EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION

Chatzopoulos, E.; Van Rossum, Daniel R.; Craig, Wheeler J.; Whalen, Daniel J.; Smidt, Joseph; Wiggins, Brandon

doi:10.1088/0004-637X/799/1/18

Title: EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION

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Abstract

Pair-instability supernovae (PISNe) have been suggested as candidates for some superluminous supernovae, such as SN 2007bi, and as one of the dominant types of explosion occurring in the early universe from massive, zero-metallicity Population III stars. The progenitors of such events can be rapidly rotating, therefore exhibiting different evolutionary properties due to the effects of rotationally induced mixing and mass-loss. Proper identification of such events requires rigorous radiation hydrodynamics and radiative transfer calculations that capture not only the behavior of the light curve but also the spectral evolution of these events. We present radiation hydrodynamics and radiation transport calculations for 90-300 M {sub ☉} rotating PISNe covering both the shock breakout and late light curve phases. We also investigate cases of different initial metallicity and rotation rate to determine the impact of these parameters on the detailed spectral characteristics of these events. In agreement with recent results on non-rotating PISNe, we find that for a range of progenitor masses and rotation rates these events have intrinsically red colors in contradiction with observations of superluminous supernovae. The spectroscopic properties of rotating PISNe are similar to those of non-rotating events with stripped hydrogen and helium envelopes. We find that the progenitor metallicitymore »« less

Authors:

Chatzopoulos, E.; Van Rossum, Daniel R. ^[1]; Craig, Wheeler J. ^[2]; Whalen, Daniel J. ^[3]; Smidt, Joseph ^[4]; Wiggins, Brandon ^[5]

Department of Astronomy and Astrophysics, Flash Center for Computational Science, University of Chicago, Chicago, IL 60637 (United States)
Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)
Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Albert-Ueberle-Strasse. 2, D-69120 Heidelberg (Germany)
T-2, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)
CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

Publication Date:: Tue Jan 20 00:00:00 EST 2015

OSTI Identifier:: 22364558

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 799; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COLOR; DIAGRAMS; HELIUM; HYDRODYNAMICS; HYDROGEN; MASS TRANSFER; METALLICITY; RADIANT HEAT TRANSFER; RADIATION TRANSPORT; ROTATION; STAR EVOLUTION; STELLAR WINDS; SUPERNOVAE; UNIVERSE; VISIBLE RADIATION

Citation Formats


                    Chatzopoulos, E., Van Rossum, Daniel R., Craig, Wheeler J., Whalen, Daniel J., Smidt, Joseph, and Wiggins, Brandon. EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION.  United States: N. p., 2015. 
        Web.  doi:10.1088/0004-637X/799/1/18.

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                    Chatzopoulos, E., Van Rossum, Daniel R., Craig, Wheeler J., Whalen, Daniel J., Smidt, Joseph, & Wiggins, Brandon. EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION.  United States.  https://doi.org/10.1088/0004-637X/799/1/18

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                    Chatzopoulos, E., Van Rossum, Daniel R., Craig, Wheeler J., Whalen, Daniel J., Smidt, Joseph, and Wiggins, Brandon. 2015.  
        "EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION".  United States.  https://doi.org/10.1088/0004-637X/799/1/18.

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@article{osti_22364558,

  title        = {EMISSION FROM PAIR-INSTABILITY SUPERNOVAE WITH ROTATION},

  author       = {Chatzopoulos, E. and Van Rossum, Daniel R. and Craig, Wheeler J. and Whalen, Daniel J. and Smidt, Joseph and Wiggins, Brandon},

  abstractNote = {Pair-instability supernovae (PISNe) have been suggested as candidates for some superluminous supernovae, such as SN 2007bi, and as one of the dominant types of explosion occurring in the early universe from massive, zero-metallicity Population III stars. The progenitors of such events can be rapidly rotating, therefore exhibiting different evolutionary properties due to the effects of rotationally induced mixing and mass-loss. Proper identification of such events requires rigorous radiation hydrodynamics and radiative transfer calculations that capture not only the behavior of the light curve but also the spectral evolution of these events. We present radiation hydrodynamics and radiation transport calculations for 90-300 M {sub ☉} rotating PISNe covering both the shock breakout and late light curve phases. We also investigate cases of different initial metallicity and rotation rate to determine the impact of these parameters on the detailed spectral characteristics of these events. In agreement with recent results on non-rotating PISNe, we find that for a range of progenitor masses and rotation rates these events have intrinsically red colors in contradiction with observations of superluminous supernovae. The spectroscopic properties of rotating PISNe are similar to those of non-rotating events with stripped hydrogen and helium envelopes. We find that the progenitor metallicity and rotation rate properties are erased after the explosion and cannot be identified in the resulting model spectra. It is the combined effects of pre-supernova mass-loss and the basic properties of the supernova ejecta such as mass, temperature, and velocity that have the most direct impact in the model spectra of PISNe.},

  doi          = {10.1088/0004-637X/799/1/18},

  url          = {https://www.osti.gov/biblio/22364558},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 1,

  volume       = 799,

  place        = {United States},

  year         = {Tue Jan 20 00:00:00 EST 2015},

  month        = {Tue Jan 20 00:00:00 EST 2015}

}

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