Stellar helium burning in other universes: A solution to the triple alpha fine-tuning problem
详细信息 查看全文
- 作者：Fred C. Adams ; a ; b ; fca@umich.edu ; Evan Grohsa
- 关键词：Fine-tuning ; Multiverse ; Stellar nucleosynthesis ; Triple alpha
- 刊名：Astroparticle Physics
- 出版年：2017
- 出版时间：January 2017
- 年：2017
- 卷：87
- 期：Complete
- 页码：40-54
- 全文大小：999 K
- 卷排序：87
文摘
Motivated by the possible existence of other universes, with different values for the fundamental constants, this paper considers stellar models in universes where 8Be is stable. Many previous authors have noted that stars in our universe would have difficulty producing carbon and other heavy elements in the absence of the well-known 12C resonance at 7.6 MeV. This resonance is necessary because 8Be is unstable in our universe, so that carbon must be produced via the triple alpha reaction to achieve the requisite abundance. Although a moderate change in the energy of the resonance (200–300 keV) will indeed affect carbon production, an even smaller change in the binding energy of beryllium (∼100 keV) would allow 8Be to be stable. A stable isotope with A=8A=8 would obviate the need for the triple alpha process in general, and the 12C resonance in particular, for carbon production. This paper explores the possibility that 8Be can be stable in other universes. Simple nuclear considerations indicate that bound states can be realized, with binding energy ∼0.1−1∼0.1−1 MeV, if the fundamental constants vary by a ∼few−10∼few−10%. In such cases, 8Be can be synthesized through helium burning, and 12C can be produced later through nuclear burning of beryllium. This paper focuses on stellar models that burn helium into beryllium; once the universe in question has a supply of stable beryllium, carbon production can take place during subsequent evolution in the same star or in later stellar generations. Using both a semi-analytic stellar structure model as well as a state-of-the-art stellar evolution code, we find that viable stellar configurations that produce beryllium exist over a wide range of parameter space. Finally, we demonstrate that carbon can be produced during later evolutionary stages.