天囷增廿一
  | |
| 觀測數據 曆元 J2000 分點 J2000 | |
|---|---|
| 星座 | 金牛座 |
| A | |
| 赤經 | 03h 36m 47.291s[1] |
| 赤緯 | 00° 35′ 15.94″[1] |
| 視星等 (V) | 5.91[2] |
| B | |
| 赤經 | 03h 36m 46.844s[3] |
| 赤緯 | 00° 35′ 15.93″[3] |
| 視星等 (V) | 8.79[2] |
| 特性 | |
| 光譜分類 | K2:Vnk[4] (K1 IV + G5 V + K3 V)[5] |
| 變星類型 | RS CVn[6] |
| 天體測定 | |
| A | |
| 徑向速度 (Rv) | −21.24+6.62 −[1] km/s |
| 自行 (μ) | 赤經：−32.894 mas/yr 赤緯：−161.772 mas/yr |
| 視差 (π) | 33.7528 ± 0.0866[1] mas |
| 距離 | 96.6 ± 0.2 ly (29.63 ± 0.08 pc) |
| 絕對星等 (MV) | 3.6[2] |
| B | |
| 徑向速度 (Rv) | −15.34±0.18[3] km/s |
| 自行 (μ) | 赤經：−34.359 mas/yr 赤緯：−138.137 mas/yr |
| 視差 (π) | 33.8664 ± 0.0226[3] mas |
| 距離 | 96.3 ± 0.2 ly (29.53 ± 0.02 pc) |
| 絕對星等 (MV) | 6.5[2] |
| 軌道[7] | |
| 繞行週期 (P) | 2.83774 d |
| 半長軸 (a) | 10.3 R☉[8] |
| 偏心率 (e) | 0.00 (assumed) |
| 傾斜角 (i) | 38[9]° |
| 近心點 曆元 (T) | 2,442,767.4 HJD |
| 近心點幅角 (ω) (secondary) | 0.00 (assumed)° |
| 半振幅 (K1) (primary) | 52.6 km/s |
| 半振幅 (K2) (secondary) | 64.1 km/s |
| 詳細資料 | |
| 成員 Aa | |
| 質量 | 1.0[8] M☉ |
| 半徑 | 3.7[8] R☉ |
| 表面重力 (log g) | 3.30[5] |
| 溫度 | 4,750[5] K |
| 金屬量 [Fe/H] | −0.16[10] dex |
| 自轉速度 (v sin i) | 39[9] km/s |
| 成員 Ab | |
| 質量 | 0.8[8] M☉ |
| 半徑 | 1.1[8] R☉ |
| 表面重力 (log g) | 4.26[5] |
| 溫度 | 5,500[5] K |
| 成員 B | |
| 質量 | 0.78[11] M☉ |
| 半徑 | 0.78[11] R☉ |
| 表面重力 (log g) | 4.55[11] |
| 亮度 | 0.30[11] L☉ |
| 溫度 | 4,829[11] K |
| 金屬量 [Fe/H] | +0.10[10] dex |
| 自轉速度 (v sin i) | 4.1[12] km/s |
| 年齡 | 2.2[3] Gyr |
| 其他命名 | |
| 參考資料庫 | |
| SIMBAD | 資料 |
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11′[15]。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[6]，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[1]，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5.4″。（2016年測量的角距離為6.7″。）[16]。拉爾夫·埃爾默·威爾遜在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[17]。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[18]。
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[20]。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[21]。1976年，弗雷澤·納爾遜·歐文探測到了該聯星的電波發射[22]。1978年使用HEAO1衛星證明它是軟X射線源[23]。
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%[5]。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[24][4]。G型伴星不太活躍，有一個淺對流區[5]。
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[25]。都卜勒成像證實這些多少與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[26]。）。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[20]。這些斑點比太陽上的要大得多[5]，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[9][24]。一個極地斑點已經存在了至少二十年[5]。
減去星斑的影響後，這兩顆恆星的基線視星等分別為5.80和7.20[5]。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[26]。
相關條目
參考資料
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進階讀物
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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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