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 | |
| 演化階段 | 主序前星[5] |
| 光譜分類 | F5IVe[6] |
| B−V 色指數 | 0.696+0.091 −[3] |
| 變星類型 | 獵戶型變星[4] |
| 天體測定 | |
| 徑向速度 (Rv) | 22.60+2.7 −[7] km/s |
| 自行 (μ) | 赤經：2.987 mas/yr 赤緯：−26.364 mas/yr |
| 視差 (π) | 6.6946 ± 0.0600[2] mas |
| 距離 | 487 ± 4 ly (149 ± 1 pc) |
| 絕對星等 (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 |
| 金屬量 [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 | 資料 |
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~20 AU，質量為6–9 MJ的行星嵌入盤中，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
[編輯]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1.5×10−4 M☉[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40 AU以外的晶粒尺寸逐漸減小[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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. doi:10.1051/0004-6361/202039657 . 已忽略未知參數|collaboration=(幫助) (勘誤: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR. - ^ 3.0 3.1 Anderson, E.; Francis, Ch., XHIP: An extended hipparcos compilation, Astronomy Letters, 2012, 38 (5): 331, Bibcode:2012AstL...38..331A, S2CID 119257644, arXiv:1108.4971 , doi:10.1134/S1063773712050015.
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進階讀物
[編輯]- Safonov, Boris S.; et al, Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light, The Astronomical Journal, January 2022, 163 (1): 31, Bibcode:2022AJ....163...31S, S2CID 242757117, arXiv:2111.02726 , doi:10.3847/1538-3881/ac36cb, 31.
- Wölfer, L.; et al, A highly non-Keplerian protoplanetary disc. Spiral structure in the gas disc of CQ Tau, Astronomy & Astrophysics, April 2021, 648, Bibcode:2021A&A...648A..19W, S2CID 228064514, arXiv:2012.04680 , doi:10.1051/0004-6361/202039469, A19.
- Assani, K., Variability in the Gas and Dust Emission of the UX Orioni Star CQ Tau, Bulletin of the American Astronomical Society, January 2020, 52 (1), Bibcode:2020AAS...23545101A.
- Ubeira Gabellini, Maria Giulia, The gas and dust disk around the CQ Tau pre-main sequence star, Protoplanetary disks seen through the eyes of new-generation high-resolution instruments. Proceedings of the conference held 25–28 June 2018 in Rome, Italy, December 2018: 30, Bibcode:2018ppd..confE..30U, doi:10.5281/zenodo.1893261.
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