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ELECTRONIC NEWSLETTER OF THE EUVE OBSERVATORY
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Vol 5, No. 6 16 Jun 1995 ISSN 1065-3597
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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
follows:
1. EUVE Science News
1.1 Recent Science Highlights
1.2 User's Committee Meeting at GSFC
1.3 Newly Approved RAP Proposals
1.4 Abstracts of *Accepted* EUVE Papers
2. Science Operations News
2.1 CEA Director Appointed
2.2 Test of New Dithering Operation
2.3 Scanner C Anode Blanking Enabled
2.4 Correction to EUVE GO Data Products Guide
2.5 On-Line Access to EUVE
3. Testbed and Technology Transfer Highlights
To comment on or make suggestions for the EUVE electronic newsletter,
please send e-mail to ceanews@cea.berkeley.edu (Internet).
The EUVE observatory performed well throughout the month of May,
performing 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
===================================================================
MRK 421 UGC 6132 BLLac 25 Apr - 06 May 1995 ---
ALEXIS Transient -------- NOID 06 May - 07 May 1995 TOO
MRK 421 UGC 6132 BLLac 07 May - 15 May 1995 ---
Test -------- ---- 15 May - 15 May 1995 TS1
RE 1307+535 -------- CVAM 15 May - 17 May 1995 ---
1455-3330 -------- NeutSt 15 May - 17 May 1995 RAP
Cen X-4 V822 Cen LMXB 15 May - 17 May 1995 RAP
Moon -------- SolSys 17 May - 17 May 1995 ---
RE 1307+535 -------- CVAM 17 May - 25 May 1995 ---
1455-3330 -------- NeutSt 17 May - 25 May 1995 RAP
Cen X-4 V822 Cen LMXB 17 May - 25 May 1995 RAP
Virgo -------- SNR 25 May - 26 May 1995 ---
EUVE J1147+025 -------- NOID 26 May - 27 May 1995 ---
HZ 43 WD 1314+293 DAw 27 May - 27 May 1995 TS2
WGA J1319+30 -------- NOID 27 May - 27 May 1995 RAP
1304+310 -------- AGN 27 May - 27 May 1995 RAP
PG 1116+215 Ton 1388 QSO 27 May - 28 May 1995 ---
EUVE J1636-285 -------- NOID 28 May - 30 May 1995 ---
Jupiter -------- SolSys 30 May - 06 Jun 1995 ---
NGC 4051 UGC 7030 Seyf1 30 May - 06 Jun 1995 RAP
===================================================================
Key to Notes:
TOO = Target of Opportunity
TS1 = archimedes spiral "dithering" test
TS2 = scanner calibration test
RAP = simultaneous Right Angle Program (RAP) imaging observation
1. EUVE Science News
====================
1.1 Recent Science Highlights
-----------------------------
by Dr. Antonella Fruscione, EUVE Scientist
The nearby solar analogue and K dwarf binary alpha Cen AB is the
brightest coronal EUV source in the sky as viewed from earth. It is
extremely important because it contains two stars with well-known
parameters and solar-like coronal activity, and thus forms the best
observational link between solar and stellar coronae. However, the
stars are too close together (18 arcsec) to be completely resolved
by EUVE.
Nevertheless, a recent EUVE observation of Alpha Cen AB designed
to maximally separate the two components in the medium wavelength
spectroscopic imaging direction, has enabled CEA scientist Dr. J.J. Drake
to estimate the relative brightnesses of the two components in lines of
He II 304, Mg VII/IX and Fe from charge states IX-XVI. The stars are
approximately of equal brightness at temperatures up to log T ~ 6. At
higher temperatures Alpha Cen B is brighter than Alpha Cen A by about
a factor of two. This work now enables the coronae of the G and K stars
to be studied comparatively, providing the first opportunity to probe
the change in coronal structure in the spectral sequence G-K for stars
of solar-like coronal activity.
