Explore the words cloud of the Super-DENSE project. It provides you a very rough idea of what is the project "Super-DENSE" about.
The following table provides information about the project.
CENTRUM ASTRONOMICZNE IM. MIKOLAJAKOPERNIKA POLSKIEJ AKADEMII NAUK
|Coordinator Country||Poland [PL]|
|Total cost||146˙462 €|
|EC max contribution||146˙462 € (100%)|
1. H2020-EU.1.3.2. (Nurturing excellence by means of cross-border and cross-sector mobility)
|Duration (year-month-day)||from 2016-08-01 to 2018-07-31|
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|1||CENTRUM ASTRONOMICZNE IM. MIKOLAJAKOPERNIKA POLSKIEJ AKADEMII NAUK||PL (WARSZAWA)||coordinator||146˙462.00|
Neutron stars are one of the most exciting nuclear physics laboratories in the Universe. With interior densities well above nuclear saturation density they allow us to probe conditions impossible to replicate on Earth. In addition the thermal energy of the star is negligible compared to the Fermi energy, and neutrons in the interior will be superfluid. Superfluidity affects the dynamics of the star, as now neutrons can flow relative to the ‘normal’ components of the star with little viscosity. A direct probe of such an effect is thought to come from pulsar ‘glitches’, sudden jumps in frequency observed in otherwise spinning down radio pulsars. Most theories of glitches are based on the idea that a large scale superfluid component of the star is decoupled from the spin-down of the ‘normal’ component, and its sudden re-coupling leads to a glitch. On theoretical grounds we expect this effect as a superfluid rotates by forming an array of quantised vortices, and these vortices are strongly attracted, or ‘pinned’, by ions in the neutron star crust (or superconducting flux tubes in the core). If the superfluid cannot expel ‘pinned’ vortices it cannot spin-down and builds up a lag with respect to the normal component, until hydrodynamical lift forces become strong enough to break the pinning. Despite the success of this picture in interpreting glitches, only recently has progress been made in quantitatively describing glitches with large scale hydrodynamical simulations, and statistics throughout the pulsar population with small scale quantum-mechanical simulations of vortex motion. This proposal aims to bridge the gap between these two scales by using inputs from quantum mechanical simulations to describe vortex unpinning in hydrodynamical simulations, which will include state of the art crustal physics and thermal conduction. We will thus quantitatively describe the response of the star to different kinds of glitches and obtain, for the first time, robust statistics.
|year||authors and title||journal||last update|
V. Khomenko, B. Haskell
Modelling Pulsar Glitches: The Hydrodynamics of Superfluid Vortex Avalanches in Neutron Stars
published pages: , ISSN: 1448-6083, DOI: 10.1017/pasa.2018.12
|Publications of the Astronomical Society of Australia 35||2019-07-30|
G. Woan, M. D. Pitkin, B. Haskell, D. I. Jones, P. D. Lasky
Evidence for a Minimum Ellipticity in Millisecond Pulsars
published pages: L40, ISSN: 2041-8213, DOI: 10.3847/2041-8213/aad86a
|The Astrophysical Journal 863/2||2019-07-30|
A. Patruno, B. Haskell, N. Andersson
The Spin Distribution of Fast-spinning Neutron Stars in Low-mass X-Ray Binaries: Evidence for Two Subpopulations
published pages: 106, ISSN: 1538-4357, DOI: 10.3847/1538-4357/aa927a
|The Astrophysical Journal 850/1||2019-07-30|
Probing neutron star interiors with pulsar glitches
published pages: 203-208, ISSN: 1743-9213, DOI: 10.1017/S1743921317010663
|Proceedings of the International Astronomical Union 13/S337||2019-07-30|
B. Haskell, A. Patruno
Are Gravitational Waves Spinning Down PSR J 1023 + 0038 ?
published pages: , ISSN: 0031-9007, DOI: 10.1103/PhysRevLett.119.161103
|Physical Review Letters 119/16||2019-07-30|
P. M. Pizzochero, M. Antonelli, B. Haskell, S. Seveso
Constraints on pulsar masses from the maximum observed glitch
published pages: 134, ISSN: 2397-3366, DOI: 10.1038/s41550-017-0134
|Nature Astronomy 1/7||2019-07-30|
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