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A Measurement of Hard X and Gamma Radiation from Sco

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A Measurement of Hard X and Gamma Radiation from Sco RICE UNIVERSITY A MEASUREMENT OP HARD X AND GAMMA RADIATION PROM SCO X-l DONALD BAKER TWIEG A THESIS SUBMITTED IN PARTIAL FULFILLMENT OP THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE IN SPACE SCIENCE Thesis Director's Signature: Houston, Texas April, 1971 TABLE OF CONTENTS I. INTRODUCTION 1 A. Experimental Findings 1 B. X-Ray Production Mechanisms 9 C. The Need for Hard X-ray Investigations of Sco X-l 11 II. EXPERIMENT 69-2 13 A. Detector System 13 B. Experimental Procedure 16 C. Data Reduction 17 III. RESULTS AND CONCLUSION 27 IV. APPENDIX 32 A. General Considerations and Models 32 B. The Synchrotron Models 36 C. The Close Binary Model 37 V. ACKNOWLEDGMENTS 54 VI. REFERENCES 55 ABSTRACT A MEASUREMENT OP HARD X AND GAMMA RADIATION PROM SCO X-l by Donald Baker Twieg Sco X-l is the brightest extrasolar X-ray source in the sky. Additional knowledge of its output in the hard X~ray and gamma-ray regions could be particularly valuable in judging the validity of hypotheses intended to explain its unusual emission characteristics. On November 26, 1969, a balloon-borne scintillation detector was launched from Parana, Argentina to measure the output of Sco X-l above *10 keV. Despite complications caused by a partial battery failure and a solar X-ray flare, a flux above 75 keV was measured. The instrument and experimental procedures are dis¬ cussed briefly, and the reduction procedures and calculated fluxes are presented and discussed. Because of a possible solar contribution, the measured fluxes are interpreted as upper limits, but the results appear to verify the existence of a previously observed possibly non-thermal flux component departing at about *10 keV from the softer thermal component. Observations of Sco X-l in the X-ray, visual, infrared, and microwave regions are reviewed. Derived source param- eters and proposed models for the source are discussed In an appendix. No hypothesis has thus far been completely successful in explaining the many unusual characteristics of the electromagnetic emission of Sco X-l, but the close-binary hypothesis may be the most satisfactory. I. INTRODUCTION Sco X-l was discovered in 1962 in an X-ray survey of the sky (Giacconi et al. 1962); it is therefore histor¬ ically the first extra-solar system discrete source of X-radiation to be found. Its X-ray emission has been studied on numerous occasions since then. In the low-energy X-ray region, it is the brightest source in the sky, bright¬ er even than the quiet sun. In this section we survey the present knowledge of the electromagnetic fluxes from Sco X-l. We then discuss briefly the emission mechanisms which are likely to be responsible for the X-radiation from Sco X-l, and the rea¬ sons that hard X-ray investigations are needed. Sections II and III are concerned with the experiment and its re¬ sults, respectively. The theoretical models proposed for Sco X-l are dis¬ cussed in an appendix; the close-binary hypothesis is dis¬ cussed at some length, not because it seems to be verified by the results of this experiment, but because it seems the most valid on the basis of the general body of evidence. A. EXPERIMENTAL FINDINGS 1. X-rav Observations The findings in the rocket energy range (~1 keV:£E;£ ^0 keV) have been almost invariably consistent with a single exponential spectrum, and thus, presumably, with emission due to thermal bremsstrahlung (however, see Appendix). The nature of these rocket-borne experiments and their results should be mentioned here. Most of the Investiga¬ tions in this energy range use gas-filled proportional counters as detectors. Because of K- and L-shell edges in the detector absorption function, there are discontinuities in the detector response kernel, so that the process of un¬ folding the incident photon spectrum becomes a non-trivial matter. Thus the data must be interpreted by testing hypo¬ thetical input spectra, by folding them through the detector response, and then comparing the resulting pulse-height spectrum with the observed one. The most successful hypoth¬ esis tested in the case of Sco X-l has been invariably a single exponential spectrum, though there is obviously no guarantee that this is a unique solution. The point here is that experimental complications make it necessary to present proportional counter data in a model-dependent form. A list of X-ray investigations of Sco X-l is given in Table 1. The presumably exponential emission in this range has exhibited at various times different integrated intensities and has had e-folding energies varying from kT = 3 keV to kT = 8 keV. Apparently the softer spectra coincide with periods of greater total intensity. In a balloon-borne ex¬ periment, Lewin et al. (1968) observed a flare above 20 keV for which the e-folding energy was kT — 3 keV; the duration -3- of the flare was about 30 minutes. The presence of X-ray line structure has not been con¬ clusively demonstrated, though Holt et al. (1969) and Acton et al. (1970) have reported detection of an iron line near 7 keV. More observations are needed to verify this. The high-energy X-ray observations of Sco X-l indicate the presence of another, possibly non-thermal, continuum component (see Figures 1 and 2). The flux of photons with hV>40 keV is apparently variable, but is apparently always in excess of that expected from the kT=*6 keV thin-source bremsstrahlung spectrum observed at lower energies. The findings of Hudson and Peterson (1966) first sug¬ gested the presence of a harder spectral component for pho¬ tons with hi>S:i|0 keV. Agrawal et al. (1969) and Riegler et al. (1970) report a flux nearly an order of magnitude great¬ er than that seen by Buselli et al. (1969) near 60 keV (see Figure l). The data of Buselli et al. may be fitted equally well by an exponential with kT = 1^.8 keV or a power law with n = 3.79. The corresponding parameters for the data of Agrawal et al. are kT = 30 keV and n = ^J.5. This dis¬ parity is probably a real temporal variation; similar changes have been observed by various groups in the JjO-50 keV region, where the harder high-energy component first departs from the low-energy exponential. The flare observed by Lewin ot al. 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