We conducted three-dimensional hydrodynamical simulations to study the interaction of two late opposite jets with the ejecta of a core collapse supernova (CCSN), and study the bipolar structure that results from this interaction as the jets inflate hot-low-density bubbles. The newly born central object, a neutron star (NS; or a black hole), launches these jets at about 50 to 100 days after explosion. The bubbles cross the photosphere in the polar directions at much earlier times than the regions at the same radii near the equatorial plane. The hot bubbles releases more radiation and the photosphere recedes more rapidly in the tenuous bubble. Our results strengthen earlier claims that were based on toy models that such an interaction might lead to a late peak in the light curve, and that an equatorial observer might see a rapid drop in the light curve. Our results have implications to much earlier jets that explode the star, either jets that the newly born NS launches in a CCSN, or jets that a NS companion that merges with the core of a massive star launches in a common envelope jets supernova (CEJSN) event. Our results add indirect support to the CEJSN scenario for fast blue optical transients, e.g., AT2018cow, ZTF18abvkwla, and CSS161010.

中文翻译：

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模拟核心坍缩超新星喷出物中晚期喷流引起的气泡膨胀

我们进行了三维流体动力学模拟，以研究两个相对较晚的喷流与核心坍缩超新星 (CCSN) 喷射物的相互作用，并研究由于喷流使热低密度气泡膨胀而产生的这种相互作用的双极结构。新诞生的中心天体，一颗中子星（NS；或黑洞），在爆炸后大约 50 到 100 天发射这些喷流。气泡在极地方向穿过光球层的时间比赤道面附近相同半径的区域要早得多。热气泡释放出更多的辐射，光球层在脆弱的气泡中后退得更快。我们的结果加强了先前基于玩具模型的说法，即这种相互作用可能导致光变曲线的后期峰值，赤道观察者可能会看到光变曲线的快速下降。我们的结果对爆炸恒星的更早的喷流有影响，要么是新生的 NS 在 CCSN 中发射的喷流，要么是 NS 伴星与大质量恒星的核心合并的喷流，在共包层喷流超新星 (CEJSN)事件。我们的结果为快速蓝色光学瞬变的 CEJSN 场景增加了间接支持，例如 AT2018cow、ZTF18abvkwla 和 CSS161010。