Phases of dense matter in compact stars* David.Blaschke@gmail.com University of Wroclaw, Poland & JINR Dubna & MEPhI Moscow, Russia 1. Introduction: The Wroclaw Group 2. A few topics from *) arxiv:1803.01836 (D.B. & N. Chamel) – QCD Phase Diagram: how many critical points? – Stiffness, confinement, strangeness ... – Hybrid stars and M-R relations in view of GW170817 3. Outlook: Next Meetings in 2018 First POLNS Meeting, CAMK Warsaw, 26.-28.03.2018
Division: Theory of Elementary Particles @ IFT UWr Staff: prof. dr hab. Krzysztof Redlich (head) prof. dr hab. David Blaschke prof. dr hab. Ludwik Turko dr hab. Chihiro Sasaki, prof. Uwr dr hab. Tobias Fischer dr Pasi Huovinen dr Pok Man Lo PhD students: Dipl.-phys. Niels-Uwe Bastian mgr Łukasz Juchnowski mgr Maciej Lewicki mgr Michał Marczenko mgr Valeriya Mikhaylova mgr Michał Naskręt mgr Udita Shukla mgr Michał Szymański Main research topics: Master students: Ismail Soudi - Quantum field theory under extreme conditions - Physics of ultra-relativistic heavy-ion collisions +many visitors from 4 continents - Physics of compact stars and supernovae Current NCN research projects: Maestro (1), Opus (4), Polonez (2) Publications in 2010-2015: 241 (98 with ALICE Collab.)
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles - Collaborations
Division: Theory of Elementary Particles Collaboration with CERN Experiment NA61/SHINE since 2011 Goals of the experiment: - study of the properties of the onset of deconfinement and the search for the critical point of strongly interacting matter with nucleus-nucleus, proton-proton and proton-lead collisions at six collision momenta - Precise hadron production measurements for calibrating neutrino beams at J-PARC, Japan and Fermilab, US. Proton/pion-carbon and proton/pion-(replica target) interactions recorded - Precise hadron production measurements for reliable simulations of cosmic-ray air showers in the Pierre Auger Observatory and KASCADE experiments Energy and system size scan for Finding the QCD critical endpoint
Division: Theory of Elementary Particles Collaboration with ALICE @ CERN - excellent particle identification - high statistics data allow new level unprecendented accuracy - multihadron production near the QCD phase boundary challenges our understanding of the process of nonequilibrium QGP hadronization - confirmation of lattice QCD theory
Particle Production in Strong, Time-dependent Fields
Division: Theory of Elementary Particles Collaboration with NICA – MPD Collaboration at JINR Dubna and COST Action MP1304 “NewCompStar” Compact Stars Heavy-Ion Collisions - stiff EoS - high Mmax (at flow limit) (J1614-2230) - low Monset - low ncrit (all NS hybrid) (at NICA fixT) - excluded - soft EoS (J1614-2230) (dashed line) 29 member countries
Division: Theory of Elementary Particles PHAROS COST Action CA16214: “The multi-messenger physics and astrophysics of neutron stars”
21 member countries ! (CA15213) “T heory of HO t Matter in R elativistic Heavy-Ion Collisions” THOR ! New: Kick-off: Brussels, October 17, 2016
International Conference “Critical Point and Onset of Deconfinement” University of Wroclaw, May 29 – June 4, 2016
EPJA Topical Issues can be found at http://epja.epj.org/component/list/?task=topic
Division: Theory of Elementary Particles http://www.ift.uni.wroc.pl/~ztce
A few topics from: Phases of dense matter in compact stars* *) D. Blaschke & N. Chamel; arxiv:1803.01836 Invited contribution to the “CompStar White Book”, L. Rezzolla & P. Pizzochero (Eds.)
CEP in the QCD phase diagram: HIC vs. Astrophysics NuPECC Long Range Plan 2017; http://www.nupecc.org A. Andronic, D. Blaschke, et al., “Hadron production ...”, Nucl. Phys. A 837 (2010) 65 - 86
2 nd CEP in QCD phase diagram: Quark-Hadron Continuity? Gluons ↔ Vector mesons Quarks ↔ Baryons Goldstones ↔ Pseudoscalar mesons T. Schaefer & F. Wilczek, Phys. Rev. Lett. 82 (1999) 3956 C. Wetterich, Phys. Lett. B 462 (1999) 164 T. Hatsuda, M. Tachibana, T. Yamamoto & G. Baym, Phys. Rev. Lett. 97 (2006) 122001
Stiffness of NM / QM – where is the phase transition ? Alford & Horowitz: INT-16-2b Kurkela, Fraga, Schaffner-Bieleich, Vuorinen (2014) - stiffening necessary in order to meet the 2M_sun constraint from pulsar mass measurement - where is the phase transition? - which character has the transition? - where is the transition to pQCD ? - can nuclear matter be “matched” to pQCD?
