Relativistic astrophysics explorer

Kaaret, Philip

doi:10.1016/j.asr.2003.03.061

Cited by 3 publications

(3 citation statements)

References 20 publications

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“…Strüder et al 2004) and the Relativistic Astrophysics Explorer (e.g. Kaaret 2004), should have considerably greater potential for making use of these statistics.…”

Section: Discussionmentioning

confidence: 99%

The bicoherence as a diagnostic for models of high-frequency quasi-periodic oscillations

Maccarone

Schnittman

2004

Monthly Notices of the Royal Astronomical Society

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We discuss the use of the bicoherence – a measure of the phase coupling of oscillations at different frequencies – as a diagnostic between different models for high‐frequency quasi‐periodic oscillations from Galactic black hole candidates. We show that this statistic is capable of finding qualitative distinctions between different hotspot models which produce nearly identical Fourier power density spectra. Finally, we show that proposed new timing missions should detect enough counts to make real use of this statistic.

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“…Strüder et al 2004) and the Relativistic Astrophysics Explorer (e.g. Kaaret 2004), should have considerably greater potential for making use of these statistics.…”

Section: Discussionmentioning

confidence: 99%

The bicoherence as a diagnostic for models of high-frequency quasi-periodic oscillations

Maccarone

Schnittman

2004

Monthly Notices of the Royal Astronomical Society

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“…RXTE results indicate that the magnitude of quasi periodic oscillations in compact binaries does tend to increase with higher energy [1], and there are two objects where RXTE fails to detect one of its two quasi periodic oscillation frequencies 1 ULX's are defined here as objects that are not galactic nuclei and their luminosity is greater than 10 40 ergs/sec. However, we claim that they are outweighed by the advantages described above.…”

Section: Limitations Of Focusing Opticsmentioning

confidence: 99%

A Focusing X-Ray Timing Observatory

Gorenstein¹

2004

AIP Conference Proceedings

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The next generation X-ray timing observatory will be a more powerful and versatile facility if it is based upon focusing optics rather than large area detectors. With X-ray CCDs or active pixel detectors (or possibly even microcalorimeters) in the focal plane(s) the spectral resolution will be significantly superior to the RXTE PCA making it possible to study the dynamics of the gravitationally redshifted Fe line in great detail. With orders of magnitude reduction of background the ability to study temporal variations of fainter sources in external galaxies will be much greater than with large area counters of the same collecting area. Furthermore, source confusion will not be an issue as it may be when large area detectors observe sources near the galactic center or in other galaxies. Focusing detectors do require larger open apertures than counters and their bandwidth is smaller. However, they are not necessarily heavier and in fact one candidate optic would be much lighter.

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“…Several other large-area follow-on mission concepts have also been previously proposed. [3][4][5][6] We begin with a brief overview of the science objectives and mission drivers for AXTAR, then discuss our detector and mission concepts, and finally summarize the results of our recent mission design study.…”

Section: Introductionmentioning

confidence: 99%

AXTAR: mission design concept

Ray

Chakrabarty

Wilson-Hodge

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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The Advanced X-ray Timing Array (AXTAR) is a mission concept for X-ray timing of compact objects that combines very large collecting area, broadband spectral coverage, high time resolution, highly flexible scheduling, and an ability to respond promptly to time-critical targets of opportunity. It is optimized for submillisecond timing of bright Galactic X-ray sources in order to study phenomena at the natural time scales of neutron star surfaces and black hole event horizons, thus probing the physics of ultradense matter, strongly curved spacetimes, and intense magnetic fields. AXTAR's main instrument, the Large Area Timing Array (LATA) is a collimated instrument with 2-50 keV coverage and over 3 square meters effective area. The LATA is made up of an array of supermodules that house 2-mm thick silicon pixel detectors. AXTAR will provide a significant improvement in effective area (a factor of 7 at 4 keV and a factor of 36 at 30 keV) over the RXTE PCA. AXTAR will also carry a sensitive Sky Monitor (SM) that acts as a trigger for pointed observations of X-ray transients in addition to providing high duty cycle monitoring of the X-ray sky. We review the science goals and technical concept for AXTAR and present results from a preliminary mission design study.

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Relativistic astrophysics explorer

Cited by 3 publications

References 20 publications

The bicoherence as a diagnostic for models of high-frequency quasi-periodic oscillations

The bicoherence as a diagnostic for models of high-frequency quasi-periodic oscillations

A Focusing X-Ray Timing Observatory

AXTAR: mission design concept

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