0000012240 00000 n 0000004749 00000 n 0000007529 00000 n For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations.

We perform hydrodynamical calculations of core-collapse supernovae (SNe) with low explosion energies. H�b``�``�����@��������#D��A����N��\�2÷��JᑟDޅ>_T;}�Ht�qO{���ey?���[��w��{�y1]O�����UW^Htnxy$�//�pu����S�>��j�G���^!a|�z�ʟk_n�Nw[c��Qݯǻ�%95�ܽ\0���&�Y9�/N��?����+��wt��DD�ܸ8�Lպ�}?������%#�Nμ���m&/6w��~�Αn.�r������}�u����ϣ7g@}���� � ��jD�+������1���et@�3 0000010955 00000 n 0000010148 00000 n 0000023154 00000 n 0000025989 00000 n

0000032318 00000 n 0000018146 00000 n 0000007858 00000 n 0000011116 00000 n We perform three-dimensional simulations of mixing and fallback for selected non-rotating supernova models to study how explosion energy and asymmetries correlate with the remnant mass, remnant kick, and remnant spin. 0000009025 00000 n 0000009826 00000 n 0000006550 00000 n The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative 0000008539 00000 n 0000026012 00000 n 0000003325 00000 n We also perform calculations of nucleosynthesis and LCs of several fallback SN models, and find that a fallback SN from the progenitor with a main-sequence mass of 13 M sun can account for the properties of the peculiar Type Ia supernova SN 2008ha.

0000005150 00000 n The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. 0000014880 00000 n We show that the late time (gsimdays) power potentially associated with the accretion of this "fallback" material could significantly affect the optical light curve, in some cases producing super-luminous or otherwise peculiar supernovae.

0000032341 00000 n 0000021882 00000 n 0000007362 00000 n 5 r��n{qv���`��/� ߟ�}�L �����������. Agreement NNX16AC86A, Is ADS down? (or is it just me...), Smithsonian Privacy After freezeout of protons the remaining neutrons cause a shift out to short-lived isotopes, as is typical for the r-process. 0000023177 00000 n 0000004317 00000 n 0000021905 00000 n trailer << /Size 552 /Info 449 0 R /Root 456 0 R /Prev 520748 /ID[<8ec96e83324dc27044fee20ff2b6b653>] >> startxref 0 %%EOF 456 0 obj << /Metadata 454 0 R /PageMode /UseOutlines /Outlines 459 0 R /ViewerPreferences << >> /PageLabels 448 0 R /Pages 450 0 R /OpenAction [ 458 0 R /FitH 792 ] /Type /Catalog /Names 457 0 R /FICL:Enfocus 451 0 R >> endobj 457 0 obj << /Dests 340 0 R >> endobj 550 0 obj << /S 410 /T 624 /O 678 /E 694 /L 710 /Filter /FlateDecode /Length 551 0 R >> stream

SUPERNOVA FALLBACK ONTO MAGNETARS AND PROPELLER-POWERED SUPERNOVAE Anthony L. Piro and Christian D. Ott Theoretical Astrophysics, California Institute of Technology, 1200 East California Boulevard, M/C 350-17, Pasadena, CA 91125, USA; piro@caltech.edu, cott@tapir.caltech.edu Received 2011 March 31; accepted 2011 May 14; published 2011 July 13 ABSTRACT We explore fallback … 0000010308 00000 n B�DG�Ǥ���ʱ��������AZHGf��2a`����C�x��\p`��ݰ��[l�[�t�$(3�ppe2L�b)Pa���ƴC���%$���IE�@'��2�G�;��`CK�r��&�D}��LL^��q&�)E��w�0��si�)�D�`Q��Fk����H �/1L�Z�����P�"��D�^H:��H�.���N�Y��$��e`_ 0000027883 00000 n 0000004864 00000 n For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations. This rapid phase is followed by a relatively long (>~15 ms) simmering phase at ~2×109 K, which is the thermodynamic consequence of the hydrodynamic trajectory of the turbulent flows in the fallback outburst. 0000004564 00000 n During the slow phase, high-mass elements beyond the second peak are first made through rapid capture of both protons and neutrons. The kinetic energy and ejecta mass of the model are 1.2 × 1048 erg and 0.074M, respectively, and the ejected 56Ni mass is 0.003M. 0000029620 00000 n 0000012566 00000 n

0000002572 00000 n 0000009509 00000 n 0000036428 00000 n The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. 0000005739 00000 n 0000006711 00000 n

0000002291 00000 n These SNe do not have enough energy to eject the whole progenitor and most of the progenitor falls back to the central remnant. 0000010792 00000 n 0000008381 00000 n The resulting light curves are different and more diverse than previous fallback supernova models which ignored the input of accretion power and produced short-lived, dim transients. 0000008021 00000 n 0000015635 00000 n 0000009186 00000 n 0000016797 00000 n The flow stays close to the valley of stability during this phase. Agreement NNX16AC86A, Is ADS down? 0000013509 00000 n

The kinetic energy and ejecta mass of the model are 1.2 × 1048 erg and 0.074 M sun, respectively, and the ejected 56Ni mass is 0.003 M sun. 0000004449 00000 n 0000017420 00000 n 0000006063 00000 n (or is it just me...), Smithsonian Privacy 0000015974 00000 n



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