BD +37 442 is one of the very few hot subdwarf stars detected in the X-rayrange. The observed X-rays could arise either from accretion onto a neutron staror white dwarf companion (as suggested by the possible presence of X-raypulsations at P=19.2 s) or from intrinsic emission of the hot subdwarf itself.Both possibilities are interesting because they offer the possibility toinvestigate the poorly known properties of radiation driven winds at the lowmass-loss rates present in hot subdwarfs. A new observation is required toconfirm or reject the pulsations and to better constrain the spectralproperties.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2016-02-01T02:33:38Z/2016-02-01T22:46:59Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Dr Sandro MEREGHETTI, 2017, 'Origin of the X-ray emission in the He-rich luminous subdwarf BD +37 442', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-kx7p4f9
