Daniel C. Messina

Spectral evolution of pulse structures in gamma-ray bursts

The Hard X-Ray Burst Spectrometer (HXRBS) and Gamma-Ray Spectrometer (GRS) data from the Solar Maximum Mission satellite have been searched for gamma-ray bursts with sufficient intensities and relatively simple time profiles such that their spectral behavior may be studied on a time scale of about 1 s. Ten such events were observed with the GRS experiment, and four of these were also detected within the HXRBS field of view. Details are presented for two moderately intense bursts with relatively simple structure. The spectral evolutions of the remaining events are summarized briefly. Results suggest a pattern in the spectral evolution within burst pulses: a tendency for the high-energy emission to lead the low-energy emission, in contrast to the correlation of intensity and spectral hardness reported by Golenetskii et al. (1983).

SMM detection of diffuse Galactic 511 keV annihilation radiation

Observations of the 511 keV annihilation line from the vicinity of the Galactic center from October to February for 1980/1981, 1981/1982, 1982/1983, 1984/1985, and 1985/1986 are presented. The measurements were made with the gamma-ray spectrometer on the SMM. The design of the instrument and some of its properties used in the analysis are described, and the methods used for accumulating, fitting, and analyzing the data are outlined. It is shown how the Galactic 511 keV line was separated from the intense and variable background observed in orbit. The SMM observations are compared with previous measurements of annihilation radiation from the Galactic center region, and the astrophysical implications are discussed. It is argued that most of the measurements made to date suggest the presence of an extended Galactic source of annihilation radiation. 37 references.

Hard X-Ray Spectroscopy and Pulsar Phase Analysis of the Bursting X-Ray Pulsar GRO J1744-28 with OSSE

We report OSSE observations of the bursting X-ray pulsar GRO J1744-28 made in 1995 December and 1996 January at hard X-ray energies >35 keV. The pulse profile of the persistent (i.e., nonbursting) pulsar emission is fitted with a sinusoid in the energy range 35-90 keV. Residuals reveal a second harmonic amplitude of 3.0% ± 0.5% of the fundamental. The distribution of time intervals between bursts measured in January is characterized by a broad flat-topped function with width 35 minutes and mean 33 minutes. The burst profile averaged over an ensemble of 104 bursts in the 35-60 keV energy range has FWHM width of 3.6 ± 0.3 s and displays a factor of 2 faster rise time than decay and a pronounced dip in persistent emission after the burst. The phase of the sinusoidal pulse profile during bursts lags the phase prior to bursts by 90 ms (1.2 radians), and a 29 ± 6 ms (0.39 ± 0.08 radians) lag persists following the burst. There are no statistically significant spectral differences between the hard X-ray spectra of the bursting and persistent emission in the OSSE energy range, nor is there any evidence of annihilation or neutron capture line emission or cyclotron absorption.

Measurement of the 0. 3-8. 5 MeV Galactic gamma-ray spectrum from the Galactic center direction

The low-energy gamma-ray spectrum from the direction of the Galactic center is determined using data obtained with the SMM Gamma-Ray Spectrometer. It is found that the diffuse gamma-ray spectrum from the Galactic center region can be interpreted in a straightforward way as the sum of five components of a presented equation. The components include a hard power law dominating the continuum at high energies caused principally by cosmic ray electron bremsstrahlung radiation, two narrow lines due to Al-26 decay and positron annihilation, an excess continuum component below 0.511 MeV consistent with the annihilation of positrons by formation of Ps, and a soft power law at low energies which is consistent with an extrapolation upward in energy of known hard X-ray sources in the Galactic center region. 59 refs.

Limits on a Variable Source of 511 keV Annihilation Radiation near the Galactic Center

The Gamma Ray Spectrometer (GRS) on the Solar Maximum Mission satellite (SMM) has observed a strong Galactic source of 511 keV annihilation radiation from its launch in 1980 to its reentry in 1989. These observations are consistent with an extended source having an intensity of about 0.002 gamma/sq cm/s averaged over the central radian of Galactic longitude. These data are searched for evidence of the variable Galactic center source of 511 keV line radiation which was reported to have reappeared in 1988 by Leventhal et al. The SMM data are consistent with, but do not require, a compact source emitting a time-averaged flux of about 0.0004 gamma/sq cm/s during about 3 month transits in 1987 and 1988; they are inconsistent with a compact source flux in excess of 0.0008 gamma/sq cm/s for each year. 14 refs.

