Hybrid Gas Scintillation Proportional Counteriphoswich Detector For Hard X-Ray Astronomy

Grindlay, Jonathan E.; Manandhar, R. P.

doi:10.1117/12.962589

Cited by 3 publications

(1 citation statement)

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“…The ∼1% longer periodicity in the optical band compared to the X-ray band is likely caused by the coupling of a ∼3.9 d disk precession with the 3000 s orbital motion which is exhibited as the positive superhump seen in the SU UMa type dwarf novae. On the other hand, to explain the period of the ∼199 d long-term modulation found by Priedhorsky & Terrell (1984) and the stable optical period (Callanan et al 1995;, Grindlay (1989Grindlay ( , 1992 proposed that X1916-053 is a hierarchical triple system. The long-term variation is due to the changes of eccentricity of the inner binary, which affects the accretion rate, similar to the ∼171 d modulation seen in 4U 1820-30 ).…”

Section: Dipping X-ray Sourcesmentioning

confidence: 99%

Measuring the orbital periods of low mass X-ray binaries in the X-ray band

Chou¹

2014

Res. Astron. Astrophys.

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A low mass X-ray binary (LMXB) contains either a neutron star or a black hole accreting materials from its low mass companion star. It is one of the primary astrophysical sources for studying the stellar size compact objects and the accreting phenomena. As with other binary systems, the most important parameter of an LMXB is the orbital period, which allows us to learn about the nature of the binary system and constrain the properties of the system's components, including the compact object. As a result, measuring the orbital periods of LMXBs is essential for investigating these systems even though fewer than half of them have known orbital periods. This article introduces the different methods for measuring the orbital periods in the X-ray band and reviews their application to various types of LMXBs, such as eclipsing and dipping sources, as well as pulsar LMXBs.

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Section: Dipping X-ray Sourcesmentioning

confidence: 99%

Measuring the orbital periods of low mass X-ray binaries in the X-ray band

Chou¹

2014

Res. Astron. Astrophys.

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Imaging Gas Counters for X- and Gamma Ray Astronomy

Ramsey

1995

Imaging in High Energy Astronomy

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Abstract.Gas-filled detectors, such as proportional counters, have long been used in x-ray astronomy. They are robust, relatively easy to fabricate, and can provide large collecting areas with reasonable spatial and energy resolution. Despite coming of age in the 50's and 60's, their versatility is such that they are still planned for future missions. A vigorous development program, led mostly by the high energy physics community, has ensured cont inued improvements in proportional counter technology. These include multistep counters, microstrip technologies and optical avalanche chambers. High fill-gas pressures and the use of suitable converters permit operation up to 100s of GeV. The current status of imaging gas-filled detectors will be reviewed, concentrating on the lower energy region (< 100 keV) but also briefly covering higher energy applications up to the GeV region. This review is not intended to be exhaustive and draws heavily oil work currently in progress at MSFC.

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