Numerical Experiments for Nuclear Flashes toward Superbursts in an Accreting Neutron Star

<table>Composition distribution at <svg height="16.049999" id="M267" style="vertical-align:-0.3135pt" version="1.1" viewbox="0 0 48.474998 16.049999" width="48.474998" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink">
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</svg>). For log <svg height="11.375" id="M269" style="vertical-align:-0.17555pt" version="1.1" viewbox="0 0 69.050003 11.375" width="69.050003" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink">
<g transform="matrix(.017,-0,0,-.017,.062,11.112)"><path d="M619 482q0 -69 -40.5 -119t-96 -72.5t-118.5 -26.5h-44l-70 20l-31 -151q-14 -67 0.5 -83t89.5 -22l-5 -28h-287l8 28q65 7 81.5 22t29.5 83l79 398q12 56 0.5 70.5t-78.5 20.5l7 28h255q108 0 164 -43t56 -125zM524 478q0 141 -146 141q-25 0 -47 -8q-16 -6 -20.5 -13.5
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</svg>, the rp-process occurred and <svg height="19.987499" id="M270" style="vertical-align:-3.13504pt" version="1.1" viewbox="0 0 31.6875 19.987499" width="31.6875" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink">
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<g transform="matrix(.017,-0,0,-.017,12.112,15.85)"><path d="M561 176l29 -6q-25 -130 -36 -170h-517l-8 15l420 599h-173q-77 0 -102 -7t-39 -29q-19 -29 -35 -87l-29 1q9 111 12 183h24q9 -16 19 -20.5t34 -4.5h399l7 -14l-413 -594q48 -6 163 -6q94 0 131.5 7.5t58.5 29.5q28 29 55 103z" id="x5A"></path></g><g transform="matrix(.017,-0,0,-.017,22.584,15.85)"><path d="M524 0h-209v26q44 5 55 18t11 65v167q0 114 -91 114q-50 0 -109 -51v-235q0 -50 10 -61.5t55 -16.5v-26h-217v26q51 5 62 17t11 61v206q0 47 -9.5 58.5t-50.5 19.5v23q82 15 139 40v-79l67 47q47 30 83 30q60 0 94.5 -40t34.5 -112v-193q0 -50 10 -61.5t54 -16.5v-26z
" id="x6E"></path></g>
</svg> are produced. For the relation between lines and composition, see Table <a href="../tab2/">2</a>.</table>

Journal of Astrophysics

fig11

Figure 11

Figure 11: Numerical Experiments for Nuclear Flashes toward Superbursts in an Accreting Neutron Star 