|Title||Correlated timing and spectral study of the LMXB 4U 1608-52|
|Author||Dr Mariano Mendez|
|Description||We propose 6 TOO-like observations of the atoll source 4U 1608-52 during the decay of an outburst, for a total of 30 ksec (6 x 5 ksec). The observations should be carried out virgul40 days after the start of the outburst (as measured by the RXTE All Sky Monitor). This provides ample time for preparation and scheduling, thus minimizing the load to the XMM planners. The TOO-like trigger was chosen to maximize the probability of observing kHz QPOs. We will simultaneously observe with RXTE. Combining results from XMM and RXTE we will correlate the spectral and timing properties of this source. Our main goal is to determine how these properties depend on mass accretion rate, and whether the mass flows onto the central object through different channels of accretion.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2003-09-07T00:00:00Z, 007414, 17.56_20190403_1200. https://doi.org/10.5270/esa-g2skzti|