Present
Position: Visiting
Senior Research Scientist, Department of Astronomy, University of Maryland,
College Park, MD.
Education: B.S., Physics, 1961, Queens College, City
University of New York, Flushing, N.Y. Ph.D., Physics, 1966, University of
Rochester, Rochester, N.Y.
Experience:
NRC/NRL
Post-Doctoral Res. Assoc. in Lab. for Cosmic-Ray Physics, 1966 - 1968.
Research
Physicist in NRL/Laboratory for Cosmic-Ray Physics, 1968 - 1973.
Astrophysicist
in Space Science Division, NRL, 1973 - 2005.
Senior
Staff Scientist, Astrophysics Div., NASA Headquarters, May 1989 - May 1991.
Fellowships
and awards:
Phi Beta
Kappa (Queens College)
NRL-Sigma Xi
Pure Science Award 1992
Bruno Rossi
Prize HEAD/American Astronomical Society 1992
Fellow
American Physical Society (1997)
Fellow
American Astronomical Society (2020)
Society
Memberships:
American
Physical Society (Astrophysics Division); American Astronomical Society (HEAD,
SPD); American Geophysical Union; Sigma Xi,AAAS
Gerald Share started his research career at the University of Rochester
under the guidance of his thesis adviser, Prof. Everett Hafner. His thesis
covered the development, calibration, flight and analysis of a balloon-borne
experiment to make pioneering studies of gamma radiation above 10 MeV in the
upper atmosphere. Only upper limits were obtained on radiation from celestial
sources.
After receiving his PhD in 1967, he accepted a NAS/NRC post-doctoral
appointment in the Laboratory for Cosmic Ray Physics under the direction of Dr.
Maurice Shapiro. He worked with Mr. Nathan Seeman, Dr. Robert Kinzer, and Mr.
Carl Noggle to develop a balloon-borne experiment to
detect gamma-radiation above 10 MeV with ~2 angular resolution and 20% energy
resolution. The instrument incorporated a stack of nuclear emulsions and used
gas proportional, plastic scintillation and Cerenkov detectors, and a wide gap
spark chamber. This array enabled electron positron pairs to be tracked back
into the emulsion where the precision measurements were made. The experiment
was first flown in 1969 and observed the Crab Nebula. It provided the first
evidence for the detection of the pulsar at gamma-ray energies. The experiment
also was flown from the Southern Hemisphere in 1971 over Argentina and in 1975
over Brazil in order to view the Galactic Center region and to reduce the
background from the atmosphere. These observations provided measurements of
atmospheric background and limits on the celestial diffuse radiation, and
revealed a narrow band of gamma-ray emission along the Galactic Plane.
In 1974 Dr. Share and Dr. Kinzer transferred into the Space Science Division
and began working in the Hard X-ray and Gamma-ray Branch headed by Dr. James Kurfess. He worked on early balloon data obtained by Dr. Kurfess and established the phase of hard X-rays with other
pulsed radiation from the Crab. Dr. Share then began studies of the newly
discovered cosmic gamma-ray bursts using data from a solar hard X-ray
spectrometer on OSO-6. These measurements and those made in a joint study with
Dr. Sharad Kane using data from OGO-5 demonstrated that these gamma-ray bursts
were also detected at energies down to 10 keV.
He also worked with Dr. Kurfess and others in the
Branch on proposals for a gamma-ray detectors on
NASA's Solar Maximum Mission (SMM) and Compton Gamma Ray Observatory. As part
of this work he established the ability to separate
neutron and gamma-ray emission detected by NaI. With
the launch of NASA's first High Energy Astronomy Observatory in 1977, Dr. Share
became involved in observations of soft X-rays with the NRL's large area X-ray
instrument. This work led to the identification of GX339-4 as a black hole
candidate and to the realization that many X-ray sources were associated with
B-type stars with emission lines.
