been
released and is available on the CEA ftp site.  (See "Accessing CEA,"
below, for details on using the site.)  New material in the Data
Products Guide describes the following:

 1. Remapping of spectrometer events.  The event pipeline program
    'cep' now uses a source position derived from the deep survey data
    (when such a position can be found using the new task 'dscen').
 2. Boundaries of the pixel space covered by truncated event lists in
    QPOE files.
 3. New definition of earth blockage applied in the default valid data

All GO data is now being processed with version 1.6 of the IRAF/EUV
package, and the new Data Products Guide gives the most accurate
description of the data files and processing.  Version 1.6 of the EUVE
Guest Observer Software User's Guide will be released as soon as

2.3 1:0 Phase 1 Transition Implemented in the ESOC
	by Brett A. Stroozas, ISO Manager

   The EUVE Science Operations Center (ESOC) continues to work on the
multi-phase transition from a one-shift to a zero-shift (1:0) payload
operations scenario.  The goal of 1:0 is to design and apply
automation techniques and applications in order to eliminate all
routine payload controller shift work in the ESOC.  Upon completion of
1:0 in the Spring of 1996, the ESOC will no longer be staffed for
payload operations on a daily basis.  Controllers will, however,
remain available as necessary to attend to maintenance issues and to
respond to ground and flight anomalies.
   On 15 Nov the EUVE Science Operations Center (ESOC) completed the
first phase of the 1:0 transition.  In Phase 1 all payload telemetry
monitoring is now being handled autonomously by augmented intelligence
(AI) software that pages an on-call controller when it detects an
   The ESOC is now working to implement the transition to the Phase
1.5 "semi-operational" zero-shift scenario in which the ESOC will not
be staffed during weekends and holidays.  This transition is now
scheduled to occur in early Jan 1996 (pending GSFC approval).  By
eliminating weekend and holiday ESOC staffing we will have taken the
first step into an operational zero-shift environment.
   In preparation for this transition the ESOC will be moving to a
"simulated" Phase 1.5 scenario during the Christmas Holiday period.
In this simulation the ESOC will not be staffed on weekends and
holidays; instead, a controller will login remotely to the ESOC
computer network in order to ensure that everything is working as
expected, and to attend to various daily chores (all of which can be
handled remotely).  The Phase 1.5 simulation will provide the ESOC
with valuable experience and will relieve controllers of the burden of
having to work during the Holiday Season.

2.4 On-Line Access to EUVE

   Listed below are the various methods for on-line access to EUVE:

 o CEA World Wide Web (WWW)
   telnet 200 (for those without a WWW browser)
 o anonymous FTP
	Name:  anonymous
	Password:  type_your_full_e-mail_address
 o anonymous gopher
 o EUVE Electronic Newsletters
     Past issues -- available via the CEA WWW site
     Subscriptions -- mail ("subscribe
     Post message to all subscribers:  mail
 o GI Program
     Are you interested in finding out about or using EUVE data?  Do
     you need help in understanding EUVE data sets?  Do you need help
     in using the available EUVE data analysis software tools?  If you
     answer "yes" to any of the above, the Guest Investigator (GI)
     Program at CEA can help YOU!  For more information see the CEA
     WWW site or contact the Archive (
 o Public RAP
     The Public Right Angle Program (RAP) is an easy method for
     researchers to propose for long-exposure EUVE imaging data.  For
     more information on the Public RAP and the simple proposal
     process see the CEA WWW site or contact the EGO Center
     (  Mail all proposals to
 o Contact information for the EUVE Science Archive or GO Center:

			Center for EUV Astrophysics
			2150 Kittredge St.
			Berkeley, CA  94720-5030

		Archive 			EGO Center
	510-642-3032 (voice)    	510-643-8727 (voice)
	510-643-5660 (fax)      	510-643-5660 (fax)

3. Applied Research Technology Notes
	by Tom Morgan, EUVE ART Manager

   CEA is involved in a collaborative effort on the EUVE Virtual
Environment (EVE) project.  The purpose of this effort is to develop a
three-dimensional visualization tool for EUVE operations.  This tool
will serve as a means to visually forecast spacecraft constraint
conflicts during the observation planning process, and to visually
investigate and resolve flight anomalies.  EVE is a collaborative
effort between NASA Ames Research Center (ARC), NASA Goddard Space
Flight Center, and CEA's Applied Research Technology group.
   Delivery to CEA of ARC's Virtual Environment Vehicle Interface
(VEVI) in early Sep marked an important milestone for the EVE project.
Efforts at CEA and GSFC are currently focusing on evaluating the VEVI
3.O release and customizing EUVE functionality.

4. CEA Job Listings
	by Cathie Jones, CEA Personnel Manager

Programmer Analyst II, Job # 09-323-30 (full-time career position)

   Serve as a software engineer at the Center for EUV Astrophysics.
Design prototype software systems for low cost automated satellite
operations and human computing.  General programming areas will be
supporting Artificial Intelligence (AI) research in
model/rule/constraint-based reasoning as applied to orbiting vehicles
and data acquisition/control loops.
   Qualifications include a strong background in Electrical
Engineering, Computer Science, Space Engineering, and/or Information
Systems, with proven software development experience required.
Experience with the design and implementation of AI software, and
orbiting vehicle ground/flight software design required.  Experience
in a combination of the following: UNIX (SUN, SGI, HP), C, C++, LISP,
Fortran, and scripting; development of intelligent image processing
systems, fault diagnosis, fuzzy controllers, network algorithms and
protocols, network based parallel computing; product design
experience.  CASE tool experience a plus.  Experience with WWW
(Netscape, Mosaic), GUI development, windowing systems preferred.
   To apply, formal resume must be submitted to:

		Personnel Office #3540
		Box 09-323-30
		2200 University Ave.
		Berkeley,  CA  94720-3540

  The EUVE Electronic Newsletter is issued by the Center for Extreme
  Ultraviolet Astrophysics, University of California, Berkeley, CA
  94720, USA.  The opinions expressed are those of the authors.  EUVE
  Principal Investigators and Newsletter Publishers: Dr. R.F. Malina
  and Professor S. Bowyer.  ISO Manager and Newsletter Editor: B.A.
  Stroozas.  Funded by NASA contract NAS5-29298.  Send newsletter
  correspondence to

  The EUVE project is managed by NASA's GSFC: Paul Pashby, GSFC
  Project Manager; Dr. Yoji Kondo, Project Scientist; Dr. Ronald
  Oliversen, Deputy Project Scientist; Mr. Kevin Hartnett, Project
  Operations Director.  NASA HQ: Dr. Robert Stachnik, Program
  Scientist; Dr. G.  Riegler, Program Manager.  Information on the
  EUVE GO Program is available from Dr. Y. Kondo, Mail Code 684, GSFC,
  Greenbelt, MD 20771 at (301) 286-6247 or e-mail to

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