1.2 User's Committee Meeting at GSFC
------------------------------------
by Anne Miller, EGO Center Technical Writer
The EUVE User's Committee (UC) along with Deputy Project Scientist
Dr. Ron Oliversen and NASA Headquarters representative Dr. James Schombert
met at Goddard Space Flight Center (GSFC) on 7 June to discuss the EUVE
extended mission. UC Chairman Dr. Jay Holberg (University of Arizona),
and members Mr. Steve Howell (Planetary Sciences Institute) and Dr. Doyle
Hall (Johns Hopkins University) presented a detailed review of the CEA
EGO Center and Science Archive on-line services. Support was also expressed
for the idea of a permanently maintained archive of EUVE data. Additional
details will be discussed in next month's edition of this newsletter.
All participants in the Guest Observer (GO), Guest Investigator (GI),
Right Angle, and Archival Programs are encouraged to send their comments,
suggestions, and concerns to Dr. Holberg (holberg@vega.lpl.arizona.edu)
or to CEA (egoinfo@cea.berkeley.edu).
1.3 Newly Approved RAP Proposals
--------------------------------
by Brett A. Stroozas, ISO Manager
The EUVE Public RAP is a simple and convenient method for researchers
to acquire long-exposure EUV photometric data. As shown in the table
above, seven RAP targets were observed in May. CEA encourages all
interested researchers to submit RAP proposals! Proposing is quick and
easy -- just follow the simple directions provided on the CEA WWW site
(http://www.cea.berkeley.edu). For more information contact the EGO Center
(egoinfo@cea.berkeley.edu).
To date there have been 27 proposals submitted; 21 have been accepted
with six still under review. The table below lists the three proposals
approved in May. For each entry is given the name of the Principal
Investigator (PI), the priority assigned the proposed targets (1=high,
2=medium, 3=low), and the title of the proposal. Priorities are used to
resolve scheduling conflicts when more than one approved RAP target is
viewable at any one time.
------------------------------------------------------------------------
PI Priority Title
------------------------------------------------------------------------
Vidal-Madjar 2 Observation of Evaporating Comets Falling Towards
Beta Pictoris
Walter 2 EUVE Flux Limits for the Isolated Neutron Star
RXJ185635-3754
Barstow 2 A search for EUV Variability in the Magnetic White
Dwarf RE J0317-853
------------------------------------------------------------------------
1.4 Abstracts of *Accepted* EUVE Papers
---------------------------------------
Included below are abstracts of EUVE-related papers recently *accepted*
for publication. For those papers authored by CEA scientists, the EUVE
publication numbers are indicated. Unless otherwise noted, researchers may
obtain preprints of CEA papers by sending an e-mail request containing the
publication number(s) of interest to pub@cea.berkeley.edu.
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 archive@cea.berkeley.edu.
--------------------------------------------------------------
THE UNUSUAL UV SPECTRA OF EUV DISCOVERED AM HERCULIS STARS
A.E. Herzog, S.B. Howell, and K.O. Mason
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
During its EUV all-sky survey, the wide field camera (WFC) on the ROSAT
satellite discovered several new AM Herculis type stars. In this paper,
we present observations of RE0751+14, RE1149+28, RE1844-74, RE1938-46, and
RE2107-05. Using the International Ultraviolet Explorer (IUE), spectra were
obtained of these systems over a band pass of 1200-3400 angstroms. These
AM Her stars, discovered in the EUV, and faint at optical wavelengths, proved
to be bright UV emission line sources. The intensities of the individual
emission lines due to CIV, CII, NV, HeII, and SiIV are 1.5-3 times stronger
then usually seen. However, the equivalent width ratios of these same
emission lines are similar to those seen in typical AM Hers. Using additional
observations of these stars in the EUV, we compare the continuum flux of the
new AM Hers at optical, UV, and EUV wavelengths to previously studied AM Hers,
and discuss some of the implications of these data.
--------------------------------------------------------------
THE THREE DIMENSIONAL STRUCTURE OF EUV ACCRETION REGIONS OF AM HER STARS:
ANALYSIS OF EUVE LIGHT CURVES
M.M. Sirk and S.B. Howell
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
Using data from the Extreme Ultraviolet Explorer (EUVE) satellite we
construct high time resolution phased folded light curves for eight AM Her
Systems obtained by the Deep Survey and Scanner telescopes. All data are
in the Lexan/boron passband (67-178 A).