As a result of the Branch's efforts to build a gamma-ray spectrometer on SMM,
Dr. Share became responsible for collaborative studies with the University of
New Hampshire using their experiment. This excellent experiment, developed by
Prof. Edward Chupp and Dr. David Forrest, operated
from the 1980 to 1989 and made several discoveries in celestial and solar
physics. It was made up of seven 3 in. diam. x 3 in. NaI
detectors, well stabilized and calibrated. Dr. Share focused his early efforts
on the study of celestial radiation and cosmic gamma-ray bursts. Working with
Drs. Steve Matz and Pat Nolan, Dr. Share showed that gamma-ray burst spectra
typically extended up to energies above 1 MeV and did not exhibit any lines.
One of the bursts was observed up to 100 MeV. The lack of emission lines
conflicted with measurements made by the Soviet Konus
experiments that suggested the presence of broad lines that could be associated
with positron annihilation. A later study by Messina and Share set emission
line limits in bursts covering the full 9-year mission and the full energy
range of the instrument. In the years since those measurements no emission
lines have been detected by recently flown instruments.
Drs. Kinzer and Share developed techniques for using the solar pointed SMM
spectrometer for detecting lines and continua from celestial sources. This used
various methods for eliminating backgrounds and depended on the slow scan of
the detector along the ecliptic plane. As a result of these efforts SMM
confirmed the discovery by HEAO-3 of a diffuse glow in the 26Al line
along the galactic plane. This emission can come from supernovae, novae, Wolf-Rayet and other giant stars. Dr. Share next turned his
attention to the study of the galactic positron-electron annihilation line. At
that time it was believed to be both variable and
likely to be associated with a discrete source, possibly a black hole near the
galactic center. The SMM observations showed that annihilation source was
relatively constant over an eight-year time scale and was likely due to diffuse
galactic emission from several sources including supernovae, novae, and other
positron emitters. Dr. Barry Geldzahler worked with
Dr. Share on SMM observations of SS433. This source was reported by HEAO-3 to
emit red and blue shifted emission lines. SMM set upper limits on these lines
that were inconsistent with the HEAO-3 observations. The HEAO-3 measurements
were subsequently retracted.
In 1987 the brightest and nearest supernova to occur in 500 years occurred in
the Large Magellanic Cloud. This gave scientists the
opportunity to detect the gamma-ray lines from the Ni-Co-Fe decay chain that
would definitively show that nucleo-synthesis of
these elements occurred in supernovae. Because it was a type II supernova, the
lines were not expected to be detectable for about 2 years. However, hard
X-rays were detected from the supernova by the MIR detectors only 9 months
after the explosion. Dr. Steve Matz worked with Dr. Share and reported the
first detection of gamma-ray lines about a month later. Dr. Mark Leising continued this work with Dr. Share and showed the
full nuclear line spectrum and how it evolved in time. This early detection of
line and continuum indicated that radioactive material in the nebula was not
uniformly layered. Drs. Matz and Share also set constraining limits on
gamma-ray lines from a nearby type I supernova in Centaurus A, while Leising and Share set limits on nucleosynthetic lines from 22Na,
44Ti, and 60Fe from novae.
Dr. Michael Harris then worked with Dr. Share to make additional celestial
observations. He constructed the first gamma-ray spectrum of radiation from the
galactic plane and set limits on variable emission lines from a variety of
celestial sources. None of these lines have subsequently been detected. Harris
and Share then set upper limits on the 7Be and neutron capture lines
from compact celestial sources. They also set upper limits on galactic
de-excitation lines from 12C and 16O. This study also did
not confirm the reported broad emission lines from Orion based on measurements
from the Compton Gamma-Ray Observatory Comptel
experiment. A subsequent search from these lines was performed by Murphy and
Share using OSSE data and set even more constraining limits. The Comptel investigators subsequently determined that the
Orion observation was spurious. Harris and Share completed the SMM celestial
studies by showing that there is no new class of cosmic gamma-ray bursts that
are primarily visible at energies above 1 MeV (limited to bursts with duration
>2 s).
