fallback supernova

0000003303 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`_ 0000021905 00000 n 0000004564 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. Notice, Smithsonian Terms of 0000003963 00000 n 0000011927 00000 n 0000012566 00000 n 0000008539 00000 n 0000017807 00000 n We investigate the possibility that the energetic Type II supernova OGLE-2014-SN-073 is powered by a fallback accretion following the failed explosion of a massive star. 0000004449 00000 n 5 r��n{qv��`��/� ߟ�}�L ��. 0000009826 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 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. 0000023154 00000 n 0000014564 00000 n 0000011605 00000 n 0000006711 00000 n 0000007858 00000 n 0000008021 00000 n 0000019062 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. 0000005150 00000 n 0000006226 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. We show that such fallback SNe can have a variety of light curves (LCs) but their photospheric velocities can only have some limited values with lower limits. 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. 0000024636 00000 n 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 … 0000028313 00000 n 0000009666 00000 n 0000009509 00000 n 0000005739 00000 n 455 0 obj << /Linearized 1 /O 458 /H [ 2572 753 ] /L 529978 /E 49746 /N 9 /T 520759 >> endobj xref 455 97 0000000016 00000 n Agreement NNX16AC86A, Is ADS down? Astrophysical Observatory. 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. 0000008218 00000 n The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative 0000009025 00000 n 0000008381 00000 n 0000010955 00000 n Use, Smithsonian 0000010466 00000 n to supernova fallback disks probably means that their power-law evolution breaks down when they rst become neutral. 0000004749 00000 n After freezeout of protons the remaining neutrons cause a shift out to short-lived isotopes, as is typical for the r-process. For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations. 0000002291 00000 n 0000005281 00000 n 0000004166 00000 n 0000025989 00000 n 0000017420 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. To this end, we make use of 3d hydrodynamical simulations of fallback supernova in close binary systems with properties designed to emulate LIGO sources. 0000011768 00000 n 0000005018 00000 n The flow stays close to the valley of stability during this phase. Notice, Smithsonian Terms of Agreement NNX16AC86A, Is ADS down? 0000010308 00000 n The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative For that reason, we investigate an alternate model involving the mass ejected by fallback in a supernova explosion, through hydrodynamic and nucleosynthesis calculations. 0000036303 00000 n (or is it just me...), Smithsonian Privacy We also suggest that SN 2008ha could have been accompanied by long gamma-ray bursts, and long gamma-ray bursts without associated SNe may be accompanied by very faint SNe with significant amount of fallback, which are similar to SN 2008ha. 0000036428 00000 n 0000012086 00000 n The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. 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 0000006063 00000 n 0000011277 00000 n 0000005900 00000 n 0000007694 00000 n 0000016597 00000 n 0000026012 00000 n several fallback SN models, and ﬁnd that a fallback SN from the progenitor with a main-sequence mass of 13M can account for the properties of the peculiar Type Ia supernova SN 2008ha. (or is it just me...), Smithsonian Privacy 0000002531 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. 0000007197 00000 n 0000003325 00000 n 0000032318 00000 n 0000041687 00000 n 0000003896 00000 n 0000032341 00000 n 0000015974 00000 n Here we investigate within the context of field binary progenitors how the the spin of LIGO sources vary when the helium star-descendent black hole (BH) is formed in a failed supernova (SN) explosion rather than by direct collapse. 0000004317 00000 n 0000004864 00000 n 0000011116 00000 n 0000019456 00000 n A low electron fraction is not required in this model; however, the detailed final distribution is sensitive to the electron fraction. Trans-iron element production beyond the second peak is made possible by a rapid (<1 ms) freezeout of α-particles that leaves behind a large nucleon (including protons!) Use, Smithsonian 0000027384 00000 n 0000005406 00000 n 0000007362 00000 n 0000016797 00000 n The nucleosynthetic products of this ejected material produce r-process elements, including those in the vicinity of the elusive third peak at mass number 195. to r-process seed ratio. 0000006874 00000 n 0000024613 00000 n Fallback in core-collapse supernovae plays a crucial role in determining the properties of the compact remnants and of the ejecta composition. 0000021882 00000 n Thus, SN 2008ha can be a core-collapse SN with a large amount of fallback. 0000010631 00000 n 0000029620 00000 n During the slow phase, high-mass elements beyond the second peak are first made through rapid capture of both protons and neutrons. 0000013509 00000 n 0000002572 00000 n 0000010148 00000 n 0000006387 00000 n 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. 0000005526 00000 n 0000010792 00000 n 0000028290 00000 n %PDF-1.4 %�� 0000004066 00000 n 0000029597 00000 n 0000011442 00000 n 0000030961 00000 n Astrophysical Observatory, Astrophysics - High Energy Astrophysical Phenomena. 0000009985 00000 n 0000012240 00000 n Some fraction of the material ejected in a core collapse supernova explosion may remain bound to the compact remnant, and eventually turn around and fall back. 0000014880 00000 n 0000030984 00000 n 0000017595 00000 n 0000007036 00000 n 0000008864 00000 n 0000008701 00000 n 0000009349 00000 n 0000009186 00000 n Thus, SN 2008ha can be a core-collapse SN with a large amount of fallback. 0000027883 00000 n 0000006550 00000 n 0000033427 00000 n The conditions for the leading r-process site candidate, neutrino-driven winds, cannot be reproduced self-consistently in current supernova models. 0000007529 00000 n 0000015635 00000 n Our simulations suggest that supernova fallback is a viable alternative scenario for the r-process. We perform hydrodynamical calculations of core-collapse supernovae (SNe) with low explosion energies. 0000018146 00000 n 0000023177 00000 n

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