Balloon observations of Sco X-1 in the energy interval 17?106 keV

Jain, Abhay; Jayanthi, U. B.; Kasturirangan, K.; Rao, U. R.

doi:10.1007/bf00642196

Cited by 3 publications

(2 citation statements)

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“…Scorpius X-1 is a high-luminosity LMXB Z source, where the primary is a neutron star with a low magnetic field. The presence of a nonthermal component in Sco X-1 has been suggested (e.g., Peterson & Jacobson 1966;Riegler, Bolt, & Serlemitsos 1970;Agrawal et al 1971;Haymes et al 1972;Duldig et al 1983), and the absence of such a component has also been reported (e.g., Lewin, Clark, & Smith 1967;Buselli et al 1968;Jain et al 1973;Johnson et al 1980). In fact, highsensitivity searches have failed to detect such a component, placing strong upper limits on the nonthermal flux (e.g., Greenhill et al 1979;Rothschild et al 1980;Soong & Rothschild 1983).…”

Section: Introductionmentioning

confidence: 98%

High-Energy X-Ray Timing Experiment Detections of Hard X-Ray Tails in Scorpius X-1

D'Amico

Heindl

Rothschild

et al. 2001

The Astrophysical Journal

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We report the detection of a nonthermal hard X-ray component from Sco X-1 based on the analysis of 20-220 keV spectra obtained with the High-Energy X-Ray Timing Experiment on board the Rossi X-Ray Timing Explorer satellite. We find that the addition of a power-law component to a thermal bremsstrahlung model is required to achieve a good fit in five of 16 observations analyzed. Using Proportional Counter Array data, we were able to track the movement of the source along the Z diagram, and we found that the presence of the hard X-ray tail is not confined to a specific Z position. However, we do observe an indication that the power-law index hardens with increasing , as indicated from the position on the Z diagram. We find that the deriveḋ M nonthermal luminosities are ∼10% of that derived for the brightest of the atoll sources.

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Section: Introductionmentioning

confidence: 98%

High-Energy X-Ray Timing Experiment Detections of Hard X-Ray Tails in Scorpius X-1

D'Amico

Heindl

Rothschild

et al. 2001

The Astrophysical Journal

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“…It has been often reported that above 40 keV the spectrum appears to tend less steep (Matsuoka et al, 1972b, and the references therein ;Jain et aL, 1973), indicating the non-thermal nature of the source or the existence of a super-hot portion in the source (Haymes et al, 1972). Lewin et al (1970), however, could not observe such a hard component above 40 keV even with a large area detector at higher balloon altitude.…”

Section: Hard X-rays (~>40kev)mentioning

confidence: 93%

Sco X-1

Miyamoto

Matsuoka

1977

Space Sci Rev

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Abstract. The physical properties of X-ray, optical and radio emissions from Sco X-1 are reviewed. Sco X-I is a typical X-ray source which has an optically thick hot plasma. The observational spectra of X-ray and optical emissions are consistent with theoretical ones from the hot plasma, but the radio emission shows a non-thermal feature. The restrictive conditions for the model of Sco X-1 are discussed from the observational facts. In spite ot numerous observational facts on Sco X-1 further detailed and elaborate studies are necessary to understand this object and general compact X-ray sources comprehensively.Contents:

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