Early in the SMM mission, Dr. Erich Rieger discovered transient annihilation
line events and other high-energy transients. Working with Dr. Keith Marlowe,
Dr. Share identified the source of these events as emissions from orbiting
Soviet nuclear reactors. The annihilation line was detected by SMM when it
passed through clouds of positrons stored in the earth's magnetic field. These
events could be detected even while the SMM and reactor borne satellites were
separated by several thousand km. SMM also recorded the gamma-ray spectrum
emitted by the reactors when they passed within about 800 km and identified
several emission features.
In the early 1990's, Dr. Share focused his research on the study of nuclear
line radiation from solar flares. That started a long term
collaboration with Dr. Ron Murphy. This
study utilized data from both SMM and the Compton Observatory OSSE experiments.
Along with Tom Vestrand, they published a catalog of
high-energy flares observed by the SMM spectrometer. Using 19 of these flares
with strong nuclear line emission, Share and Murphy made some key spectral
measurements that produced some fundamental discoveries about particle
acceleration, transport and energetics in flares and the ambient abundance of
the corona and chromosphere. The framework for these discoveries was developed
in the theories and models of Drs. Reuven Ramaty,
Benz Kozlovsky, Natalie Mandzhavidze
and Ron Murphy.
These discoveries include: 1) enhancement in the concentration of low FIP
elements where accelerated particles interact, 2) a new line ratio for deriving
the spectra of accelerated particles < 10 MeV, 3) energies in accelerated
ions that exceed those in electrons for some flares, 4) a highly variable ion
to electron ratio during flares, 5) concentration of 3He in
flare-accelerated particles enhanced by a factor of >1000 over its photospheric value, 6) an accelerated alpha/p ratio >
0.1 in several flares and evidence for high ambient 4He in some
flares, 7) measurements of the positronium fraction and a temperature-broadened
511 keV line width, 8) new information on the directionality of electrons,
protons, and heavy ions and/or on the homogeneity of the interaction region,
and 9) the spectrum of broadened gamma-ray lines emitted by accelerated heavy
ions that indicates Fe enhancements consistent with those observed in solar
energetic particles.
Dr. Share continued his solar flare research using data from NASA’s RHESSI satellite launched in 2002. One of the most exciting findings of
this recent research was the observation of a rapid change in the width of the
positron-electron annihilation line during the 2003 October 28 solar
flare. In the first 10 min of the RHESSI
observation the line had a width consistent with production in a medium at
temperatures >105 K. In two minutes time
the width changed suggesting evolution to a standard active region atmosphere.
Dr. Share retired from the Naval Research Laboratory in July 2005 and
has continued his solar research as a Visiting Senior Research Scientist in the
Astronomy Department of the University of Maryland.
With the launch of the Fermi gamma-ray satellite, Dr. Share organized a
solar science team to optimize the analysis of the Large Area Telescope (LAT)
and Gamma Burst Monitor (GBM) for studying solar quiescent and flare
emission. He focused his research
activities on the study of what is called late phase gamma-ray emission (LPGRE). This emission is primarily observed at
energies above 100 MeV and has a spectrum consistent with gamma-rays from
neutral pion decays. These pions are produced by interaction of >300 MeV gamma rays
in the solar atmosphere. Because the
time profile of this emission is distinct, and typically delayed, from the
flare hard X-ray and nuclear line gamma-ray emission, it is likely that is originates
in a different acceleration process than the flare. The evidence suggests that the emission comes
from protons accelerated by the shock preceding the coronal mass ejection (CME)
which find magnetic field lines returning to the Sun and impact the Sun. This work resulted in the publication of a detailed
catalog and analysis of 30 solar LPGRE events in 2018.
Since 2019 Dr. Share has returned to his earlier solar flare nuclear
gamma-ray studies. Working with Dr. Ron
Murphy at NRL, he has made detailed spectroscopic and timing analyses of 19 flares
observed by SMM from 1980 to 1989 and from a flare observed in 2002 by
RHESSI. These spectroscopic studies enable
the determination of the ambient elemental abundance in the solar atmosphere
where the accelerated ions interact, as well as the composition of these ions.