论文标题
中央星星的运动学动力为弓箭星云和失控的OB星星的大量多数分数
Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
论文作者
论文摘要
据推测，为恒星弓箭星云（SBNE）供电的OB恒星被认为具有较大的奇特速度。我们测量了SBN中心星的特殊速度，以使用$ GAIA $ EDR3数据来评估其运动学相对于一般O恒星种群的267 SBN中心恒星，并为455个Galactic O恒星样本来得出投影速度$ v _ {\ rm 2d} $。对于每个样品的一个子集，我们获得了新的光谱，以测量径向速度并识别多星系。我们发现，在SBN中央星星中，最低多重分数为36美元$ \ pm $ 6％，在失控的银河o恒星中与$ 28％的$ 28％一致。 Runaways之间的大量多数分数意味着非常有效的动态弹出，而不是二进制 - 苏佩尔诺娃的起源。 SBN中央明星的中间$ v _ {\ rm 2d} $是$ v _ {\ rm 2d} $ = 14.6 km s $^{ - 1} $，大于$ v _ {\ rm 2d} $ v _ {\ rm 2d} $ = 11.4 km s $ s $ s $^{ - 1} $^{ - 1} $ for non-bowshock o。 SBNE的中央星星有失控（$ V _ {\ rm 2d} $$> $ 25 km S $^{ - 1} $）的分数为24 $^{+9} _ { - 7} $％，与22 $^{+3} _ {+3} _ { - 3} $ for Control-Sample-spample-o Stars一致。大多数（76％）的SBNE Central Stars不是逃亡者。我们对蛋白形态和$ v _ {\ rm 2d} $ Kinematic Positation角度之间对齐（$δ_{\ rm pa} $）之间的对齐分析显示了两个人群：高度对齐（$σ_{pa} $ = 25 $ = 25 $^\ circe $），其中包括与最大$ v _ \ v _ fly plaste flastect”。 （不结盟）人口（占样本的69％）。位于HII区域内或附近的SBNE占后一个组成部分的比例比SBNE在孤立的环境中的比例更大，这意味着局部化ISM流是塑造其方向和形态的因素。我们概述了一种计算太阳能LSR运动的新概念方法，该方法产生[U $ _ \ odot $，V $ _ \ odot $，w $ _ \ odot $] = [5.5，7.5，4.5，4.5] km s $^{ - 1} $。
OB stars powering stellar bowshock nebulae (SBNe) have been presumed to have large peculiar velocities. We measured peculiar velocities of SBN central stars to assess their kinematics relative to the general O star population using $Gaia$ EDR3 data for 267 SBN central stars and a sample of 455 Galactic O stars to derive projected velocities $v_{\rm 2D}$. For a subset of each sample we obtained new optical spectroscopy to measure radial velocities and identify multiple-star systems. We find a minimum multiplicity fraction of 36$\pm$6% among SBN central stars, consistent with $>$28% among runaway Galactic O stars. The large multiplicity fraction among runaways implicates very efficient dynamical ejection rather than binary-supernova origins. The median $v_{\rm 2D}$ of SBN central stars is $v_{\rm 2D}$=14.6 km s$^{-1}$, larger than the median $v_{\rm 2D}$=11.4 km s$^{-1}$ for non-bowshock O stars. Central stars of SBNe have a runaway ($v_{\rm 2D}$$>$25 km s$^{-1}$) fraction of 24$^{+9}_{-7}$%, consistent with the 22$^{+3}_{-3}$% for control-sample O stars. Most (76%) of SBNe central stars are not runaways. Our analysis of alignment ($Δ_{\rm PA}$) between the nebular morphological and $v_{\rm 2D}$ kinematic position angles reveals two populations: a highly aligned ($σ_{PA}$=25$^\circ$) population that includes stars with the largest $v_{\rm 2D}$ (31% of the sample) and a random (non-aligned) population (69% of the sample). SBNe that lie within or near HII regions comprise a larger fraction of this latter component than SBNe in isolated environments, implicating localized ISM flows as a factor shaping their orientations and morphologies. We outline a new conceptual approach to computing the Solar LSR motion, yielding [U$_\odot$, V$_\odot$, W$_\odot$]= [5.5, 7.5, 4.5] km s$^{-1}$.