--------------------------------------------------------------
THE FIP EFFECT AND ELEMENT ABUNDANCE ANOMALIES IN LATE-TYPE STELLAR CORONAE
J.J. Drake, J.M. Laming, and K.G. Widing
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
We present an analysis of lines from species with high and low first
ionization potentials (FIP) in the Extreme Ultraviolet Explorer ( EUVE)
spectra of the dMe binary FK Aqr and of the G8 dwarf xi Boo A. This study
is a part of our continuing investigation of the "FIP effect" and element
abundance anomalies in late-type stellar coronae. Our earlier studies have
found that the FIP effect -- elements with a FIP < 10 eV (e.g., Fe, Mg, Si,
Ca) are observed to be enhanced relative to those with FIP > 10 eV (e.g., O,
Ne, S) in the solar corona by factors of 3-10 with respect to the photosphere
-- is also present in the coronae of alpha Cen (G2 V + K0 V) and epsilon Eri
(K2 V), but apparently not in the corona of Procyon (F5 IV). Coronal
abundance anomalies from ASCA studies of more active stars have also been
reported in the literature recently; however, these abundance anomalies are
generally opposite to the solar FIP effect, inasmuch as depletions rather
than enhancements of heavy elements are found. In this context, the very
active dMe binary FK Aqr and the active dwarf xi Boo A are quite interesting.
We will discuss the results in the context of what is currently known concerning
element abundance anomalies in stellar coronae. The detection or otherwise of
a FIP effect in FK Aqr also has a bearing on the possible origin of galactic
cosmic rays. This work is supported by NASA contract NAS5-30180.
----------------------------------------------------------------------------
MODELING OF EUVE OBSERVATIONS OF THE IO PLASMA TORUS
R. Lieu, N. Thomas, D.E. Innes, G.R. Gladstone, D.T. Hall, and F. Herbert
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
Jupiter is surrounded by a torus of sulphur and oxygen ions that
have been injected into the magnetosphere by the Galilean satellite, Io.
Although ground-based observations at visible wavelengths have been used
to investigate torus phenomena for 20 years, the principal radiative
losses occur in the extreme ultraviolet (EUV). The Voyager UVS instruments
provided low resolution spectra in this wavelength range during fly-bys
in 1979. The Extreme Ultraviolet Explorer (EUVE) spacecraft first observed
the torus in 1993 giving two-dimensional spatially resolved spectra. The
data showed a strong asymmetry (Hall et al., ApJ, 426, L51, 1994) between
the dawn and dusk sides of the planet. A series of observations were
conducted in 1994 to coincide with the impact of the fragments of comet
Shoemaker-Levy 9 with Jupiter. The data suggest that the torus may have
been affected by dust particles entering the system. In this poster, we
present data from the observing run and make an initial interpretation of
the data using a semi-empirical, three-dimensional simulation of the torus.
Variations of the order of 10% in the electron temperature in the torus,
caused by electron-dust collisions, may have been responsible for the
observed phenomena. This work has been supported by NASA contract NAS5-30180.
----------------------------------------------------------------------------
EUVE OBSERVATIONS OF THE SEYFERT GALAXY MRK 279
C.-Y. Hwang and S. Bowyer
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
We present extreme ultraviolet (EUV) data on the Seyfert 1 galaxy MRK 279.
The total EUV flux from this object exceeds the the extrapolation of the
ROSAT power-law fit by an order of magnitude. The spectroscopic data show
that most of the excess count rate is due to emission features between 80-100
Angstroms. The total EUV count rates of the source changed by 50% on a time
scale of days. We discuss mechanisms that might produce these emission
features. The constraints upon various active galactic nuclei models are
also addressed. This work has been supported by NASA contract NAS5-30180.
