Talk detail

Participant	Rosinska, Dorota
Institution	Institute of Astronomy, University of Zielona Gora - Szafrana 2 - Zielona Gora - Lubuskie - Poland

Session	GW1	Accepted		Order	Time
Talk	Poster abstract	Title	Gravitational wave signals from ensemble of rotating neutron stars in Galaxy
Coauthors
Abstract	A spinning neutron star is a source of continuous gravitational waves, if its mass distribution is non-axisymmetric. Such asymmetry can be caused by various instabilities and deformations, e.g., due to magnetic field. We have performed calculations of the gravitational waves background produced by the ensemble of rotating neutron stars in the Milky Way. In our calculations we use a model of population of neutron stars which takes into account the distribution of birth places, kicks, and evolution of pulsars. We analyse the spatial shape and the spectrum of such background. We find that the signal is detectable above 20 Hz with a one year Einstein Telescope observations and above 40 Hz with Advanced Virgo/Ligo observation if the mean asymmetry is as high as $10^{-6}$.
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Session	GW1	Accepted		Order	Time
Talk	Poster abstract	Title	New view on properties of differentially rotating neutron stars
Coauthors
Abstract	An understanding of differentially rotating relativistic stars is key to many areas of astrophysics, in particular to the emission of gravitational waves. A newly born, proto-neutron star or a compact remnant of neutron stars binary merger are expected to rotate differentially and to be important sources of gravitational radiation. A highly accurate, multidomain spectral code is used in order to construct sequences of general relativistic, differentially rotating neutron stars in axisymmetry and stationarity. The high level of accuracy and stability of the code enable us to study stars with maximal masses and high rotation profiles. We investigate the solution space corresponding to broad ranges of degree of differential rotation and stellar densities. We find various types of configurations, which were not considered in previous work, mainly due to numerical limitations. The maximum allowed mass for the new types of configurations and moderate degree of differential rotation can be even 2-4 times higher then the maximum mass of non-rotating neutron stars with the same equation of state. Differential rotation can temporarily stabilize a hyper-massive neutron star against gravitational collapse.
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