PROPERTIES OF DISK GALAXIES IN A HIERARCHICAL FORMATION SCENARIO
PROPERTIES OF DISK GALAXIES IN A HIERARCHICAL FORMATION SCENARIO
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发表时间：
2000-01
影响因子：
1
通讯作者：
V. Avila-Reese;C. I. D. Astronomia;Unam;M. O. A. D. Brera;Italy.
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作者：
V. Avila-Reese;C. I. D. Astronomia;Unam;M. O. A. D. Brera;Italy.
我们使用星系演化模型在一个层次的由内而外的磁盘形成的情况下，研究盘星系的主要本地和全球的属性，以及它们的全球属性之间的一些相关性的起源。我们发现，盘星系的性质及其相关性主要是由系统的维里质量、晕质量聚集历史（MAH）和由自旋参数λ给出的角动量这三个初始因子及其色散共同作用的结果。MAH主要决定暗晕结构和积分色指数，λ主要决定盘面亮度和鼓盘比。我们利用引力不稳定性判据和盘状湍流星际介质中能量平衡驱动的自调节机制计算了星星的形成。在这个模型中，s的形成效率几乎与系统的质量无关。因此，星系积分色指数B V或恒星质光比M/LB并不依赖于质量。我们表明，由Wang & Heckman经验确定的亮度依赖的尘埃吸收解释了所观察到的色星等和色Tully-Fisher（TF）关系，而无需引入质量依赖的星星形成效率。在我们的模型中，星星的形成历史是由MAH和表面密度（λ）驱动的。处于离心平衡状态的圆盘在不断增长的冷暗物质晕内形成，其气体吸积速率与晕MAH成正比。磁盘呈现指数表面密度和亮度分布，负径向颜色指数梯度，和几乎平坦的旋转曲线。我们还计算了长期形成的隆起，由于在恒星盘的引力不稳定性。我们的模型的密集属性非常符合观测数据，它们遵循相同的趋势，星系遵循整个哈勃序列。本文所用宇宙学模型预测的红外TF关系和亮度-半径关系也与观测数据一致。本文提出的由内而外的分层地层模型的主要缺点是过多的径向颜色梯度和旋转曲线分解中的暗晕自治领。
We used galaxy evolutionary models in a hierarchical inside-out disk formation scenario to study the origin of the main local and global properties of disk galaxies as well as some of the correlations between their global properties. We found that most of disk galaxy properties and their correlations are the result of three (cosmological) initial factors of the system and their dispersions: the virial mass, the halo mass aggregation history (MAH), and the angular momentum given through the spin parameter λ. The MAH determines mainly the dark halo structure and the integral color indexes while λ determines mainly the disk surface brightness and the bulge-to-disk ratio. We calculated star formation using a gravitational instability criterion and a self-regulation mechanism driven by the energy balance in the disk turbulent interstellar medium. The efficiency of s formation in this model is almost independent from the mass of the system. Therefore, the galaxy integral color index B V or the stellar mass-to-luminosity ratio, M/LB, do not depend upon mass. We show that the luminosity-dependent dust absorption empirically determined by Wang & Heckman explains the observed color-magnitude and color Tully-Fisher (TF) relations without the necessity of introducing a massdependent star formation efficiency. The star formation history in our models is driven by both the MAH and the surface density (λ). The disks in centrifugal equilibrium form within growing cold dark matter halos with a gas accretion rate proportional to the halo MAH. The disks present exponential surface density and brightness profiles, negative radial color index gradients, and nearly flat rotation curves. We also calculated the secular formation of a bulge due to gravitational instabilities in the stellar disk. The intensive properties of our models agree very well with the observational data and they follow the same trends galaxies follow across the Hubble sequence. The infrared TF relations and the luminosity-radius relation predicted for the cosmological model used here also agree with the observational data. The main shortcomings of the inside-out hierarchical formation models presented in this paper are the excessive radial color gradients and the dark halo dominion in the rotation curve decompositions.