Towards determination of the symmetry energy: GW170817, Nuclear - - PowerPoint PPT Presentation

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Towards determination of the symmetry energy: GW170817, Nuclear - - PowerPoint PPT Presentation

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Towards determination of the symmetry energy: GW170817, Nuclear Polarizability and Direct Urca Cooling David E. lvarez Castillo Joint Institute for Nuclear Research POLNS18 CAMK Warsaw March 28, 2018 Outline Brief introduction to the

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Towards determination of the symmetry energy: GW170817, Nuclear Polarizability and Direct Urca Cooling

David E. Álvarez Castillo Joint Institute for Nuclear Research POLNS18 CAMK Warsaw March 28, 2018

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Outline

  • Brief introduction to the neutron star equation of state.
  • Symmetry energy measurements: the static nuclear

polarizability.

  • Astrophysics measurements of compact stars: multi-

messenger astronomy.

  • Astrophysical implications and perspectives.
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Nuclear Matter

  • C. Fuchs, H.H. Wolter, EPJA 30(2006)5
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Nuclear Equation of State

DD2 equation of state (dotted line) [S. Typel et al., Phys. Rev. C 81 (2010)] compares very well with chiral EFT N3LO (grey band)

Compilation of Neutron matter Equations of State;

  • T. Fischer et al.,

EPJA 50, 46 (2014)

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is the difference between symmetric nuclear matter and pure neutron matter: where α=1-2x

Nuclear Symmetry Energy

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Measuring the symmetry energy

Lattimer and Lim (2013) ApJ 771 51

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Measuring the symmetry energy:

Second-order effect in Coulomb-excitation measurements

  • J. N. Orce, Phys. Rev. C 91, no. 6, 064602 (2015)
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Second-order effect in Coulomb-excitation measurements

  • J. N. Orce, Phys. Rev. C 91, no. 6, 064602 (2015)
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Compact Star Sequences

(M-R ↔ EoS)

  • TOV Equations
  • Equation of State (EoS)

Lattimer,

  • Annu. Rev. Nucl. Part. Sci.

62, 485 (2012) arXiv: 1305.3510

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Symmetry energy effects

  • S. Kubis and D. E. Alvarez-Castillo - arXiv:1205.6368

PALu & MDI k models L models High density models

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Symmetry energy effects

  • S. Kubis and D. E. Alvarez-Castillo - arXiv:1205.6368
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Nuclear Symmetry Energy

  • S. Typel, Phys. Rev. C 89,

064321 (2014)

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Symmetry energy effects

11 12 13 14 15 16 R [km] 0.5 1 1.5 2 2.5 3 M [Msun]

DD2- DD2 DD2+ DD2++ g=1/6 g=1/3 g=1/2 g=2/3 g=4/5 g=9/10 g=1

symmetric EoS E0(n): DD2 symmetry energy Es(n):

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DUrca Process Constraint

  • D. E. Alvarez-Castillo, D. Blaschke and T. Klahn. (2016)

arXiv: 1604.08575

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Symmetry energy Conjecture

Klaehn et al. PhysRev C74 (2006)

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Universal symmetry energy contribution

The symmetry energy contribution to the neutron star EoS behaves universal!

arXiv: 1604.08575

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Predictions for neutron stars properties

  • J. Margueron, R. Hoffmann Casali, F. Gulminelli - Phys. Rev. C 97, 025806 (2018)

If composed exclusively of nucleons and leptons, our prediction is that neutron stars have a radius of 12.7 ± 0.4 km for masses between 1 and 2M⊙

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Predictions for neutron stars properties

  • J. Margueron, R. Hoffmann Casali, F. Gulminelli - Phys. Rev. C 97, 025806 (2018)

If composed exclusively of nucleons and leptons, our prediction is that neutron stars have a radius of 12.7 ± 0.4 km for masses between 1 and 2M⊙

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GW170817

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Implications from GW170817

GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral B.

  • B. P. Abbott et al. arXiv:1712.00451
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Implications from GW170817

GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral B.

