絮状波纹盘中年轻星协的诞生地和最近的恒星形成
Birth Sites of Young Stellar Associations and Recent Star Formation in a Flocculent Corrugated Disk
摘要：
与后向轨道积分，我们估计出生的年轻恒星协会和移动集团确定在太阳附近的年龄小于70万年的位置。大多数恒星协的诞生位置都比太阳的银河中心半径小，这意味着它们的恒星在诞生后径向向外移动。这一规则的适用者包括在太阳银河系中心半径之外形成的阿古斯星协和Octans星协。这些星协诞生高度的变化表明，它们诞生于分子云的波纹盘中，这与从目前的分子云分布和尘埃消光图中推断的结果相似。多个旋臂的功能，不同的，但近共转模式的速度和在不同的高度可以解释恒星协会的诞生地点。我们发现，年轻的恒星协会位于太阳附近的恒星的UV恒星速度分布的峰值之间。如果它们诞生在一个螺旋臂中，而螺旋臂会扰动穿过它的恒星轨道，这是可以预料的。相反，恒星协星似乎位于垂直相空间分布的峰值附近，这表明恒星协星诞生的气体与低速弥散盘星一起垂直运动。
英文摘要：
With backwards orbit integration we estimate birth locations of young stellar associations and moving groups identified in the solar neighborhood that are younger than 70 Myr. The birth locations of most of these stellar associations are at smaller galactocentric radius than the Sun, implying that their stars moved radially outwards after birth. Exceptions to this rule include are the Argus and Octans associations which formed outside the Sun's Galactocentric radius. Variations in birth heights of the stellar associations suggest that they were born in a corrugated disk of molecular clouds, similar to that inferred from the current filamentary molecular cloud distribution and dust extinction maps. Multiple spiral arm features with different but near corotation pattern speeds and at different heights could account for the stellar association birth sites. We find that the young stellar associations are located in between peaks in the UV stellar velocity distribution for stars in the solar neighborhood. This would be expected if they were born in a spiral arm which perturbs stellar orbits that cross it. In contrast, stellar associations seem to be located near peaks in the vertical phase space distribution, suggesting that the gas in which stellar associations are born moves vertically together with the low velocity dispersion disk stars.
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