B. J. Teegarden

Goddard Space Flight Center

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T. L. Cline

Goddard Space Flight Center

J. Tueller

Goddard Space Flight Center

S. D. Barthelmy

Goddard Space Flight Center

G. Védrenne

Nord University

N. Gehrels

Goddard Space Flight Center

J. L. Matteson

University of California, San Diego

D. M. Palmer

Los Alamos National Laboratory

W. S. Pačiesas

Universities Space Research Association

M. Leventhal

University of California, Riverside

K. Hurley

University of California, Berkeley

Cooperative Institutions

Goddard Space Flight Center

138

Centre National de la Recherche Scientifique

Max Planck Institute for Extraterrestrial Physics

University of California, Berkeley

University of California, Santa Cruz

Marshall Space Flight Center

University of Maryland, College Park

Commissariat à l'Énergie Atomique et aux Énergies Alternatives

Los Alamos National Laboratory

Deleted Institution

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Interplanetary Mev electrons of Jovian origin

Journal of Geophysical Research Atmospheres (1974)

B. J. Teegarden F. B. McDonald J. H. Trainor W. R. Webber E. C. Roelof

In this paper we report observations of low energy (0.2-8 MeV) electron increases observed in interplanetary space on Pioneer 10 as it approached within 1 AU of Jupiter.These discrete bursts or increases were typically several hundred times the normal quiet-time electron flux, and became much more frequent as one approached Jupiter resulting in the quasi-continuous presence of large fluxes of these electrons in interplanetary space.In view of the likely origin of these electrons at Jupiter, and the similarity of these increases to quiet-time electron increases previously observed at earth we have re-examined the temporal presence of the quiet-time increases.It is found that these increases have a 13 month periodicity indicating a Jovian origin for the events near the earth as well.It is noted that the integrated flux from quiet-time increase electrons at 1 AU is comparable to the integrated ambient electron flux itself.In addition, the spectrum of electrons observed in Jupiter's m4gnetosphere, on Pioneer 10 in interplanetary space near Jupiter, for the quiet-time increases near the earth, and for the ambient electron spectrum are all remarkably similar.These two lines of evidetce suggest the possibility that Jupiter could be the source of most of the ambient electrons at low energies.At the same time it is difficult to understand how Jovian electrons could be distributed uniformly throughout the inner solar system so as to produce the relatively constant quiet-time spectrum.At this time it is not possible to decide between a galactic knock-on origin coupled with a small residual solar modulation or a Jovian origin for the ambient electron intensity in the 0.2-40 MeV range. //

Jupiter (rocket family)

Interplanetary medium

10.1029/ja079i025p03615

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Citations (135)

Frequency of fast, narrow gamma-ray bursts and burst classification

AIP conference proceedings (1984)

J. P. Norris T. Cline U. D. Desai B. J. Teegarden

Evidence from the Vela satellites 1 that very brief, ∼0.1 s, gamma‐ray bursts constitute a class distinct from the longer, highly structured bursts has been strengthened by the results of the Venera 11 and 12 KONUS experiments 2. The Goddard ISEE‐3 Gamma‐Ray Burst Spectrometer, utilizing a trigger criterion which is more likely to be independent of duration than previous experiments, has detected a sample of events which enhances this bimodal distribution. The ISEE‐3 result is corroborated by an increase in the frequency of detection of short bursts in the KONUS 13/14 database over KONUS 11/12, an effect attributable to the use of a shorter trigger integration time in the later experiments. Considerations such as repeating bursters complicate a simple dichotomous classification of gamma‐ray bursts.

Vela

Sample (material)

10.1063/1.34542

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The search for gamma-ray burst spectral features in the Compton GRO BATSE data

AIP conference proceedings (1994)

D. M. Palmer B. J. Teegarden Bradley E. Schaefer T. L. Cline D. L. Band

The Spectroscopy Detectors (SDs) of the Burst and Transient Source Experiment (BATSE) on the Compton Gamma Ray Observatory (GRO) have seen no convincing line features in Gamma‐Ray Burst (GRB) data, in contrast to expectations based on results from other instruments. In this paper we discuss the search for lines in the SD data. The search has examined 148 bursts, of which ∼17 were intense enough that lines like those seen by the Ginga satellite would have been visible between ∼20 and ∼100 keV. Crude calculations show that the Ginga and BATSE results are consistent at the ∼3–13% level, depending on the definition of consistency.