SMM observation of a cosmic gamma-ray burst from 20 keV to 100 MeV

Abstract The Solar Maximum Mission γ-ray spectrometer (GRS) has detected an intense γ-ray burst that occurred on 1984 August 5. The burst originated from a source in the constellation Hydra and lasted about 45 s. Its integral fluence 20 keV was 3 × 10−3 erg cm−2. Spectral evolution similar to other bursts detected by SMM was observed. The overall shape of the spectrum from 20 keV to 100 MeV, on timescales as short as 2 s, is relatively constant. This shape can be fitted by the sum of an exponential-type function and a power law. The spectral shape of this event may be characteristic of many γ-ray bursts. There is no evidence for narrow or broadened emission lines.

Geomagnetic Origin for Transient Particle Events from Nuclear Reactor-Powered Satellites

Transient events observed since 1980 by the Gamma-Ray Spectrometer experiment on the Solar Maximum Mission satellite (SMM) have been identified with radiation emitted from 18 different Soviet nuclear reactor—powered satellites. Most of these satellites are similar to Cosmos 954 and 1402 which reentered the atmosphere. Gamma radiation from these satellites was detected when they passed within about 400 to 500 kilometers of SMM. Positron annihilation line radiation (511 kiloelectron volts) and charged-particle events were detected when SMM encountered clouds of positrons and electrons emitted by these satellites and stored up to tens of minutes in the geomagnetic field. The rate of these events varied from about 1 in 5 days to over 30 per day and was strongly dependent on the operating altitudes of the Cosmos satellites and density of the upper atmosphere.

Spectral evolution in gamma-ray bursts

Abstract The Hard X-ray Burst Spectrometer (HXRBS) and the Gamma-Ray Spectrometer (GRS) on NASAs Solar Maximum Mission satellite (SMM) have independently monitored cosmic gamma-ray bursts since launch in February 1980. Several bursts with relatively simple pulse structure and sufficient intensity have been analyzed for evidence of spectral variability on timescales shorter than the pulse durations. In many of these bursts we find pulse structures, ranging in duration from 1 to 10 seconds, which exhibit a trend of hard-to-soft spectral evolution. No significant evidence for soft-to-hard evolution has been found, although the possibility of weak, extended low-energy emission is suggested in a few bursts. The HXRBS data above 100 keV and the GRS data above 1 MeV indicate that the spectral evolution generally is not due to time-varying absorption features at energies below 100 keV.

A search for evidence of energetic protons immediately prior to the impulsive phase of solar flares

Abstract Studies of gamma ray flares from the Solar Maximum Mission (SMM) show that energetic protons are present close, if not simultaneous, to the onset of the impulsive phase. It is important to flare models to know if such protons are (a) accelerated rapidly at the impulsive phase; (b) present as a non-thermal seed population and finally accelerated at the impulsive phase or (c) accelerated slowly prior to the flare. We have analysed data from the Gamma Ray Spectrometer on SMM for evidence of nuclear line emission prior to the impulsive phase, which would indicate the presence of protons > 5–10 MeV. The selected flares were accompanied by one or more of the following: extensive pre-cursor activity in soft X-rays; coronal activity; energetic protons in interplanetary space from a preceding flare. No evidence for any statistically-significant line emission prior to the impulsive phase was found, which lends support to (a) above, while putting limits on the spectrum of the seed population in (b). An upper limit of ≃ 1025 erg −1 is placed on the power in non-thermal protons above 10 MeV in the pre-flare phase.

Observations of Galactic gamma-radiation with the SMM spectrometer

Preliminary results from the SMM γ-ray spectrometer indicate the detection of a constant source of 0.511 MeV annihilation radiation from the Galaxy. This source was observed in each of 5 years as the region of the Galactic center passed through the instruments ∼120° field of view. Any year-to-year variability appears to be less than 30%. The measured intensity of the source is model dependent: for a point source at the center the average flux is (1.6 - 2.9) × 10−3 γ cm−2 s−1; for a distributed source following the Galactic CO emission the flux is (1.4 - 2.7) × 10−3 γ cm−2 s−1 rad−1 (uncertainty is due primarily to systematic errors). It is likely that the radiation comes from a diffuse source and is not associated with the reported compact source at the Galactic center. We have no new information to report on the distribution of 26Al γ-rays. Upper limits of 1.5 × 10−3 γ cm−2 s−1 are placed on Doppler-shifted lines from SS433.