----------------------------------------------------------------------------
A SPECTROSCOPIC SURVEY IN THE EUV OF THE "COOLEST" HOT DA STARS
J. Dupuis, S. Vennes, and A.K. Pradhan
IAU Colloquium #152: Astrophysics in the Extreme Ultraviolet, 27-30 March 1995
We present an analysis of the extreme ultraviolet (EUV) spectroscopy of a
large sample of DA white dwarfs observed by the Extreme Ultraviolet Explorer
(EUVE), the spectra of which are available on the EUVE public archive. We
have selected a sample of white dwarfs cooler than about 50,000 K and with
extremely low metal abundances. The goal of the study is to determine the
fundamental atmospheric parameters, namely effective temperature and log g,
of these stars by fitting their continua with synthetic spectra computed from
pure hydrogen model atmospheres. We will also put lower limits on the
thickness of the hydrogen layers by fitting H/He stratified models. The
question of the presence (or absence) of metals is explored by putting lower
limits on C, N, O, and Fe abundances using local thermodynamic equilibrium
model atmospheres of DA stars with metal opacities computed from Opacity
Project data. Comparisons are made with predictions of radiative acceleration
calculations, and implications on spectral evolution of hot white dwarfs is
discussed. This work has been supported by NASA contract NAS5-30180 and
NASA grants NAG5-2626 and NAG-2405.
----------------------------------------------------------------------------
AN OPTICAL AND FAR UV STUDY OF THE FIELD OF THE SOURCE EUVE J1027+323
R. Genova, S. Bowyer, S. Vennes, R. Lieu, J.P. Henry, and I. Gioia
To appear in Astronomical Journal. [CEA publication #654]
We have carried out optical and Far UV studies of the field around
the EUV source EUVE J1027+323. We find two objects which contribute
to this flux which are spatially unresolvable with EUVE. One is a
non-cataloged QSO and one is a hidden hot white dwarf. The relative
contributions of each of these to the total EUV flux is uncertain;
reasonable scenarios ascribe the majority of the flux to the white dwarf.
--------------------------------------------------------------
THE EUVE OPTICAL IDENTIFICATION CAMPAIGN II: LATE-TYPE AND WHITE DWARF STARS
N. Craig, A. Fruscione, J. Dupuis, M. Mathioudakis, J.J. Drake, M. Abbott,
C. A. Christian, R. Green, T. Boroson, and S.B. Howell
To appear in Astronomical Journal. [CEA publication #655]
We present optical identifications of nine previously unidentified extreme
ultraviolet (EUV) sources discovered during the Extreme Ultraviolet Explorer
(EUVE) satellite surveys. The all-sky survey detected four of the sources
and the more sensitive deep survey detected the other five sources. Three
of the four all-sky survey sources, EUVE J1918+599, EUVE J2249+585, and
EUVE J2329+414, are listed in present catalogs as having possible associations
with optical counterparts but without spectral class. The first two of these
sources are hot DA white dwarfs showing an optical spectrum with broad Balmer
lines. The source EUVE J2329+414 is listed as having a possible association
with an unclassified M star. We show that a pair of dMe stars are actually
optical counterparts located within the error circle of the EUVE source
position. The EUVE 2114+503 remains unidentified even though all the possible
candidates have been studied. Based on the count rates we predict a fainter
white dwarf or a cataclysmic variable counterpart for this candidate. All
five sources discovered with the EUVE deep survey, EUVE J0318+184, EUVE
J0419+217, EUVE J2053-175, EUVE J2056-171 and EUVE J2233-096, have been
identified as late-type stars. The spectral classes, distances, visual
magnitudes, and estimated hydrogen column densities for these EUVE sources
are presented.
--------------------------------------------------------------
EXTREME ULTRAVIOLET EMISSION FROM THE MILLISECOND PULSAR J0437-4715
J. Edelstein, R.S. Foster, and S. Bowyer
To appear in Astrophysical Journal. [CEA publication #656]
We report the first detection of extreme ultraviolet (EUV) emission
from a millisecond pulsar. The EUV flux is not consistent with standard
models used to describe the X-ray flux from this object. The size of an
EUV-emitting hot polar cap disagrees with the size derived from the X-ray
data by a factor from ~3 to 25. However, a blackbody with a temperature
of ~5.7E5 K and an area of ~3 km^2 can explain both EUV and X-ray observations
below 0.4 keV. Alternatively, if the EUV emission is independent of the X-ray
emission and is due entirely to a thermalized neutron star surface, we place a
limit on the surface temperature of 1.6 - 4.0E5 K. Surface reheating would
be required to explain this temperature according to standard neutron star
cooling models because of the pulsar's 5 Gyr age. The EUV data rule out
reheating by crust-core friction, accretion from the interstellar medium,
accretion from the white dwarf companion, and heating by a particle-wind
generated nebula. We use models of pulsar reheating by magnetic monopole
catalysis of nucleon decay to establish an upper limit to the flux of
monopoles in the Galaxy from 1 to 3 orders of magnitude below existing limits.
