金牛座CQ
觀測資料 曆元 J2000.0 | |
---|---|
星座 | 金牛座 |
星官 | |
赤經 | 05h 35m 58.467s[2] |
赤緯 | 24° 44′ 54.09″[2] |
視星等(V) | 10.48[3] () 8.7 to 12.25[4] |
特性 | |
演化阶段 | 主序前星[5] |
光谱分类 | F5IVe[6] |
B−V 色指数 | 0.696+0.091 −[3] |
变星类型 | 獵戶型變星[4] |
天体测定 | |
徑向速度 (Rv) | 22.60+2.7 −[7] km/s |
自行 (μ) | 赤经:2.987 mas/yr 赤纬:−26.364 mas/yr |
视差 (π) | 6.6946 ± 0.0600[2] mas |
距离 | 487 ± 4 ly (149 ± 1 pc) |
绝对星等 (MV) | 5.92[8] |
詳細資料 | |
質量 | 1.67[9] M☉ |
半徑 | 1.7[10] R☉ |
表面重力 (log g) | 4.0[8] |
亮度 | 10[9] L☉ |
溫度 | 6,900[9] K |
金属量 [Fe/H] | +0.14[11] dex |
自轉速度 (v sin i) | 105.0+5.0 −[6] km/s |
年齡 | 10[9] Myr |
其他命名 | |
參考資料庫 | |
SIMBAD | 资料 |
金牛座CQ是位於黃道星座金牛座的一顆年輕變星[5]。它太微弱了,視星等的範圍在 8.7 to 12.25[4],因此肉眼無法直接看到。基於視差測量,這顆恆星的距離大約是487光年,並以~23Km/s的徑向速度遠離太陽系[7]。它似乎是T-星協金牛4的成員[8]。金牛座CQ離黃道足夠近,因此會發生月掩星的天象[13]。
這顆恆星在1948年被阿爾朱基諾夫(Artjukinov,sp?)和1949年被庫諾·霍夫邁斯特獨立報導為一顆變星[14]。霍夫邁斯特將其歸類為類似御夫座RW變星,亮度範圍從8.7等到10.5等[15], 使其成為該類型中最明亮的成員之一[14]。G·H·赫比格在1960年發現了這顆恆星的光譜為F2[16],到1973年,它被歸類為獵戶型變星的金牛T星。 [17]。在1968年,沃爾德瑪律·格茨和W.溫澤爾發現來自系統的微弱藍光發射[18]。
1973年該系統的光譜圖像在F型恆星上顯示雙發射線[19]。它被IRAS發現為紅外源,並與星雲相關聯,這使得它能夠在1994年被P. S. Thé和同事編目為赫比格Ae/Be星[20]。恆星經歷不規則的亮度降低,在其他方面類似於大陵五型變星。 它有一個不均勻的吸積盤繞行著,這是發射線的來源[21]。
金牛座CQ是一顆主序前星,恆星分類為F5IVe[6]。它的質量是太陽的1.67倍,輻射亮度是太陽的10倍,表面有效溫度為6,900K。這顆恆星大約有1,000萬年的歷史[9],並且以105km/s的投影旋轉速度旋轉[6]。旨在再現星周盤分佈的模擬表明,一顆距離為,質量為 ~20 AUMJ的 6–9 行星嵌入盤中,正在圍繞該恆星運行[9]。2018年的近紅外觀測顯示,圓盤中存在螺旋結構,這與軌道行星的存在一致。然而,並沒有發現任何行星[22]。
原行星系統
在2000年,甚大天線陣的觀測證明了圍繞恆星運行的大質量原行星盤的範圍,估計盤面中的灰塵質量為×10−4 M☉ 1.5[23]。量測表明,金牛座CQ周圍圓盤中的塵粒已生長到最大約一釐米大小[24],與主星相距AU以外的晶粒尺寸逐漸减小 40 [25]。來自阿塔卡瑪大型毫米及次毫米波陣列的資料顯示,內盤中有一個裡面的氣體和灰塵都耗盡了的空腔[9]。孤立的、厚厚的塵埃雲隨機地遮蔽著這顆恆星[26]。
在2022年,探測到原行星盤中的四個旋臂。懷疑是被一顆位於偏心傾斜軌道上,尚未發現的行星擾亂了圓盤的形狀[27]。
參考資料
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|url=
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進階讀物
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