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Vol 6, No. 1                 31 Jan 1996                    ISSN 1065-3597
	  (C) 1996, Regents of the University of California

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 Abstracts of Recently *Accepted* EUVE Papers
 2. Science Operations News
    2.1 Accepted Cycle 4 Proposals and Targets
    2.2 Public Data Release for 1 Feb 1996
    2.3 On-Line Access to EUVE
 3. CEA Job Listings

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

   The EUVE observatory performed well throughout the month of Dec
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

   Capella          alpha Aur       G5III   30 Nov - 04 Dec 1995  ---
   RE 1016-053      EUVE J1016-053  DA+M    04 Dec - 06 Dec 1995  ---
   EK Dra           --------        G0V     06 Dec - 13 Dec 1995  ---
   V837 Tau         HD 22403        G2V     06 Dec - 13 Dec 1995  RAP
   Mkn 142          --------        AGN     13 Dec - 13 Dec 1995  ---
   RE J0521-102     EUVE J0521-104  DA      13 Dec - 13 Dec 1995  RAP
   PN G215.2-24.2   --------        PlanNeb 13 Dec - 13 Dec 1995  RAP
   EUVE J0503+231   --------        NOID    13 Dec - 13 Dec 1995  ---
   1156+295         --------        AGN     13 Dec - 13 Dec 1995  RAP
   RE J1149+284     EUVE J1149+287  CV-AM   13 Dec - 13 Dec 1995  RAP
   Moon             --------        SolSys  13 Dec - 13 Dec 1995  ---
   beta CMa         HD 44743        B1II    13 Dec - 15 Dec 1995  ---
   C 0512-400       NGC 1851        LMXB    15 Dec - 16 Dec 1995  ---
   rxirMCG+08-12-003 -------        AGN     15 Dec - 16 Dec 1995  RAP
   RE J0720-314     EUVE J0720-317  DA      16 Dec - 20 Dec 1995  ---
   zeta Pup         --------        O4f     20 Dec - 25 Dec 1995  ---
   Coma Cluster     --------        GalClus 25 Dec - 28 Dec 1995  ---
   EUVE J0700-034   --------        NOID    25 Dec - 28 Dec 1995  RAP
   EUVE J1034+073   --------        NOID    28 Dec - 29 Dec 1995  ---
   beta CMa         HD 44743        B1II    29 Dec - 31 Dec 1995  ---
   GJ 354.1         HD 82443        K0      31 Dec - 11 Jan 1996  ---

   Key to Notes:
	RAP = simultaneous Right Angle Program imaging observation

1. Science News

1.1 Recent EUVE Science Highlights
	by Dr. Pierre Chayer, EUVE/CEA Scientist

 o Light Curve Obtained of 5.75 millisecond Pulsar EUVE J0437-4715

      Jules Halpern, Chris Martin, and Herman Marshall obtained a
   light curve of the 5.75 millisecond pulsar J0437-4715 using the
   Deep Survey instrument on the EUVE satellite.
         This is the first EUVE observation to make use of the full 0.5
   millisecond time resolution of the spacecraft clock in WSZ mode.
   The single-peaked pulse profile contains approx 4200 photons, and
   is the result of correcting the photon arrival times from the
   satellite to the solar system barycenter, as well as from the
   pulsar to the center of mass of its 5.74 day binary orbit.  It is
   not yet established whether the observed emission (from this or any
   recycled pulsar) is non-thermal from the magnetosphere, or surface
   thermal emission from a hot polar cap.
         A combined analysis of the EUVE and ROSAT data, to appear in The
   Astrophysical Journal, is used to place limits on the temperature
   and surface area of thermally emitting regions that might be

1.2 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


D.H. Cohen, R.G. Cooper, J.J. MacFarlane, S.P. Owocki, J.P.
  Cassinelli, and P. Wang
To appear in the Astrophysical Journal.