--------------------------------------------------------------
DISCOVERY OF A WHITE DWARF COMPANION (EUVE J0254-053) TO THE KO IV
STAR HD18131
S. Vennes, M. Mathioudakis, J.G. Doyle, and J.R. Thorstensen
To appear in Astronomy & Astrophysics Letters. [CEA publication #657]
New ultraviolet (UV) observations of late-type stars detected in the
Extreme Ultraviolet Explorer (EUVE) all-sky survey revealed an unsuspected
white dwarf companion to the K0 star HD18131. The International Ultraviolet
Explorer (IUE) spectrum show a composite of a white dwarf and a late-type
star. The white dwarf dominates the emission below 2000 A while the K0 star
prevails at longer wavelengths. A model atmosphere analysis of the new
ultraviolet spectrophotometry and of the extreme ultraviolet (EUV) photometry
reveals a hot, hydrogen-rich (DA) white dwarf (T_eff ~ 30,000 K) that is the
most likely source of the EUV emission (EUVE J0254-053). We estimate a
distance to the white dwarf of 70-90 pc. The K0 star shows a modest level
of chromospheric activity with the detection of Mg ii h and k emission in
the IUE spectrum. Optical spectroscopy revealed that the K0 star is a
subgiant (K0 IV). The star is located at a distance of ~70 pc, consistent
with the estimated distance of the white dwarf. Therefore, it most likely
constitutes a physical pair with the white dwarf. Until results of a radial
velocity study are made available we cannot establish whether the pair is
wide or close. In earlier works the strong EUV emission was attributed to
the K0 star; however, our multiwavelength observations show the white dwarf
as the most likely source. This discovery has important implications for
the EUV white dwarf population survey and, in particular, for the binary
frequency.
--------------------------------------------------------------
2. Science Operations News
==========================
2.1 CEA Director Appointed
--------------------------
Dr. Roger Malina has been appointed Director of the Space Sciences
Laboratory's Center for EUV Astrophysics (SSL/CEA) at the University
of California, Berkeley, through July 1997.
2.2 Test of New Dithering Operation
-----------------------------------
by Anne Miller, EGO Center Technical Writer
On 6 June a test observation of the bright white dwarf continuum source
HZ 43 was conducted in order to evaluate a new pointing pattern for dithered
observations. The new pattern is an Archimedes Spiral in which pointing
positions are generated according to the rule R = theta instead of by choosing
random spots on a grid of locations. The spiral is started 20 arc seconds
from the detector center to avoid the Deep Survey dead spot. Analysis
of the test results in the next few weeks will determine whether the new
pattern is at least equivalent to the current random pointing dithering
mode for eliminating the detector fixed pattern noise. The use of the
Archimedes Spiral method of dithering fits in well with CEA's efforts to
streamline and automate operations as it is a much simpler operation and
will greatly reduce the science planning efforts for dithered observations.
2.3 Scanner C Anode Blanking Enabled
------------------------------------
A new software patch was loaded that blanks out in telemetry events from
the tin filter quadrants of the long wavelength scanner imaging telescope
(Scanner C). This anode blanking will relieve the adverse affects of the
high number of background events in the tin quadrants. Because the science
payload is now operating in WSZ mode, there are fewer photon slots available
in telemetry than when in XY mode. Therefore, without anode blanking the
primbsching algorithm (which allocates telemetry slots among the different
detectors) may cause deep survey/spectrometer (DS/S) photon events to be
excluded from telemetry because of the high background rates in the tin
quadrants. The anode blanking changes the primbsching algorithm so that it
stops allocating telemetry slots to events from the Scanner C tin quadrants.
The standard operating payload configuration is now WSZ mode with anode
blanking enabled on the Scanner C tin quadrants. If another configuration
is required (e.g., for a RAP target), the science planner will ensure that
the necessary adjustments are made.
