中子星内部 $\Delta$-直接Urca过程中的中微子发射率
Neutrino Emissivity in $Δ$-direct-Urca Processes Inside Neutron Stars
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中文总结 AI 辅助
本研究推导了中子星内部 $\Delta$-直接Urca过程的中微子发射率，发现其与核子-直接Urca过程相当，填补了该过程冷却贡献的量化空白。
中文摘要 AI 辅助
观测到的大质量中子星内部可能包含更重的重子，如 $\Delta$ 同位旋体和超子。在存在 $\Delta$ 同位旋体的情况下，发射中微子的核子Urca过程可以伴随涉及核子和超子的 $\Delta$-直接Urca过程。在过去三十年中，大量理论工作致力于理解中子星的热演化，其中核子和超子Urca过程作为主要冷却机制出现。虽然最近的研究提出在中子星致密核心中存在 $\Delta$ 同位旋体，但 $\Delta$-直接Urca过程对中微子发射率的具体贡献尚未被明确量化。在本工作中，我们通过推导中子星内部致密物质中 $\Delta$-直接Urca过程相关的中微子发射率来填补这一空白。我们表明，一旦 $\Delta$-直接Urca过程在运动学上被允许，其发射率与核子-直接Urca过程的发射率相当。
英文摘要
Observed massive neutron stars may contain heavier baryons such as $Δ$ isobars and hyperons in their interiors. In the presence of $Δ$ isobars, the neutrino emitting nucleonic Urca processes can be accompanied by $Δ$-direct-Urca processes involving nucleons and hyperons. Over the past three decades, significant theoretical effort has been dedicated to understanding the thermal evolution of neutron stars with the nucleonic and hyperonic Urca processes emerging as dominant cooling mechanisms. While recent studies have proposed the presence of $Δ$ isobars in the dense core of neutron stars, the specific contribution of the $Δ$-direct-Urca process to neutrino emissivity has not been explicitly quantified. In this work, we address this gap by deriving the neutrino emissivity associated with $Δ$-direct-Urca processes in dense matter inside neutron stars. We show that once $Δ$-direct-Urca processes become kinematically allowed, their emissivities are comparable to those of nucleonic-direct-Urca processes.
发表机构
- Indian Institute of Technology Jodhpur（焦特普尔印度理工学院）
- INFN, Sezione di Pisa（意大利国家核物理研究所比萨分部）
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