|Title||X-ray emission from brown dwarfs: A sequence of temperatures and ages|
|Author||Dr Ralph Neuhaeuser|
|Description||We propose to observe several brown dwarfs. Two such sub-stellar objects were detected as X-ray sources for the first time recently with ROSAT. It is not known, how brown dwarfs emit X-rays, possibly as coronal emission like very late-type stars. In that case, we should expect a correlation of brown dwarf X-ray emission with spectral type, ie. temperature, and also with age, ie. bolometric luminosity. After the deuterium burning phase, central temperature and, hence, temperature gradient will decrease. Hence, convection and X-ray emission may cease. Our targets, 2 fields with one brown dwarf each and one field with several sub-stellar objects, are selected to probe a range in age and temperature, to study cooling time-scale and internal structure of brown dwarfs.|
|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, 2003-06-06T00:00:00Z, 000274, 17.56_20190403_1200. https://doi.org/10.5270/esa-q53a4dj|