We propose to observe 3 dG halo stars with chromospheric emission, with the aimto determine if these metal poor stars can have coronae with properties similarto those of population I stars. By assuming the relationship found forpopulation I stars between MgII and coronal emission we have predicted the levelof X-ray luminosity of our targets. Their detection at the predicted level, aswell their non detection, will allow us to determine if old metal poor stars canhost a solar-like dynamo or if MgII emission is due to a basal flux, originatedby acustic waves without any r^ant magnetic component.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2004-06-28T16:02:36Z/2004-06-29T00:54:31Z
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 GIUSEPPINA MICELA, 2005, 'CORONAL EMISSION FROM DG HALO STARS', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-autku49