2.4 Correction to EUVE GO Data Products Guide
---------------------------------------------
There is an error in section 4.3.2 -- "Earth Blockage" -- of the EGO
Center Data Products Guide (DPG), version 1.5. The section describes the
creation of filters during EGO Center nominal data reduction to remove
earth-blocked data from the spectral images. The parameter for the minimum
altitude through the atmosphere at which the line of site has unacceptable
EUV absorption should be 450 km, instead of 200 km. The equation on
page 4-8 describing the calculation of the maximum DS/S zenith angle
is correct. 450 km is the atmospheric altitude used in batch processing,
with the further assumption that the satellite orbit is 516 km above
the earth's surface. This leads to a limiting DSSZEN angle of 97.93 degrees.
The information in the DPG illustrates the EGO Center processing of
GO data, which is quite conservative in that it filters out all data from
lines of site <= 450 km above the earth's surface. GO's may choose to create
an alternative earth blockage filter for any limiting altitude they feel
is more appropriate.
To recreate the earth blockage filter for a different altitude (A),
GO's should use both the angle from the DS/S line of site to the satellite
zenith, DSSZEN, and the satellite height, SatHt, in the table produced
by the task backmon, which is extracted from the aspect and ephemeris
data in telemetry. The chosen line-of-sight altitude, along with the
height (H) will produce a correct limiting angle for that observation
when used in the formula in the DPG.
The angle will vary within some small range, depending on the range
of satellite altitudes, but this variation can be safely overlooked. A
specific example will be published in the upcoming EGO Center Software
User's Guide, version 1.5.
2.5 On-Line Access to EUVE
--------------------------
Listed below are the various methods for on-line access to EUVE:
o CEA World Wide Web (WWW) URL:
http://www.cea.berkeley.edu/ (for those with WWW browsers)
telnet www.cea.berkeley.edu 200 (for those without WWW browsers)
o anonymous FTP/gopher: ftp.cea.berkeley.edu
o EUVE Electronic Newsletters (past issues available via CEA WWW):
Subscriptions: mail majordomo@cea.berkeley.edu ("subscribe euvenews")
Post message to all subscribers: mail euvenews@cea.berkeley.edu
o For additional information contact the Archive:
The EUVE Science Archive
Center for EUV Astrophysics
2150 Kittredge St.
Berkeley, CA 94720-5030
510-642-3032 (voice) or 510-643-5660 (fax)
archive@cea.berkeley.edu
3. Testbed and Technology Transfer Highlights
=============================================
by Tom Morgan, Test-Bed Manager
In collaboration with CEA, NASA's Ames Research Center (ARC) and GSFC
will sign a Memorandum of Understanding this month to develop the EUVE Virtual
Environment(EVE). EVE will address the visualization problem for complex
science planning and engineering anomaly resolution. EVE will allow
instantaneous real-time visualization of the health and safety of the
observatory, as well as predictive capability for new spacecraft attitudes.
EUVE constraints will be modeled and represented by a 3-d model of the
observatory. A VRML client will be added for WWW access.
CEA student Navid Sabbaghi is spending his summer at ARC in order to tailor
the Virtual Environment Vehicle Interface (VEVI) to meet EUVE requirements
for the EVE project. Navid Sabbaghi is a second year Electrical Engineering
and Computer Science major at the University of California and plans to
pursue graduate level research in augmented intelligence software.
The "alpha" delivery of VEVI to CEA is scheduled for late August 95. VEVI
is based on the commercial software libraries offered by World Tool Kit, Sense8
Corp. EVE will be developed from the VEVI alpha and EUVE-specific functionality
(i.e., thermal constraint visualization).
---------------------------------------------------------------------------
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
C.S. Bowyer. EUVE Science and Technology Manager: Dr. C.A. Christian.
ISO Manager and Newsletter Editor: B.A. Stroozas. Funded by NASA contracts
NAS5-30180 and NAS5-29298. Send newsletter correspondence to:
ceanews@cea.berkeley.edu. 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
Guest Observer Program is available from: Dr. Y. Kondo, Mail Code 684,
GSFC, Greenbelt, MD 20771 at (301) 286-6247 or e-mail to
euve@stars.span.nasa.gov.
END-----------EUVE------------ELECTRONIC---------------NEWS-------------END
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