天囷增廿一
  | |
| 观测数据 历元 J2000 分点 J2000 | |
|---|---|
| 星座 | 金牛座 |
| A | |
| 赤经 | 03h 36m 47.291s[1] |
| 赤纬 | 00° 35′ 15.94″[1] |
| 视星等 (V) | 5.91[2] |
| B | |
| 赤经 | 03h 36m 46.844s[3] |
| 赤纬 | 00° 35′ 15.93″[3] |
| 视星等 (V) | 8.79[2] |
| 特性 | |
| 光谱分类 | K2:Vnk[4] (K1 IV + G5 V + K3 V)[5] |
| 变星类型 | RS CVn[6] |
| 天体测定 | |
| A | |
| 径向速度 (Rv) | −21.24+6.62 −[1] km/s |
| 自行 (μ) | 赤经：−32.894 mas/yr 赤纬：−161.772 mas/yr |
| 视差 (π) | 33.7528 ± 0.0866[1] mas |
| 距离 | 96.6 ± 0.2 ly (29.63 ± 0.08 pc) |
| 绝对星等 (MV) | 3.6[2] |
| B | |
| 径向速度 (Rv) | −15.34±0.18[3] km/s |
| 自行 (μ) | 赤经：−34.359 mas/yr 赤纬：−138.137 mas/yr |
| 视差 (π) | 33.8664 ± 0.0226[3] mas |
| 距离 | 96.3 ± 0.2 ly (29.53 ± 0.02 pc) |
| 绝对星等 (MV) | 6.5[2] |
| 轨道[7] | |
| 绕行周期 (P) | 2.83774 d |
| 半长轴 (a) | 10.3 R☉[8] |
| 偏心率 (e) | 0.00 (assumed) |
| 倾斜角 (i) | 38[9]° |
| 近心点 历元 (T) | 2,442,767.4 HJD |
| 近心点幅角 (ω) (secondary) | 0.00 (assumed)° |
| 半振幅 (K1) (primary) | 52.6 km/s |
| 半振幅 (K2) (secondary) | 64.1 km/s |
| 详细资料 | |
| 成员 Aa | |
| 质量 | 1.0[8] M☉ |
| 半径 | 3.7[8] R☉ |
| 表面重力 (log g) | 3.30[5] |
| 温度 | 4,750[5] K |
| 金属量 [Fe/H] | −0.16[10] dex |
| 自转速度 (v sin i) | 39[9] km/s |
| 成员 Ab | |
| 质量 | 0.8[8] M☉ |
| 半径 | 1.1[8] R☉ |
| 表面重力 (log g) | 4.26[5] |
| 温度 | 5,500[5] K |
| 成员 B | |
| 质量 | 0.78[11] M☉ |
| 半径 | 0.78[11] R☉ |
| 表面重力 (log g) | 4.55[11] |
| 亮度 | 0.30[11] L☉ |
| 温度 | 4,829[11] K |
| 金属量 [Fe/H] | +0.10[10] dex |
| 自转速度 (v sin i) | 4.1[12] km/s |
| 年龄 | 2.2[3] Gyr |
| 其他命名 | |
| 参考数据库 | |
| SIMBAD | 资料 |
天囷增廿一（HR 1099）是位于黄道星座金牛座的一个三合星系统，位置在恒星天囷增十五（金牛座10）以北11′[15]。该系统有变星名称金牛座V711，而HR 1099是“亮星星表”中的恒星识别字。它的视星等亮度组合范围从5.71到5.94[6]，其亮度用肉眼隐约可见。基于视差量测，到该系统的距离为96.6光年[1]，但它正在以大约−15 km/s的径向速度向接近太阳系的方向漂移。
1822年，弗里德里希·冯·斯特鲁维发现该系统是一颗双星，其中A和B分量的角距离为5.4″。（2016年测量的角距离为6.7″。）[16]。拉尔夫·埃尔默·威尔逊在1953年确定，这对中较亮的成员A，具有可变的径向速度。1963年，奥林·查多克·威尔逊指出，相同的成员在钙H和K吸收线中显示出非常高的发射核[17]。奥林·查多克·威尔逊在1964年的后续观察表明，成员A的氢-α线完全处于发射状态，并且由于旋转而显示出适度的加宽。他发现成员B的恒星光谱分类为K3V，与一颗普通的K型主序星相匹配[18]。
1974年至1975年的观测表明，成员A是猎犬座RS型变星类的光谱联星恒星系统。考虑到它的平均星等约为5.9，它是这类已知较亮的变星之一[20]。没有观测到食，但确定了2.838天的轨道周期。大部分发射被发现来自这对中质量较大的成员[21]。1976年，弗雷泽·纳尔逊·欧文探测到了该联星的电波发射[22]。1978年使用HEAO1卫星证明它是软X射线源[23]。
这个双线光谱联星系统由一颗演化中的K型次巨星和一颗普通的G型主序星组成。这两颗恒星的轨道距离如此之近，以至于它们的潮汐效应使它们呈椭圆形。该次巨星正在填充其洛希瓣的大约80%[5]。次巨星的色球层是已知的最活跃的磁活动之一，有一个很深的对流区为磁发电机供电[24][4]。G型伴星不太活跃，有一个浅对流区[5]。
1980年，在一些与表面温度有关的光谱特征中发现了显著的变化，表明存在星斑[25]。多普勒成像证实这些多少与K型次巨星有关（它是第一颗对其表面进行多普勒成像的低温恒星[26]。）。证据表明，这些斑点首先出现在低纬度地区，然后向两极迁移[20]。这些斑点比太阳上的要大得多[5]，大约70%的斑点是在纬度高于50°的地方观测到的，尤其是在极地地区[9][24]。一个极地斑点已经存在了至少二十年[5]。
减去星斑的影响后，这两颗恒星的基线视星等分别为5.80和7.20[5]。长期监测表明，次巨星有两个活动周期，类似于11年的太阳周期。一个5.3±0.1 年周期与半球之间斑点区域的对称翻转有关。较长的15-16年周期是总斑点面积的周期性变化。恒星的整体磁场可能是相对于自转轴的进动[26]。
相关条目
参考资料
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进阶读物
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- Ransom, R. R.; et al, Possible Corotation of the Milliarcsecond Radio Structure of the Close Binary HR 1099, Astrophysical Journal, June 2002, 572 (1): 487–502, Bibcode:2002ApJ...572..487R, S2CID 120225374, doi:10.1086/340300 .
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