We present an enhanced version of the Zernike wavefront sensor (WFS), which simultaneously measures phase and amplitude aberrations. The "vector-Zernike" WFS consists of a patterned liquid-crystal mask, which imposes a π∕2 phase on the point spread function core through the achromatic geometric phase acting with the opposite sign on opposite circular polarizations. After splitting circular polarization, the ensuing pupil intensity images are used to reconstruct the phase and the amplitude of the incoming wavefront. We demonstrate reconstruction of the complex wavefront with monochromatic lab measurements and show in simulation the high accuracy and sensitivity over a bandwidth up to 100%.
A planet hardly ever survives the supernova of the host star in a
bound orbit, because mass loss in the supernova and the natal kick
imparted to the newly formed compact object cause the planet to be
ejected. A planet in orbit around a binary has a considerably higher
probability to survive the supernova explosion of one of the inner
binary stars. In those cases, the planet most likely remains bound to
the companion of the exploding star, whereas the compact object is
ejected. We estimate this to happen to \sim 1/33∼1/33
the circum-binary planetary systems. These planetary orbits tend to be
highly eccentric
(e \ {\raise-.5ex\hbox{>}}\ 0.9),
and \sim 20∼20,%
of these planets have retrograde orbits compared to their former binary.
The probability that the planet as well as the binary (now with a
compact object) remains bound is about ten times smaller
(\sim 3\cdot 10^{-3}∼3⋅10−3).
We then expect the Milky way Galaxy to host
\ {\raise-.5ex\hbox{<}}\ 10
x-ray binaries that are still orbited by a planet, and
\\ {\raise-.5ex\hbox{<}}\ 150
planets that survived in orbit around the compact object’s companion.
These numbers should be convolved with the fraction of massive binaries
that is orbited by a planet.
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