   We use both EUVE and ROSAT data sets to test three general pictures
-- coronal, wind shock, and external -- for the production of the
observed high energy emission from the B giant, epsilon CMa (B2 II).
Because of the very low interstellar opacity along its line of sight,
epsilon CMa is the only early-type star that has strong emission lines
detected with the EUVE spectrometers.  The line spectrum provides the
first solid observational evidence that the emission is thermal.
Theoretical EUV spectra based upon two-temperature model fits to the
ROSAT data predict too much flux, especially in the iron line complex
near 175 Angstroms.  We use progressively more complex models until we
are able to achieve a fit to the combined data sets.  We find that
both a temperature distribution in the emitting plasma and some
attenuation of the EUV and soft X-ray emission by the ionized stellar
wind must be included in the models.  The model fitting indicates that
only 13 to 21 percent of the emission line complex near 175 Angstroms
escapes the wind.  This amount is consistent with the wind shock
model, in which the emitting material is distributed throughout the
stellar wind.  It is much more absorption than is predicted by the
external source model, where all of the emitting material is at radii
beyond the cold stellar wind.  And it is significantly less absorption
than is expected in the coronal model, given what is known about the
star's mass loss rate.  The derived temperature distribution and wind
filling factor of hot gas are also qualitatively consistent with our
numerical simulations of wind shocks.  We conclude that although the
observed flux from epsilon CMa in the interval 54 eV < E < 100 eV is
approximately the same as that above 100 eV, because of wind
attenuation the total generated radiation in the EUV band between 54
eV and 100 eV is 5 times greater than that in the X-ray region.


I. Hawkins and R.F. Malina
Presented at the International Astronautical Federation, Symposium: P,
  Space and Education Symposium, Session: P2, Education Structures,
  1995.  [CEA publication #678]

   We describe the bilingual Astronomia Para La Familia/Family
Astronomy Project, which is a bilingual (Spanish-English) education
outreach project of UC Berkeley's Center for EUV Astrophysics.  The
project develops and operates weekend astronomy and space science
workshops for 7-8 grade students and their parents of Hispanic
background. The project is patterned on the successful Family Science
and Family Math programs from UC Berkeley's Lawrence Hall of Science.
Family Astronomy has been designed and implemented in collaboration
with UC Berkeley`s Graduate School of Education, the East Bay
Consortium (a non-profit organization that develops education programs
involving students and teachers of the Oakland Unified School
District), and the Association of Mexican Professionals of Silicon
Valley. The collaboration also involves Professor Emily van Zee from
the University of Maryland's College of Education and a graduate
student from the UC Berkeley School of Education to help guide the
design and assess the effectiveness of the program.  The workshops
will be pilot-tested in fall of 1995 during weekend activities for 7-8
grade students and their families as part of East Bay Consortium
programs.  This project investigates methods by which collaboration
among teachers, other professional educators, scientists, and families
can help increase (a) middle-school students' and their parents'
interest in science as well as (b) parental involvement in the science
education of their children.  The study focuses on collaborative
science activities enhanced by images and data accessible through
World Wide Web technology carried out in an informal and supportive
   The workshops focus on hands-on activities requiring child and
parent participation that demonstrate explicit concepts in astronomy
and space science.  Such activities include observations of
astronomical objects using the naked eye and measuring instruments
constructed during the workshops, such as a simple astrolobe.  The
program includes a visit to the satellite operations center for the
NASA Extreme Ultraviolet Explorer Satellite at the University of
California, Berkeley, and involves workshop participants in using the
Internet to access astronomy and space science data on the World Wide
Web. All the project materials, activities, and methods are being
documented on the CEA Education World Wide Web pages (URL: The CEA's Science Information
Infrastructure NASA-funded project disseminates the materials to
collaborating science museums such as the Exploratorium and Lawrence
Hall of Science.


S. Bowyer
In X-Ray and EUV/FUV Spectroscopy and Polarimetry, ed. S. Fineschi,
  Proceedings of SPIE 2517, 90-96, 1995.  [CEA publication #679a]

   The development of grazing incidence optics for extreme ultraviolet
(EUV) astronomy occurred in a vastly different science-political
environment than that of X-ray astronomy.  X-ray astronomy had been
proven as an extremely useful field of research, and in the
environment of the 1960s funds were available for X-ray glass mirror
systems costing tens of millions of dollars for a single telescope. In
that era, EUV astronomy had not yet been demonstrated as a viable
field, and indeed, the general belief was that only a few astronomical
sources would be observable in this band. In that environment there
was no hope of obtaining funding for EUV telescopes similar to those
used in X-ray astronomy. As a consequence, an entirely different
approach was employed in the development of EUV grazing incidence
   The general approach was to attempt to make grazing incidence EUV
optics out of metal. In the end, the best of these optics were as good
as the X-ray glass optics developed for the Einstein Observatory, but
with a cost of 1/20 of the Einstein mirrors.
   The various technologies developed in order to carry out EUV
astronomy are discussed with an emphasis on EUV grazing incidence
mirrors. A report of a few of the astronomical results obtained
through the use of these optics are presented.


