229 research outputs found
Gamma ray constraints on the Galactic supernova rate
We perform Monte Carlo simulations of the expected gamma ray signatures of Galactic supernovae of all types to estimate the significance of the lack of a gamma ray signal due to supernovae occurring during the last millenium. Using recent estimates of the nuclear yields, we determine mean Galactic supernova rates consistent with the historic supernova record and the gamma ray limits. Another objective of these calculations of Galactic supernova histories is their application to surveys of diffuse Galactic gamma ray line emission
Gamma ray constraints on the galactic supernova rate
Monte Carlo simulations of the expected gamma-ray signatures of galactic supernovae of all types are performed in order to estimate the significance of the lack of a gamma-ray signal due to supernovae occurring during the last millenium. Using recent estimates of nuclear yields, we determine galactic supernova rates consistent with the historic supernova record and the gamma-ray limits. Another objective of these calculations of galactic supernova histories is their application to surveys of diffuse galactic gamma-ray line emission
Gamma-Ray Limits on Na-22 Production in Novae
Data accumulated from 1980 to1987 by the gamma-ray spectrometer on SMM have been searched for evidence of cosmic line emission at 1.275 MeV. This emission would result from the decay of 22Na, which might be produced by classical nova outbursts. No evidence of any 1.275 MeV emission of celestial origin has been found. A limit of 3×10-6M_sun; is placed on the accumulated 22Na from many novae occurring near the Galactic center, and a limit of 7×10-7M_sun; is placed on the mass of 22Na ejected by the closest of the recent neon-rich novae. These limits, while lower than any previous ones, are not in conflict with recent theoretical predictions of the production of 22Na in novae. The product of the frequency and average initial neon abundance of novae of the neon-rich class is constrained by the Galactic center 22Na limit
Constraining the Cosmic Star Formation Rate with the MeV Background
The Cosmic Gamma-ray Background (CGB) in the MeV regime has been measured
with COMPTEL and SMM. The origin of the CGB in this energy regime is believed
to be dominated by gamma-rays from Type Ia supernovae. We calculate the CGB
spectrum within the framework of FRW cosmology as a function of the cosmic star
formation rate, SFR(z). Several estimates of the SFR(z) have been reported
since the pioneering work of Madau et al. Here we discuss observational
constraints on SFR(z) derived from models of the CGB. In particular, we
consider the SFR obtained from Gamma-Ray Burst observations, which increases
dramatically with redshift beyond z ~ 1 in contrast to most estimates which
saturate or show a mild increase with redshift. Gamma-ray bursts may be the
most powerful tracers of star formation in the early universe and thus provide
signposts of the initial epoch of element synthesis. The star formation rate
implied by GRB statistics results in a gamma-ray background that matches the
observations more closely than that inferred from other tracers of star
formation. This may provide some support for the GRB/SFR-paradigm, which in
turn promises a powerful diagnostic of star formation, and thus cosmic chemical
evolution, from the era of Population III stars to the present
Supernovae and Positron Annihilation Radiation
Radioactive nuclei, especially those created in SN explosion, have long been sug-gested to be important contributors of galactic positrons. In this paper we describe the findings of three independent OSSE/SMM/TGRS studies of positron annihi-lation radiation, demonstrating that the three studies are largely in agreement as to the distribution of galactic annihilation radiation. We then assess the predicted yields and distributions of SN-synthesized radionuclei, determining that they are marginally compatible with the findings of the annihilation radiation studies
Comparative Studies of Line and Continuum Positron Annihilation Radiation
Positron annihilation radiation from the Galaxy has been observed by the
OSSE, SMM and TGRS instruments. Improved spectral modeling of OSSE observations
has allowed studies of the distribution of both positron annihilation radiation
components, the narrow line emission at 511 keV and the positronium continuum
emission. The results derived for each individual annihilation component are
then compared with each other. These comparisons reveal approximate agreement
between the distribution of these two emissions. In certain regions of the sky
(notably in the vicinity of the previously reported positive latitude
enhancement), the distribution of the emissions differ. We discuss these
differences and the methods currently being employed to understand whether the
differences are physical or a systematic error in the present analysis.Comment: 5 pages, to appear in the proceedings of the Gamma 2001 Symposium
(Baltimore, April 2001
Comparative Studies of Line and Contiuum Positron Annihilation Radiation
Positron annihilation radiation from the Galaxy has been observed by the OSSE, SMM and TGRS instruments. Improved spectral modeling of OSSE observa-tions has allowed studies of the distribution of both positron annihilation radiation components, the narrow line emission at 511 keV and the positronium continuum emission. The results derived for each individual annihilation component are then compared with each other. These comparisons reveal approximate agreement between the distribution of these two emissions. In certain regions of the sky (notably in the vicinity of the previously reported positive latitude enhancement), the distribution of the emissions differ. We discuss these differences and the methods currently being employed to understand whether the differences are physical or a systematic error in the present analysis
Positron Escape from Type Ia Supernovae
We generate bolometric light curves for a variety of type Ia supernova models
at late times, simulating gamma-ray and positron transport for various
assumptions about the magnetic field and ionization of the ejecta. These
calculated light curve shapes are compared with light curves of specific
supernovae for which there have been adequate late observations. %The selection
of models is generally not based upon the %ability to fit the late
observations, but rather because the %model has been demonstrated by other
authors to approximate the spectra %and early light curves of that specific SN.
From these comparisons we draw two conclusions: whether a suggested model is
an acceptable approximation of a particular event, and, given that it is, the
magnetic field characteristics and degree of ionization that are most
consistent with the observed light curve shape. For the ten SNe included in
this study, five strongly suggest Co positron escape as would be
permitted by a weak or radially-combed magnetic field. Of the remaining five
SNe, none clearly show the upturned light curve expected for positron trapping
in a strong, tangled magnetic field. Chandrasekhar mass models can explain
normally, sub-, and super- luminous supernova light curves; sub-Chandrasekhar
mass models have difficulties with sub- (and potentially normally) luminous
SNe. An estimate of the galactic positron production rate from type Ia SNe is
compared with gamma-ray observations of Galactic 511 keV annihilation
radiation. Additionally, we emphasize the importance of correctly treating the
positron transport for calculations of spectra, or any properties, of type Ia
SNe at late epochs ( 200 d).Comment: 82 pages including 25 figure
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