  • B. P. Abbott et al. arXiv:1712.00451
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Implications from GW170817

9 10 11 12 13 14 15 16 17 R [km] 1.2 1.4 1.6 1.8 2 2.2 2.4 M[MO

. ]

PSR J0437-4715 PSR J1614-2230 PSR J0348+0432 GW170817 M1 M2

DD2-ddm DD2-dd2 DD2-ddp DD2F-ddm DD2F-dd2 DD2F-ddp

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Implications from GW170817

500 1000

L1

1000 2000 3000

L2 DD2-dd2 DD2-dd2m DD2-dd2p DD2F-dd2 DD2F-dd2m DD2F-ddp

50% 90%

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  • E. Annala et al. arXiv:1711.02644
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Perspectives

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NEUTRON-STAR RADIUS CONSTRAINTS FROM GW170817 AND FUTURE DETECTIONS

Andreas Bauswein,1 Oliver Just,2 Hans-Thomas Janka,3 and Nikolaos Stergioulas4

1Heidelberger Institut f¨

ur Theoretische Studien, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany

2Astrophysical Big Bang Laboratory, RIKEN, Saitama 351-0198, Japan 3Max-Planck-Institut f¨

ur Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany

4Department of Physics, Aristotle University of Thessaloniki, GR-54124 Thessaloniki, Greece

(Received July 1, 2016; Revised September 27, 2016; Accepted October 19, 2017)

Submitted to ApJL ABSTRACT We introduce a new, powerful method to constrain properties of neutron stars (NSs). We show that the total mass

  • f GW170817 provides a reliable constraint on the stellar radius if the merger did not result in a prompt collapse as

suggested by the interpretation of associated electromagnetic emission. The radius R1.6 of nonrotating NSs with a mass

  • f 1.6 M can be constrained to be larger than 10.68+0.15

0.04 km, and the radius Rmax of the nonrotating maximum mass

configuration must be larger than 9.60+0.14

0.03 km. We point out that detections of future events will further improve

these constraints. Moreover, we show that a future event with a signature of a prompt collapse of the merger remnant will establish even stronger constraints on the NS radius from above and the maximum mass Mmax of NSs from above. These constraints are particularly robust because they only require a measurement of the chirp mass and a distinction between prompt and delayed collapse of the merger remnant, which may be inferred from the electromagnetic signal or even from the presence/absence of a ringdown gravitational-wave (GW) signal. This prospect strengthens the case of

  • ur novel method of constraining NS properties, which is directly applicable to future GW events with accompanying

electromagnetic counterpart observations. We emphasize that this procedure is a new way of constraining NS radii from GW detections independent of existing efforts to infer radius information from the late inspiral phase or postmerger

  • scillations, and it does not require particularly loud GW events.

Mthres > M GW170817

tot

= 2.74+0.04

0.01 M,

Mthres = ✓ −3.606GMmax c2R1.6 + 2.38 ◆ · Mmax fit Mthres = ✓ −3.38GMmax c2Rmax + 2.43 ◆ · Mmax

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GW170817 Radius Constraints

8 10 12 14 16

R [km]

0.5 1.0 1.5 2.0 2.5 3.0

M [M]

excluded excluded Andreas Bauswein, Oliver Just, Hans-Thomas Janka and Nikolaos Stergioulas arXiv: 1710.06843

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Fictitious GW constraints

8 10 12 14 16

R [km]

0.5 1.0 1.5 2.0 2.5 3.0

M [M]

hypothetical Andreas Bauswein, Oliver Just, Hans-Thomas Janka and Nikolaos Stergioulas arXiv: 1710.06843

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Moments of Inertia

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Perspectives for new Instruments?

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NICER 2017

Gendreau, K. C., Arzoumanian, Z., & Okajima, T. 2012, Proc. SPIE, 8443, 844313

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Hot Spots

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Conclusions

  • The symmetry energy strongly determines the NS radius.
  • USEC conjecture has been corroborated and Es related

quantities found to be correlated with the NS radius.

  • There are future possible ways to measure those quantities

in the laboratory: NICO

  • GW170817 favours softer EoS and together with the Durca

constraint DD2F-like EoS are favoured.

  • Future GW observations, NICER and SKA will soon result

into stronger NS EoS constraints.

Gracias