S. Bowyer
To appear in Proceedings of Frascati Workshop 1995, held in Vulcano,
  Italy.  [CEA publication #680]

   From the beginnings of NASA in the late 1950's, the promise was
offered that the entire electromagnetic spectrum would be explored
providing new insights into stars, the Galaxy, and the universe.
There was one exception to this expansive view; the extreme
ultraviolet band of the spectrum, ranging from approximately 90 to 900
A, would be forever hidden from our view, because of severe absorption
due to the interstellar medium.  Only in the early 1990s was this
overall appraisal shown to be incorrect with over 400 sources of
extreme ultraviolet radiation detected with the English Wide-field
camera on the German ROSAT satellite, (Pye et al. 1995) and more than
700 sources detected with NASA's Extreme Ultraviolet Explorer (EUVE;
Bowyer et al. 1995).
   In the following, I would like to briefly comment on a few of the
results obtained with EUVE.


N. Craig, S.B. Howell, M.M. Sirk, and R.F. Malina
Astrophysical Journal Letters, 457, L91, 1996 [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 cannot 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
Astrophysical Journal Letters, 458, L5, 1996.  [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 year.


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 Conf. Ser. (San Francisco: ASP), 1996.  [CEA publication #706]

   Much progress has been made toward our understanding of coronal
activity in late-type stars as the result of observations with
spaceborne instrumentation (UV, EUV, and X-rays). A general picture
has emerged that the most active stars are the fastest rotators.  EUV
radiative losses are comparable to the X-ray losses and are important
in the energy balance of the corona (Mathioudakis et al. 1995).  The
Extreme Ultraviolet Explorer (EUVE) 58 to 740 A bandpass is
particularly sensitive to the coronal emission.


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 Conf. Ser. (San Francisco: ASP), 1996.  [CEA publication #707]

   The most recently published EUV source catalogs reveal the types of
objects observable in the EUV (Bowyer et al. 1996; Pounds et al.
1993).  About 40% of the sources are late-type stars (G, K, and M
dwarfs and tidally interacting binaries) whose coronae have typical
temperatures of ~(1-10)E+6 K (e.g., Pallavicini 1989). The other ~27%
comprise primarily hot white dwarfs (WD), with a smaller number of
early-type stars, active galactic nuclei, planetary nebulae,
cataclysmic variables, X-ray binaries, one or two novae, and thermally
emitting neutron stars.  The remaining ~33% of all sources are NOIDs
(sources without plausible optical counterparts).


R. Lieu, J.P.D. Mittaz, S. Bowyer, F.J. Lockman, C.-Y. Hwang, and
  J.H.M.M. Schmitt
To appear in Proceedings of the X-ray Meeting in Wurzburg.  [CEA
  publication #710]

   An observation of M87, the central galaxy of the Virgo cluster, was
performed in the 0.065-0.245 keV energy band by the deep survey (DS)
telescope aboard the Extreme Ultraviolet Explorer (EUVE).  A central
source and an extended emission halo of radius ~120 kpc 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 at X-ray temperatures (Fabricant & Gorenstein
1983; Forman, Jones, & DeFaccio 1985; Stewart et al. 1984a; Bohringer
et al. 1994).  Instead, it is necessary to introduce a second gas
component, with temperature between 5E+5 and 1E+6 K.  The rapid
cooling of plasmas at such temperatures implies a mass accretion rate
of > 300 M_(solar) per yr.  It is unlikely that the phenomenon is
directly related to a cooling flow, which involves a much lower rate
of ~10 M_(solar) per yr.  More recently, we examined ROSAT PSPC data
of other galaxy clusters located in directions of low galactic
absorption, and found that all of them show evidence of extended
central emission at T ~ 1E+6 K.  In particular, the Coma cluster,
which was also detected by the EUVE sky survey, exhibits soft emission
out to a radius of ~1 Mpc from the X-ray centroid, with an estimated
gas cooling (accretion) rate of ~2E+5 M_(solar) per yr.  This result
is a major surprise, since Coma does not have a cooling flow.


