|Title||Searching for thermal emission from nearby high magnetic field radio pulsars|
|Author||Dr Marjorie Gonzalez|
|Description||A major open issue in neutron star astrophysics is the connection between high magnetic field radio pulsars (HBRP), isolated neutron stars (INS), and magnetars. It is unclear why young HBRPs do not exhibit magnetar-like emission, and how INSs are related to both populations. We propose to observe three nearby, HBRPs to search for thermal emission from their surface. This emission is predicted to be observable if dominated by magnetic field decay. The pulsars have small distances and are regions of low interstellar absorption, offering us a rare opportunity to detect this emission or place strong constraints on its presence. We will then be able to test whether there are overlapping radiative properties from the HBRPs to magnetars, or whether they really are two distinct classes.|
|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, 2010-04-02T00:00:00Z, 055414, 17.56_20190403_1200. https://doi.org/10.5270/esa-xwzubn7|