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Multimessenger asteroseismology of core-collapse supernovae
Univ Arizona, Dept Astron Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.;Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada.;Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada.;Univ Copenhagen, Niels Bohr Inst, DARK, Lyngbyvej 2, DK-2100 Copenhagen, Denmark..
Stockholm Univ, Dept Astron, AlbaNova, S-10961 Stockholm, Sweden.;Stockholm Univ, Oskar Klein Ctr, AlbaNova, S-10961 Stockholm, Sweden..
Stockholm Univ, Oskar Klein Ctr, AlbaNova, S-10961 Stockholm, Sweden.;Stockholm Univ, Dept Phys, AlbaNova, S-10961 Stockholm, Sweden..
Univ Copenhagen, Niels Bohr Inst, DARK, Lyngbyvej 2, DK-2100 Copenhagen, Denmark.;Univ Copenhagen, Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark..
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2019 (English)In: Physical Review D: covering particles, fields, gravitation, and cosmology, ISSN 2470-0010, E-ISSN 2470-0029, Vol. 100, no 12, article id 123009Article in journal (Refereed) Published
Abstract [en]

We investigate correlated gravitational wave and neutrino signals from rotating core-collapse supernovae with simulations. Using an improved mode identification procedure based on mode function matching, we show that a linear quadrupolar mode of the core produces a dual imprint on gravitational waves and neutrinos in the early post-bounce phase of the supernova. The angular harmonics of the neutrino emission are consistent with the mode energy around the neutrinospheres, which points to a mechanism for the imprint on neutrinos. Thus, neutrinos carry information about the mode amplitude in the outer region of the core, whereas gravitational waves probe deeper in. We also find that the best-fit mode function has a frequency bounded above by similar to 420 Hz, and yet the mode's frequency in our simulations is similar to 15% higher, due to the use of Newtonian hydrodynamics and a widely used pseudo-Newtonian gravity approximation. This overestimation is particularly important for the analysis of gravitational wave detectability and asteroseismology, pointing to limitations of pseudo-Newtonian approaches for these purposes, possibly even resulting in excitation of incorrect modes. In addition, mode frequency matching (as opposed to mode function matching) could be resulting in mode misidentification in recent work. Lastly, we evaluate the prospects of a multimessenger detection of the mode using current technology. The detection of the imprint on neutrinos is most challenging, with a maximum detection distance of similar to 1 kpc using the IceCube Neutrino Observatory. The maximum distance for detecting the complementary gravitational wave imprint is similar to 5 kpc using Advanced LIGO at design sensitivity.

Place, publisher, year, edition, pages
American Physical Society, 2019. Vol. 100, no 12, article id 123009
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Physical Sciences
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URN: urn:nbn:se:kth:diva-266238DOI: 10.1103/PhysRevD.100.123009ISI: 000502125100003Scopus ID: 2-s2.0-85076756728OAI: oai:DiVA.org:kth-266238DiVA, id: diva2:1382469
Note

QC 20200103

Available from: 2020-01-03 Created: 2020-01-03 Last updated: 2020-01-03Bibliographically approved

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