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
exper tise 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 proceedings 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
(CEA) in cooperation with NASA Ames Research Center has developed and
deployed a partially autonomous satellite-telemetry monitoring system
to monitor the health of the Extreme Ultraviolet Explorer (EUVE)
payload. Originally, telemetry was monitored on a 24 hour basis by
human operators. Using RTworks, a software package from Talarian
Corporation, our development team has developed a rule-based, expert
system capable of detecting critical EUVE payload anomalies and
notifying an anomaly coordinator. This paper discusses the process of
capturing and codifying the knowledge of EUVE operations into rules
and how our rule-based system is applied in EUVE autonomous


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 Accepted Cycle 4 Proposals and Targets
	by Dr. Ron Oliversen, Deputy Project Scientist @GSFC
        and Dr. Damian Christian, CEA Scientist, ISO Observation
		Support Team

   The following lists the approved Cycle 4 observing programs.  For
each program is listed the proposal ID (PID), Principal Investigator
(PI), and proposal title (TITLE).  Also listed for each proposal are
the approved targets (TARGET), associated exposure time in ksec
(KSEC), and whether the target is priority 1 or 2 (TYPE).  Note that
there may still be some small changes made to this list.


002 -- Lieu -- Origin of the EUV Emission from the Center of the Virgo
    Cluster Spectrum
	M87		180	1
003 -- Lieu -- EUV Emission from Clusters of Galaxies
	COMA		35	1
004 -- Peters -- EUVE Observations of Active B Stars
	ALPHA_COL	200	2
005 -- Drake -- Abundance Anomalies in Stellar Coronae
	KSI_UMA		350	1
006 -- Giampapa -- The Coronae of Quiescent M Dwarf Stars
	GL_205		400	1
007 -- Stern -- EUVE Observations of the Hyades Giants
	GAMMA_TAU	250	2
010 -- Lampton -- Verification and Identification of EUVE NO-ID Sources
	EUVE_J0858-002	20	2
	EUVE_J0908+326	20	2
	EUVE_J1100+344	20	2
	EUVE_J1434+357	20	2
	EUVE_J1618-179	20	2
	EUVE_J1627+101	20	2
	EUVE_J1906+169	20	2
	EUVE_J1935-192	20	2
	EUVE_J2055+164	20	2
	EUVE_J2206+637	20	2
	EUVE_J2240+097	20	2
016 -- Kaastra -- THe Physical Conditions of the Warm Absorber in NGC 5548
	NGC_5548	300	2
018 -- Mauche -- EUVE Spectroscopy of the Accretion Region in EF Eridanus
	EF_ERI		240	1
019 -- Mauche -- Simultaneous Multiwavelength Observations of Dwarf Novae
	SS_CYG		300	1
	VW_HYI		100	1
020 -- Szkody -- A Multiwavelength Study of Accretion in V1159 Ori
	V1159_ORI	150	1
021 -- Lampton -- Reobservation of Two Diffuse Absorption Features
    Along the Ecliptic Plane
	DIFFUSE309	100	1
	DIFFUSE052	100	1
022 -- Simon -- DK UMa, A Star On the Ascent
	HD_82210	240	2
025 -- Linsky -- Probing Coronal Flare Energetics: Coordinated EUVE,
    XTE, and IUE Observations of Nearby Flare Stars
	EQ_PEG		70	1
	AU_MIC		70	1
027 -- Dempsey -- The First Multiwavelength, Multiple Layer Doppler
    Imaging of an Active Binary
	HD155555	85	2
028 -- Lallement -- Local Interstellar Cloud Ionization and Size of
    The Heliosphere
	WD0549+158	200	1
029 -- Guinan -- Probing the Dynamo for Stars With Shallow Convective
    Zones: The Young F0V Star 47 Cas
	47_CAS		180	1
030 -- Bloch -- Location, Spectroscopy, and Time Behavior of EUV
    Transients Detected With Alexis
	ALEXIS_Trans	100	1
032 -- Judge -- Consolidation and Verification of EUVE'S Lunar
    Observing Program
	MOON		40	1
033 -- Holberg -- Probing the Local ISM with Bright White Dwarfs
	SIRIUS_B	190	1
037 -- Siegmund -- A Multiwavelength Observation of the Gas in V471 Tauri
	V471_TAURI	100	1
	V471_TAURI	100	1
038 -- Provencal -- The Connection Between Hydrogen, the Interstellar