Stiffness, confinement, strangeness ... T. Klaehn & T. Fischer, ApJ 810 (2015) 134 N.-U. Bastian & D.B., in preparation
Was GW170817 not a neutron star merger? EoS: DD2_P40 – SFM_α=0.3 M. Kaltenborn et al. PRD 96 (2017) 056024 TOV / TD calculation: M. Bejger et al. Alternative: Hybrid star (HS) – HS / HS-NS merger David Blaschke, INT Seattle, 12.03. 2018
Other examples: Multi-polytrope and multi-CSS model V. Paschalidis et al., arxiv:1712.00451 (Phys. Rev. D) Nonlocal NJL model (with interpolation), D. Alvarez-Castillo et al. (in preparation)
Effect of a mixed phase: KVOR_cut2 – SFM_α=0.3, A. Ayriyan et al., 1711.03926 (PRC accepted) Small surface tension – small structures K. Maslov, N. Yasutake et al. (in prep.) Pasta structures do not destroy the HS-NS merger alternative
Upcoming events in 2018 - PHAROS WG2 Meeting, CAMK Warsaw, April 9-11 - Quark matter 2018, Venice, May 14-19 - NFQCD 2018, YITP Kyoto, May 28 – June 29 - ICNFP 2018, OAC Kolymbari, July 3 – 13 - HISS Dubna “Matter under Extreme Conditions ...”, August 20-31 - CPOD 2018, Corfu, September 26-31 (?) - IWARA 2018, Machu Pichu, September 9-16 - Erice School 2018, September 16-24
Backup slides
Alternative facts of the day: New hybrid star solutions! arxiv:1711.06244v1, 1611.2017
Alternative facts of the day: New hybrid star solutions! arxiv:1711.06244v1, 1611.2017 Nuclear matter would be unstable! Not in our part of the Multiverse !!! Fake News:
History: Third family & Nonidentical Twins
History: Third family & Nonidentical Twins astro-ph/9807155; A&A (2000) L9 The original Twin paper uses Glendenning construction, not Maxwell one - Surface tension zero vs. infty! Pasta phases in-between ...
Neutron Star Interiors: Strong Phase Transition?
Neutron Star Interiors: Strong Phase Transition?
Neutron Star Interiors: Strong Phase Transition?
Neutron Star Interiors: Strong Phase Transition?
Mass-Radius Constraints: GW170817 & NICER GW170817, announced on 16.10.2017 B.P. Abbott et al. [LIGO/Virgo Collab.], PRL 119, 161101 (2017); ApJLett 848, L12 (2017)
GW170817: NS-NS Merger Multi-Messenger Astrophysics !! M < 2.17 M_sun (arxiv:1710.05938) GW170817, announced on 16.10.2017 B.P. Abbott et al. [LIGO/Virgo Collab.], PRL 119, 161101 (2017); ApJLett 848, L12 (2017)
GW170817: NS-NS Merger – Equation of State Constraints M. Bejger, D.B., et al., in preparation (2017) V. Paschalidis, K. Yagi, D. Alvarez-Castillo, D.B., A. Sedrakian, arxiv:1712.00451 (2017) Suggestion: The heavier NS be a hybrid star (HS) with a quark core, evtl. member of a “third family”!
Neutron Star Interiors: Strong Phase Transition? M-R Relation! V. Paschalidis et al., arxiv:1712.00451 High-mass twins (HMT) or typical-mass twins (TMT) ? For a classification see: J.-E. Christian, A. Zacchi, J. Schaffner-Bielich, arxiv:1707.07524
2.1 Constant Speed of Sound (CSS) Model PRD88, 013083 (2013)
Key fact: Mass “twins” ↔ 1 st order PT Systematic Classification [Alford, Han, Prakash: PRD88, 083013 (2013)] EoS P(ε) <--> Compact star phenomenology M(R) Most interesting and clear-cut cases: (D)isconnected and (B)oth – high-mass twins!
“Holy Grail” - High-Mass Twin Stars Twins prove exitence of disconnected populations (third family) in the M-R diagram Consequence of a first order phase transition Question: Do twins prove the 1st order phase trans.? Alvarez & Blaschke, arxiv:1304.7758
Neutron Star Interiors: Sequential Phase Transitions? How likely is it that s-quarks (and no s-bar) exist and survive in neutron stars in a QGP or in hyperons. How large is then the ratio s/(u+d) in neutron stars and in the Universe? There could also be single flavor quark matter, mixed with nuclear matter (d-quark dripline) Increasing density D.B., F. Sandin, T. Klaehn, J. Berdermann, PRC 80 (2009) 065807
Neutron Star Interiors: Sequential Phase Transitions? How likely is it that s-quarks (and no s-bar) exist and survive in neutron stars in a QGP or in hyperons. How large is then the ratio s/(u+d) in neutron stars and in the Universe? There could also be single flavor quark matter, mixed with nuclear matter (d-quark dripline) D.B., F. Sandin, T. Klaehn, J. Berdermann, PRC 80 (2009) 065807
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