Salvato in:
| Autori principali: | , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2025
|
| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2508.14535 |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866918452782956544 |
|---|---|
| author | Wang, Zihang Gao, Yu |
| author_facet | Wang, Zihang Gao, Yu |
| contents | Axionic dark matter can form structures known as miniclusters that host an axion star at their center. The axion star feeds on the host, and the axion star mass may grow beyond its stability limit, leading to a potential bosenova. Since a dilute axion star has a stable mass limit only when self-interaction is considered, we include axion self-interaction effects in this paper, and specify the condition for bosenova in the QCD axion and temperature-independent axion-like particle parameter spaces. We find that self-interaction may dominate the mass growth of the axion star. For a minicluster with a large initial overdensity, bosenova occurs in a large fraction of axion parameter space. For the QCD axion, bosenova occurs within the age of the Universe for miniclusters with an initial overdensity $δ\gtrsim 100$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_14535 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Axion Star Bosenova in Axion Miniclusters Wang, Zihang Gao, Yu High Energy Physics - Phenomenology High Energy Astrophysical Phenomena Axionic dark matter can form structures known as miniclusters that host an axion star at their center. The axion star feeds on the host, and the axion star mass may grow beyond its stability limit, leading to a potential bosenova. Since a dilute axion star has a stable mass limit only when self-interaction is considered, we include axion self-interaction effects in this paper, and specify the condition for bosenova in the QCD axion and temperature-independent axion-like particle parameter spaces. We find that self-interaction may dominate the mass growth of the axion star. For a minicluster with a large initial overdensity, bosenova occurs in a large fraction of axion parameter space. For the QCD axion, bosenova occurs within the age of the Universe for miniclusters with an initial overdensity $δ\gtrsim 100$. |
| title | Axion Star Bosenova in Axion Miniclusters |
| topic | High Energy Physics - Phenomenology High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.14535 |