    Medium, and the DBV GD358
	GD358		50	2
039 -- Finley -- Moderate S/N Spectroscopy of Metal-Rich Hot DA White Dwarfs
	RE0457-280	155	2
	WD2309+105	155	2
041 -- Dupuis -- EUV Spectroscopy of Exotic White Dwarfs
	EUVEJ0512-006	200	2
	EUVEJ1746-706	200	2
042 -- Vennes -- Physical Parameters of White Dwarfs Paired with an
    Active Companion
	EUVEJ1925-565	120	1
	EUVEJ1629+780	120	1
044 -- Brown -- Activity on the Edge of Convection: The Atmosphere of
    DA White Dwarfs
	ALPHA_CAR	200	2
045 -- Ayres -- Gappers & Clumpers: Finale
	MU_VEL		250	2
047 -- Cassinelli -- An EUVE Study of the B Stars epsilon CMa and beta CMa
	EUVEJ0622-17.9	750	2
048 -- Hall -- Coordinated EUVE/GALILEO Observations of the Jupiter System
	JUPITER		50	1
	JUPITER		150	1
	JUPITER		50	1
	JUPITER		50	1
049 -- Jordan -- Probing the Absorption by Photoionization in Highly
    Magnetic White Dwarfs
	RE_J0317-853	300	1
050 -- Foster -- EUV Emission from Old Millisecond Pulsars
	PSR_J2124-3358	100	2
	PSR_J1024-0719	100	2
051 -- Rosen -- An EUV Study of the Accretion Mode Changes in the
    Polar, QS Tel
	QS_TEL		80	1
053 -- Barstow -- Testing the Theory of Radiative Levitation in DA
    White Dwarfs
	REJ2334-471	170	2
	HD74389B	215	2
054 -- Polidan -- Hidden Companions to Early Type Stars
	EUVE_J0729-388	160	2
055 -- Bruhweiler -- Ultra-High Ionization Species and Coronae of Hot
    White Dwarfs
	NGC_246		200	1
057 -- Bruhweiler -- Multifrequency and EUVE Observations of the
    Unusual Gamma-Ray Emitting Blazar, Mkn 421
	MKN_421		350	1
058 -- Mumma -- Continued Search for Neon and Helium in Comets
059 -- Dupree -- A Multiwaveband Study of AR Lac
	AR_LAC		120	2
061 -- Brickhouse -- Capella: Structure and Abundances
	CAPELLA		130	1
063 -- Leighly -- Coordinated EUVE And ASCA Observation of the
    Ultra-Soft Variable Narrow Line QSO TON S180
	TON_S_180	150	1
	TON_S_180	50	2
065 -- Marshall -- Multiwavelength Spectral Variability of PKS 2155-304
	PKS2155-304	80	1
	PKS2155-304	75	2
067 -- Brown -- Linking the Impulsive and Gradual Phases of RS CVN Flares
	HR1099		200	2
068 -- Anderson -- Target of Opportunity Reobservation of AG Draconis
069 -- Schwope -- An EUVE Key Project: Binary Accretion Studies Using
    the Unique Eclipsing Polar HU Aquarii
	HU_AQR		450	1
071 -- Silber -- Extreme Ultraviolet Observations of the Bright AM
    Herculis Type Cataclysmic Variable AR Ursa Majoris
	AR_UMa		100	1
073 -- Schmitt -- Does UV Ceti Suffer from the MAD Syndrome?
	UV_CETI		350	2
074 -- Fruscione -- EUV and X-Ray Variability in Seyfert Galaxies: A
    Study with Simultaneous EUVE and XTE Observations
	NGC4051		250	1
	NGC4051		80	2
075 -- Stringfellow -- A Search for Coronal Emission in the Lowest
    Mass Stars and the Rotation-Activity Relation for Spectral Types
    Later Than M8
	BRI0021-0214	200	1
	LHS2065		100	1
	LHS2924		100	2
	PC0025+0447	100	2

2.2 Public Data Release for 1 Feb 1996
        by Dr. Nahide Craig, CEA Scientist, ISO User Support Team

   The table below lists the GO observations that become public on 1
Feb 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 Feb 1996:

     PSR 0437-47      100    23 Oct - 26 Oct 1994    Pulsar   go0268
     PSR 0437-47      100    26 Oct - 30 Oct 1994    Pulsar   go0269
     PSR 0437-47      100    30 Oct - 02 Nov 1994    Pulsar   go0270
     PSR 0437-47      100    02 Nov - 06 Nov 1994    Pulsar   go0271
     PSR 0437-47      100    06 Nov - 09 Nov 1994    Pulsar   go0272
     PSR 0437-47       70    09 Nov - 12 Nov 1994    Pulsar   go0273


2.3 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. 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. 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

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