NewCompStar - working group 1 Observations and modelling of compact stars. Pablo Cerdá-Durán (U. Valencia) Trento 13 Oct. 2017
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1 NewCompStar - working group 1 Observations and modelling of compact stars Pablo Cerdá-Durán (U. Valencia) Trento 13 Oct. 2017
2 WG1 objectives EM Observations Experiments Physics of strong interaction (WG2) Astrophysical scenarios: Core-collapse supernovae Neutron star cooling Bursting activity in neutron stars BNS merger Low mass X-ray binaries Pulsar glitches Modelling of astrophysical scenarios (WG1) Gravitational physics (WG3) GW Observations
3 Structure of the WG1 WG Leader: Nanda Rea (IEEC-CSIC/Anton Pannekoek I.) Topic leaders: Niccoló Bucciantini (U. Florence) Core collapse SN and the GRB connection Tiziana di Salvo (U. Cagliari) Compact stars in binary systems Wynn Ho (U. Southampton) Cooling of NSs Pablo Cerdá-Durán (U. Valencia) Magnetar flares and QPOs
4 Activities Working group meetings 2014, Barcelona (NewCompstar School) 2015, Meudon (MODE-SNR-PWN workshop) 2015, Tessaloniki (BNS merger workshop) 2016, Bormio (High energy transient sky thinkshop) 2016, Alicante (Origin, equilibrium and evolution of the magnetic field in NS workshop) 2016, Southampton (Oscillations and instabilities on NS workshop) 2016, Basel (Compact objects, EOS, explosive events and nucleosynthesis workshop) 2017, Caen (MODE-SNR-PWN workshop) 2017, Trento (New perspectives on Neutron Star Interiors) ~45 Short Term Scientific Missions (STSM) funded with WG1 topics White book
5 Neutron stars Pizzochero et al 2017 Glitches: Pizzochero (Milan), Haskell (Warsaw), I. Jones/Lander (Southampton) Constraints on crust-core coupling Pinning Constraints on pulsar mass Cumming et al 2016 X-ray binaries: Haskell (Warsaw), Cumming (McGuill) Mountains and GWs Measurement of heat capacity Asteroseismology: Ho/Andersson (Southampton), Glampedakis (Murcia), Passamonti(Alicante), Haskell (Warsaw), Torres-Forné/CD (Valencia) - g-modes in PNS and NS time evolution - r-modes and stability window Torres-Forné et al 2017
6 Neutron star evolution Braking index / CCOs/ Hidden magnetic field: Ho (Southampton), Torres-Forne/CD (Valencia) Ho et al 2015 Torres-Forne et al 2015 Magnetothermal evolution: Raduta (Bucharest), Graber (McGill), Grigorian (Dubna), Haensel (Warsaw) Stiffness Superconductivity Directly related to WG2
7 Magnetars QPOs: Gabler/CD/Stergioulas (MPA/Valencia/Tessaloniki), Passamonti/Lander (Alicante/Tübingen) - Magneto-elastic model - Constraining NS properties Magnetosphere structure: Akgün (Alicante), Bucciantini/Pili (Florence) - Maximum twist reconnection limit flares - Degeneracy and instability - Interior/exterior configurations (with rotation) Gabler et al 2017 Pili et al 2014 Akgün et al 2017 Magnetothermal evolution of magnetars: Pons/Akgün/CD (Alicante/Valencia), Gourgouliatos (Leeds), Geppert (Zielona Góra) - Recurrence time of flares - Ambipolar difusion in NS cores - First 3D simulations strong local field Akgün et al 2017 Gourgouliatos et al 2017
8 Core-collapse SNe and GRBs Multi-dimensional core-collapse supernovae: Janka/Müller (Garching), Foglizzo (Saclay), Obergaulinger(Valencia), Liebendörfer/Thielemann (Basel) 2D simulations: code comparisons/successful explosions (M<18 M sun ) 3D simulations with successful explosions Observables: GWs, neutrino luminosity, ejected mass, nucleosynthesis New transport schemes (M1) Muons facilitate explosion Progenitor dependence and NS properties: Kazeroni/Foglizzo (Saclay), Ertl/Janka (Garching) Non-monotonic dependence on progenitor mass Impact of SASI (spiral modes) on rotation Müller et al 2017 Kazeroni et al 2017 Ertl el al 2012 Ugliano el al 2012
9 MHD instabilities Magneto-rotational instability: Guilet(Saclay), Bugli (MPA), Bucciantini (Florence), Rembiasz/Obergaulinger/CD (Valencia) Local box simulations limited amplification Effect of neutrinos MRI suppressed Global simulations of disks PPI suppressed Tearing modes/reconnection: Del Zanna (Florence), Rembiasz/Obergaulinger/CD (Valencia) Fast reconnection (flares, PWN ) Meassuring numerical viscosity/resistivity Bugli et al 2017 Rembiasz et al 2016 Proto-magnetar formation in core-collapse: Obergaulinger/Aloy (Valencia)
10 Ideas for the future Towards complete/consistent models (SN, Magnetar QPOs, ) All necessary microphysics included Consistent microphysics allows to reduce parameter space/find correlations We cannot avoid magnetic turbulence in dynamic situations (BNS, SNe) Learn to the basics: dynamos, local simulations Then go back to global simulations: larger simulations (hexascale computers) vs subgrid-models Theoretical predictions have to match observations and give reasonable even rates Discussion on >3 rd branch and twins Connect with population synthesis models Even if you are a theorist, get involved in future observatories (Radio to X-rays) Devise new strategies to constrain NS properties Figure up and explain what are your needs
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