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Probing the metastability of a protoneutron star with hyperons in a core-collapse supernova

Sarmistha Banik
Phys. Rev. C 89, 035807 – Published 25 March 2014
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  • INTRODUCTION
  • THE EOS AND THE NUMERICAL SIMULATION
  • RESULTS AND DISCUSSION
  • SUMMARY
  • ACKNOWLEDGEMENTS
    • References

    Abstract

    The role of Λ hyperons is investigated in the dynamical collapse of a nonrotating massive star to a black hole using a one-dimensional general-relativistic (gr1d) code. The dynamical formation and evolution of a protoneutron star (PNS) to a black hole is followed using various progenitor models, adopting a hyperonic equation of state (EoS) generated by Shen et al. [Shen, Toki, Oyamatsu, and Sumiyoshi, Astrophys. J., Suppl. Ser. 197, 20 (2011)]. The results are compared with those of a nuclear EoS by Shen et al. [Shen, Toki, Oyamatsu, and Sumiyoshi, Nucl. Phys. A 637, 435 (1998)] to understand the role of Λ hyperons in the core-collapse supernova. The neutrino signals that may be used as a probe for core collapse is also discussed. Further, an exotic EoS may support a cold neutron star with a maximum mass much lower than that of a PNS. In this regard, the metastability of a PNS in the presence of Λ hyperons is studied in the long-time evolution of the progenitors, relevant to supernova SN1987A.

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    • Received 13 December 2013
    • Revised 28 January 2014

    DOI:https://doi.org/10.1103/PhysRevC.89.035807

    ©2014 American Physical Society

    Authors & Affiliations

    Sarmistha Banik*

    • BITS Pilani, Hyderabad Campus, Hyderabad 500078, India

    • *sarmistha.banik@hyderabad.bits-pilani.ac.in

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    Issue

    Vol. 89, Iss. 3 — March 2014

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    Images

    • Figure 1
      Figure 1

      Temporal evolution of baryonic and gravitational mass for the Shen np and npΛ EoS.

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    • Figure 2
      Figure 2

      Temporal evolution of central density for the Shen np and npΛ EoS.

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    • Figure 3
      Figure 3

      Temporal evolution of temperature for teh Shen np and npΛ EoS.

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    • Figure 4
      Figure 4

      Density profile of the 40M⊙ (black lines) and 23M⊙ (red/gray lines) progenitors with np [panel (a)] and npΛ [panel (b)] EoS at t=tbounce and at postbounce times of 0.363 and 0.563 s.

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    • Figure 5
      Figure 5

      Temperature profile of the 40M⊙ (black lines) and 23M⊙ (red/gray lines) progenitors with np [panel (a)] and npΛ [panel (b)] EoS at t=tbounce and at postbounce times of 0.363 and 0.563 s.

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    • Figure 6
      Figure 6

      Mass fractions of the constituents for the 40M⊙ (black lines) and 23M⊙ (red/gray lines) progenitors with the Shen npΛ EoS.

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    • Figure 7
      Figure 7

      Snapshots of mass fractions of the constituents vs radius at t=0.363 s (black lines) and 0.563 s (red/gray lines) postbounce for the 40M⊙ progenitors (a) and t=0.363 s (black lines) and 0.84 s (purple/gray lines) postbounce for the 23M⊙ progenitors (b) with the Shen npΛ EoS.

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    • Figure 8
      Figure 8

      Evolution of shock radii for the 23M⊙ progenitor models.

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    • Figure 9
      Figure 9

      Long-time evolution of central density for the 23M⊙ progenitor model with teh npΛ EoS.

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    • Figure 10
      Figure 10

      Long-time evolution of temperature for the 23M⊙ progenitor model with teh npΛ EoS.

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    • Figure 11
      Figure 11

      Long-time evolution of gravitational mass for the 23M⊙ progenitor model with teh npΛ EoS. The dark solid line is with fheat=1 for the 40M⊙ progenitor, and the rest of the lines are for the 23M⊙ progenitor.

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