Jets launched at magnetar birth cannot be ignored |
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| Institution: | 1. TEI of Western Macedonia, Kozani, Greece;2. KAIST, Daejeon, South Korea;3. University of Ioannina, Ioannina Gr 451 10, Greece;4. Department of Theoretical Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece;5. Department of Physics, Ben Gurion University, Israel;1. Astronomy Department and Meteorology, Faculty of Science, Al-Azhar University, Cairo, Egypt\n;2. Astronomy Department, National Research Institute of Astronomy and Geophysics, Helwan, Cairo, Egypt\n;3. Kottamia Center of Scientific Excellence in Astronomy and Space Sciences (KCScE) STDF, ASRT, Cairo, Egypt\n;1. INAF Astronomical Observatory of Padova, via dell’Osservatorio 8, 36012 Asiago (VI), Italy;2. ANS Collaboration, c/o Astronomical Observatory, 36012 Asiago (VI), Italy |
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| Abstract: | I question models for powering super energetic supernovae (SESNe) with a magnetar central engine that do not include jets that are expected to be launched by the magnetar progenitor. I show that under reasonable assumptions the outflow that is expected during the formation of a magnetar can carry an amount of energy that does not fall much below, and even surpasses, the energy that is stored in the newly born spinning neutron star (NS). The rapidly spinning NS and the strong magnetic fields attributed to magnetars require that the accreted mass onto the newly born NS possesses high specific angular momentum and strong magnetic fields. These ingredients are expected, as in many other astrophysical objects, to form collimated outflows/jets. I argue that the bipolar outflow in the pre-magnetar phase transfers a substantial amount of energy to the supernova (SN) ejecta, and it cannot be ignored in models that attribute SESNe to magnetars. I conclude that jets launched by accretion disks and accretion belts are more likely to power SESNe than magnetars are. This conclusion is compatible with the notion that jets might power all core collapse SNe (CCSNe). |
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