Supernovalike explosions of massive rotating stars from disks surrounding a black hole

Abstract

We perform a new general-relativistic viscous-radiation hydrodynamics simulation for supernovalike explosions associated with stellar core collapse of rotating massive stars to a system of a black hole and a massive torus, paying particular attention to large-mass progenitor stars with the zero-age main-sequence mass of <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:msub><a:mi>M</a:mi><a:mrow><a:mi>ZAMS</a:mi></a:mrow></a:msub><a:mo>=</a:mo><a:mn>20</a:mn></a:math>, 35, and <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mn>45</c:mn><c:msub><c:mi>M</c:mi><c:mo stretchy="false">⊙</c:mo></c:msub></c:math> of Aguilera-Dena [ ]. Assuming that a black hole is formed in a short timescale after the onset of the stellar collapse, the new simulations are started from initial data of a spinning black hole and infalling matter that self-consistently satisfy the constraint equations of general relativity. It is found that, with a reasonable size of the viscous parameter, the supernovalike explosion is driven by the viscous heating effect in the torus around the black hole, irrespective of the progenitor mass. The typical explosion energy and ejecta mass for the large-mass cases (<f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:msub><f:mi>M</f:mi><f:mrow><f:mi>ZAMS</f:mi></f:mrow></f:msub><f:mo>=</f:mo><f:mn>35</f:mn></f:math> and <h:math xmlns:h="http://www.w3.org/1998/Math/MathML" display="inline"><h:mn>45</h:mn><h:msub><h:mi>M</h:mi><h:mo stretchy="false">⊙</h:mo></h:msub></h:math>) are <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:mo>∼</k:mo><k:msup><k:mn>10</k:mn><k:mn>52</k:mn></k:msup><k:mtext> </k:mtext><k:mtext> </k:mtext><k:mi>erg</k:mi></k:math> and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:mo>∼</m:mo><m:mn>5</m:mn><m:msub><m:mi>M</m:mi><m:mo stretchy="false">⊙</m:mo></m:msub></m:math>, respectively, with <p:math xmlns:p="http://www.w3.org/1998/Math/MathML" display="inline"><p:mrow><p:mmultiscripts><p:mrow><p:mi>Ni</p:mi></p:mrow><p:mprescripts/><p:none/><p:mrow><p:mn>56</p:mn></p:mrow></p:mmultiscripts></p:mrow></p:math> mass larger than <r:math xmlns:r="http://www.w3.org/1998/Math/MathML" display="inline"><r:mn>0.15</r:mn><r:msub><r:mi>M</r:mi><r:mo stretchy="false">⊙</r:mo></r:msub></r:math>. These are consistent with the observational data of stripped-envelope and high-energy supernovae such as broad-lined type Ic supernovae. This indicates that rotating stellar collapses of massive stars to a black hole surrounded by a massive torus can be a central engine for high-energy supernovae. By artificially varying the angular velocity of the initial data, we explore the dependence of the explosion energy and ejecta mass on the initial angular momentum and find that the large explosion energy <u:math xmlns:u="http://www.w3.org/1998/Math/MathML" display="inline"><u:mo>∼</u:mo><u:msup><u:mn>10</u:mn><u:mn>52</u:mn></u:msup><u:mtext> </u:mtext><u:mtext> </u:mtext><u:mi>erg</u:mi></u:math> and large <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mrow><w:mmultiscripts><w:mrow><w:mi>Ni</w:mi></w:mrow><w:mprescripts/><w:none/><w:mrow><w:mn>56</w:mn></w:mrow></w:mmultiscripts></w:mrow></w:math> mass <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mo>≥</y:mo><y:mn>0.15</y:mn><y:msub><y:mi>M</y:mi><y:mo stretchy="false">⊙</y:mo></y:msub></y:math> are possible only when a large-mass compact torus with mass <bb:math xmlns:bb="http://www.w3.org/1998/Math/MathML" display="inline"><bb:mo>≳</bb:mo><bb:mn>1</bb:mn><bb:msub><bb:mi>M</bb:mi><bb:mo stretchy="false">⊙</bb:mo></bb:msub></bb:math> is formed. Published by the American Physical Society 2024

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