天囷增廿一

天囷增廿一（HR 1099）是位於黃道星座金牛座的一個三合星系統，位置在恆星天囷增十五（金牛座10）以北6997319977029532294♠11′。該系統有變星名稱金牛座V711，而HR 1099是「亮星星表」中的恆星識別字。它的視星等亮度組合範圍從5.71到5.94，其亮度用肉眼隱約可見。基於視差量測，到該系統的距離為96.6光年，但它正在以大約−15 km/s的徑向速度向接近太陽系的方向漂移。 1822年，弗里德里希·馮·斯特魯維發現該系統是一顆雙星，其中A和B分量的角距離為6995261799387799150♠5.4″。（2016年測量的角距離為6995324825166343389♠6.7″。）。拉爾夫·埃爾默·威爾遜（英语：Ralph Elmer Wilson）在1953年確定，這對中較亮的成員A，具有可變的徑向速度。1963年，奧林·查多克·威爾遜（英语：Olin Chaddock Wilson）指出，相同的成員在鈣H和K吸收線中顯示出非常高的發射核。奧林·查多克·威爾遜在1964年的後續觀察表明，成員A的氫-α線完全處於發射狀態，並且由於旋轉而顯示出適度的加寬。他發現成員B的恆星光譜分類為K3V，與一顆普通的K型主序星相匹配。 1974年至1975年的觀測表明，成員A是獵犬座RS型變星類的光譜聯星恆星系統。考慮到它的平均星等約為5.9，它是這類已知較亮的變星之一。沒有觀測到食，但確定了2.838天的軌道週期。大部分發射被發現來自這對中質量較大的成員。1976年，弗雷澤·納爾遜·歐文（英语：Frazer Nelson Owen）探測到了該聯星的電波發射。1978年使用HEAO1（英语：High Energy Astronomy Observatory 1）衛星證明它是軟X射線源。 這個雙線光譜聯星系統由一顆演化中的K型次巨星和一顆普通的G型主序星組成。這兩顆恆星的軌道距離如此之近，以至於它們的潮汐效應使它們呈橢圓形。該次巨星正在填充其洛希瓣的大約80%。次巨星的色球層是已知的最活躍的磁活動之一，有一個很深的對流區為磁發電機供電。G型伴星不太活躍，有一個淺對流區。 1980年，在一些與表面溫度有關的光譜特徵中發現了顯著的變化，表明存在星斑。都卜勒成像（英语：Doppler imaging）證實這些多少與K型次巨星有關（它是第一顆對其表面進行都卜勒成像的低溫恆星。）。證據表明，這些斑點首先出現在低緯度地區，然後向兩極遷移。這些斑點比太陽上的要大得多，大約70%的斑點是在緯度高於50°的地方觀測到的，尤其是在極地地區。一個極地斑點已經存在了至少二十年。 减去星斑的影響後，這兩顆恆星的基線視星等分別為5.80和7.20。長期監測表明，次巨星有兩個活動週期，類似於11年的太陽週期。一個7008167255280000000♠5.3±0.1 年週期與半球之間斑點區域的對稱翻轉有關。較長的15-16年週期是總斑點面積的週期性變化。恆星的整體磁場可能是相對於自轉軸的進動。 白羊座UX Vallenari, A.; et al. 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