论文标题
标量场暗物质模型中的核心 - 障碍质量关系及其对超大质量黑洞形成的后果
Core-Halo Mass Relation in Scalar Field Dark Matter Models and its Consequences for the Formation of Supermassive Black Holes
论文作者
论文摘要
标量场暗物质（SFDM）光晕显示出具有孤子状核心和类似CDM的信封的核心 - 内螺旋结构。没有自我交互的模拟（自由场案例）报告了核心 - 纳洛质量关系$ m_c \ propto m_ {h}^β$，其中$β= 1/3 $或$β= 5/9 $，如果Core和Halo遵守某些能量或速度尺度，则可以理解这一点。我们将核心质量关系扩展到包括SFDM，具有自我交流（SI），即排斥或有吸引力，并研究了其对引力不稳定性和孤子核的崩溃的影响，从而导致超级质量黑洞（SMBH）形成。对于SFDM参数，在大尺度上却在小尺度上抑制了$ \ sim $ kpc大小的核心和类似CDM的结构形成，从自由场到排斥的SI极限，核心对于所有感兴趣的银河系均具有稳定。 For attractive SI, however, halos masses $M_h\sim (10^{10}-10^{12}) M_\odot$ have cores that collapse to SMBHs with $M_{SMBH}\sim 10^{6}-10^8 M_\odot$, as observations seem to require, while smaller-mass halos have stable cores, for particle masses $m\simeq （2.14 \ times 10^{ - 22} -9.9 \ times 10^{ - 20}）\ rm {ev}/c^2 $，如果自由场具有$β= 1/3 $，或$ m = 2.23 \ times 10^\ times 10^{ - 21}}}}}} -1.7 \ \ \ 18 \ \ \ \ 18} { - 18} $^$^$^$^$^$^$^/c^2 $^/c^2 $^/c^2 $^/c^2 $^/c^2 $^/c^2 $^/c.但是，对于自由场和排斥性情况，如果对粒子参数的先前约束放宽以使较小的（半乳酸尺度）核心构成较小的核心，那么对于相同范围的Halo和BH质量，HALOS也可以形成SMBH，只要$β= 5/9 $是正确的，对于自由场是正确的。在这种情况下，SFDM中的结构形成在很大程度上与冷暗物质（CDM）无法区分。这样的SFDM模型可能无法解决CDM的小规模结构问题，但它们会自然地解释SMBH的形成。由于尚未排除CDM本身，因此此类SFDM模型也必须是可行的（缩写）。
Scalar-field dark matter (SFDM) halos exhibit a core-envelope structure with soliton-like cores and CDM-like envelopes. Simulations without self-interaction (free-field case) report a core-halo mass relation $M_c\propto M_{h}^β$, with either $β=1/3$ or $β=5/9$, which can be understood if core and halo obey certain energy or velocity scalings. We extend the core-halo mass relations to include SFDM with self-interaction (SI), either repulsive or attractive, and investigate its implications for the gravitational instability and collapse of solitonic cores, leading to supermassive black hole (SMBH) formation. For SFDM parameters that make $\sim$ Kpc-sized cores and CDM-like structure formation on large scales but suppressed on small scales, cores are stable for all galactic halos of interest, from the free-field to the repulsive SI limit. For attractive SI, however, halos masses $M_h\sim (10^{10}-10^{12}) M_\odot$ have cores that collapse to SMBHs with $M_{SMBH}\sim 10^{6}-10^8 M_\odot$, as observations seem to require, while smaller-mass halos have stable cores, for particle masses $m\simeq (2.14\times 10^{-22}-9.9\times 10^{-20})\rm{eV}/c^2$, if the free-field has $β=1/3$, or $m = 2.23\times 10^{-21}-1.7\times 10^{-18}\rm{eV}/c^2$, if $β=5/9$. For free-field and repulsive cases, however, if previous constraints on particle parameters are relaxed to allow much smaller (sub-galactic scale) cores, then halos can also form SMBHs, for the same range of halo and BH masses, as long as $β= 5/9$ is correct for the free-field. In that case, structure formation in SFDM would be largely indistinguishable from Cold Dark Matter (CDM). Such SFDM models might not resolve the small-scale structure problems of CDM, but they would explain the formation of SMBHs quite naturally. Since CDM, itself, has not yet been ruled out, such SFDM models must also be viable (Abbreviated).
