论文标题
新的径向速度观察：潮汐半径以外的物质的证据
New radial velocity observations of AH Her: evidence for material outside the tidal radius
论文作者
论文摘要
提出了对AH Herculis的光谱观察结果。我们在罕见的最小值中找到了该物体，允许我们准确地得出半缩合：$ k_1 = 121 \ pm \，4 $ \ kmms \ and $ k_2 = 152 \ pm 2 $ \ kmms \及其质量函数$ m_w {\ sin}^{\ sin}^{3}^{3} $ 0.01 $ 0.01 $ = 0.01 $ 0.01 $ 0.01 $ \ \ $ m_r {\ sin}^{3} i = 0.24 \ pm 0.02 $ m $ _ {\ odot} $，而其二进制分离由$ a \ sin i = 1.39 \ pm 0.02 $ 0.02 $ 〜r $ $ _ {\ odot} $。轨道周期$ p_ {orb} $〜= 〜0.25812〜 $ \ pm 〜0.00032 $〜天数是从次级恒星的径向速度的功率谱分析中找到的。这些值与\ citet {Horne：1986}确定的值一致。我们的观察结果表明，K5是次级的最可能的光谱类型。我们讨论为什么我们赞成以下假设：啊，她是一个略微发展的恒星，在这种情况下，我们发现倾斜度的最佳解决方案会产生$ i = 48^\ circ \ pm 2^\ circ $。尽管如此，如果捐赠者是ZAMS星星，我们可以获得倾斜度在$ i = 43^\ circ $和$ i = 44^\ circ $之间。我们还提出了H $α$和H $β$的多普勒断层扫描，并发现两条线的发射都集中在低速下的大型不对称区域，但与二级恒星相反，在潮汐半径之外，因此在不稳定位置处。我们还分析了H $α$和H $β$线的轮廓，该轮廓显示了一个宽峰，并将其与先前的静态状态研究进行了比较，该研究显示了双峰型的轮廓，提供了其瞬时性质的证据。
Spectroscopic observations of AH Herculis during a deep quiescent state are put forward. We found the object in a rare long minima, allowing us to derive accurately the semi-amplitudes: $K_1 =121 \pm \, 4$ \kms\ and $K_2 =152 \pm 2$ \kms\ and its mass functions $M_W{ \sin }^{ 3 }i=0.30 \pm 0.01$ M$_{\odot}$ and $M_R{ \sin }^{ 3 }i=0.24 \pm 0.02$ M$_{\odot}$, while its binary separation is given by $a \sin i =1.39 \pm 0.02$~R$_{\odot}$. The orbital period $P_{orb}$~=~ 0.25812~$\pm~0.00032$~days was found from a power spectrum analysis of the radial velocities of the secondary star. These values are consistent with those determined by \citet{Horne:1986}. Our observations indicate that K5 is the most likely spectral type of the secondary. We discuss why we favour the assumption that the donor in AH Her is a slightly evolved star, in which case we find that the best solution for the inclination yields $i = 48^\circ \pm 2^\circ$. Nonetheless, should the donor be a ZAMS star, we obtain that the inclination is between $ i = 43^\circ$ and $i = 44^\circ$. We also present Doppler tomography of H$α$ and H$β$, and found that the emission in both lines is concentrated in a large asymmetric region at low velocities, but at an opposite position to the secondary star, outside the tidal radius and therefore at an unstable position. We also analyse the H$α$ and H$β$ line profiles, which show a single broad peak and compare it with the previous quiescent state study which shows a double-peaked profile, providing evidence for its transient nature.
