论文标题
标量场暗物质光环中的轨道和绝热收缩：矮星系中的尖源问题
Orbits and adiabatic contraction in scalar field dark matter halos: revisiting the cusp-core problem in dwarf galaxies
论文作者
论文摘要
Bose-Einstein符合的暗物质，也称为标量场暗物质（SFDM）已成为冷暗物质（CDM）的流行替代品，因为它可以预测银河系核，而CDM Halos（“ CUSP核心问题”）。我们继续以强烈而令人反感的自我交流来研究SFDM。 SFDM（SFDM-TF）的Thomas-Fermi制度。在此模型中，结构形成被抑制低于与TF半径$ r_ \ text {tf} $相关的比例，该比例接近这些晕孔中的中心核的半径。我们首次通过研究这种光环中的绝热收缩过程（AC）的过程，首次研究巴属对现实的银河系SFDM-TF光晕曲线的影响。在此过程中，我们首先分析了适合SFDM的基本量子汉密尔顿 - 雅各布框架并计算暗物质轨道，以验证AC通常所需的假设的有效性。 Then, we calculate the impact of AC onto SFDM-TF halos of mass $\sim 10^{11}~M_{\odot}$, with various baryon fractions and core radii, $R_\text{TF} \sim (0.1 - 4)$ kpc, and compare our results with observational velocity data of dwarf galaxies.我们发现，具有KPC大小的核心半径的AC修饰的SFDM-TF光晕可很好地再现数据，这表明可能不需要出色的反馈。另一方面，具有子KPC核心半径的光环面临着与CDM相同的问题，因为它们不符合中央光晕部分中的星系数据。
Bose-Einstein-condensed dark matter, also called scalar-field dark matter (SFDM), has become a popular alternative to cold dark matter (CDM), because it predicts galactic cores, in contrast to the cusps of CDM halos ("cusp-core problem"). We continue the study of SFDM with a strong, repulsive self-interaction; the Thomas-Fermi regime of SFDM (SFDM-TF). In this model, structure formation is suppressed below a scale related to the TF radius $R_\text{TF}$, which is close to the radius of central cores in these halos. We investigate for the first time the impact of baryons onto realistic galactic SFDM-TF halo profiles by studying the process of adiabatic contraction (AC) in such halos. In doing so, we first analyse the underlying quantum Hamilton-Jacobi framework appropriate for SFDM and calculate dark matter orbits, in order to verify the validity of the assumptions usually required for AC. Then, we calculate the impact of AC onto SFDM-TF halos of mass $\sim 10^{11}~M_{\odot}$, with various baryon fractions and core radii, $R_\text{TF} \sim (0.1 - 4)$ kpc, and compare our results with observational velocity data of dwarf galaxies. We find that AC-modified SFDM-TF halos with kpc-size core radii reproduce the data well, suggesting stellar feedback may not be required. On the other hand, halos with sub-kpc core radii face the same issue than CDM, in that they are not in accordance with galaxy data in the central halo parts.