10.1063/1.45799

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X-Ray and Optical Observations of the November 19, 1978 Gamma-Ray Burst Source Region

Springer eBooks (1981)

G. Pizzichini J. Danziger P. Grosbøl M. Tarenghi T. L. Cline

Intensity

10.1007/978-94-010-9949-3_72

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Citations (7)

Solar response of the BATSE instrument on the gamma-ray observatory

G. J. Fishman C. A. Meegan T. A. Parnell Robert Wilson W. S. Pačiesas

The Burst and Transient Source Experiment (BATSE) on board the gamma ray observatory (GRO) aims at comprehensive observations of time profiles, spectra, and locations of high-energy transient sources. The mysterious cosmic gamma ray bursts provided the main motivation for the observations, but BATSE will make excellent observations of many classes of sources, and in particular solar flares. The solar response of BATSE, as inferred from its design parameters, is analyzed for two purposes: the optimization of the solar observations themselves, and the characterization of the solar effects on ordinary nonsolar observations.

Solar flare

Transient (computer programming)

Source

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Observing Gamma-Ray Bursts with the INTEGRAL Spectrometer SPI

G. K. Skinner P. Connell J. E. Naya H. Seifert B. J. Teegarden

The spectrometer for INTEGRAL (SPI) is a germanium spectrometer with a wide field of view and will provide the International Gamma Ray Astrophysics Laboratory (INTEGRAL) mission with the opportunity of studying gamma ray bursts. Simulations carried out to assess the response of the instrument using data from real burst data as input are reported on. It is shown that, despite the angular resolution of 3 deg, it is possible to locate the direction of bursts with an accuracy of a few arcmin, while offering the high spectral resolution of the germanium detectors. It is remarked that the SPI field of view is similar to the size of the halo of bursts expected around M 31 on galactic models. The detectability of bursts with such a halo is discussed.

Spectral resolution

Source

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Neutron stars as sources of gamma-ray bursts: Constraints from X-ray observations of source locations

G. Pizzichini T. L. Cline U. D. Desai B. J. Teegarden Kevin Hurley

Results for three burst locations observed with the imaging proportional counter of the Einstein Observatory are given. The observations are used to determine temperature and accretion constraints for the burst source.

Einstein Telescope

Accretion disc

Source

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Observations of the galactic center with the GSFC Low-Energy Gamma-Ray Spectrometer: Preliminary results

AIP conference proceedings (1982)

W. S. Pačiesas T. Cline B. J. Teegarden J. Tueller P. Durouchoux

The GSFC Low‐Energy Gamma‐Ray Spectrometer observed the galactic center on 20 November, 1981, during a balloon flight from Alice Springs, Australia. The positron annihilation line at 511 keV showed no excess over background when the galactic center was in the field‐of‐view; the inferred upper limit to the intensity of such a feature is 1.2±10−3 photons/cm2−s (95 percent confidence). Continuum emission was observed between 70 keV and 1 MeV.

Center (category theory)

Gamma ray spectrometer

10.1063/1.33502

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Performance of an INTEGRAL spectrometer model

ESASP (1997)

P. Jean J. E. Naya P. von Ballmoos G. Védrenne B. J. Teegarden

Model calculations for the INTEGRAL spectrometer (SPI) onboard the future INTErnational Gamma Ray Astrophysics Laboratory (INTEGAL) are presented, where the sensitivity for narrow lines is based on estimates of the background level and the detection efficiency. The instrumental background rates are explained as the sum of various components that depend on the cosmic ray intensity and the spectrometer characteristics, such as the mass distribution around the Ge detectors, the passive material, the characteristics of the detector system and the background reduction techniques. Extended background calculations were performed with Monte Carlo simulations and using semi-empirical and calculated neutron and proton cross sections. In order to improve the INTEGRAL spectrometer sensitivity, several designs and background reduction techniques were compared for an instrument with a fixed detector volume.

Source

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<title>BASIS mission concept for gamma-ray burst imaging and spectroscopy</title>

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (1996)

N. Gehrels B. J. Teegarden L. Barbier S. D. Barthelmy Lyle M. Bartlett

We are studying a gamma-ray burst mission concept called burst arcsecond imaging and spectroscopy (BASIS) as part of NASA's new mission concepts for astrophysics program. The scientific objectives are to accurately locate bursts, determine their distance scale, and measure the physical characteristics of the emission region. Arcsecond burst positions (angular resolution approximately 30 arcsec, source positions approximately 3 arcsec) will be obtained for approximately 100 bursts per year using the 10 - 100 keV emission. This will allow the first deep, unconfused counterpart searches at other wavelengths. The key technological breakthrough that makes such measurements possible is the development of CdZnTe room-temperature semiconductor detectors with fine (approximately 100 micron) spatial resolution. Fine spectroscopy will be obtained between 0.2 and 150 keV. The 0.2 keV threshold will allow the first measurements of absorption in our galaxy and possible host galaxies, constraining the distance scale and host environment.

Imaging Spectroscopy

Galactic astronomy

10.1117/12.253983

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Citations (12)