金牛座BP：修订间差异
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<ref name=MAST>{{cite web |title=MAST: Barbara A. Mikulski Archive for Space Telescopes |url=https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html |publisher=Space Telescope Science Institute |access-date=8 December 2021}}</ref> |
<ref name=MAST>{{cite web |title=MAST: Barbara A. Mikulski Archive for Space Telescopes |url=https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html |publisher=Space Telescope Science Institute |access-date=8 December 2021 |archive-date=2023-03-27 |archive-url=https://web.archive.org/web/20230327144653/https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html |dead-url=no }}</ref> |
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<ref name=SIMBAD>{{cite simbad |title=V* BP Tau}}</ref> |
<ref name=SIMBAD>{{cite simbad |title=V* BP Tau}}</ref> |
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2023年8月15日 (二) 11:55的版本
| 觀測資料 曆元 J2000 | |
|---|---|
| 星座 | 金牛座 |
| 星官 | |
| 赤經 | 04h 19m 15.8343s[2] |
| 赤緯 | +29° 06′ 26.9295″[2] |
| 視星等（V） | 12.12 |
| 特性 | |
| 演化阶段 | 主序前星 |
| 光谱分类 | K5 |
| 视星等 (G) | 11.460[3] |
| 变星类型 | T Tau |
| 天体测定 | |
| 徑向速度 (Rv) | 15.76+0.13 − km/s |
| 自行 (μ) | 赤经：8.889[3] mas/yr 赤纬：-26.011[3] mas/yr |
| 视差 (π) | 7.8494 ± 0.0362[3] mas |
| 距离 | 416 ± 2 ly (127.4 ± 0.6 pc) |
| 詳細資料 | |
| 質量 | 1.24+0.25 −0.32[4] M☉ |
| 半徑 | 2.0[5] R☉ |
| 表面重力 (log g) | 4.32+0.14 −[6] |
| 亮度 | 0.93[5] L☉ |
| 溫度 | 3640+94 −92[6] K |
| 自轉速度 (v sin i) | 11.4+0.25 −0.55[6] km/s |
| 年齡 | 6+4 −[4] Myr |
| 其他命名 | |
| 參考資料庫 | |
| SIMBAD | 资料 |
金牛座BP是在金牛座的一顆年輕的金牛T星，屬於金牛座分子雲，距離太陽大約416 光年。
性能
金牛座BP仍然以9×10−10 太陽質量和1.6×10−7 太陽質量/年的低速率吸積質量[7]，正如落入物質產生的X射線所證明的那樣[8]，並且可能仍在旋轉過程中[9]。它的色球磁場相當強，為2.5+0.15
−0.16千高斯[6]，並含有強的非偶極子成分[10]。這顆恆星有40%的光度是通過吸積釋放的能量產生[5]。
疑似伴星
金牛座BP有兩個可疑的恆星伴星，預計分離3.00和5.45 弧秒[11]。不過現在已經被蓋亞任務的數據證明，是與金牛座BP無關的背景恆星[12][13]。
原行星系統
這顆恆星被原行星盤包圍。圓盤中強烈的在消耗碳和一氧化碳[14]。
| 成員 (依恆星距離) |
质量 | 半長軸 (AU) |
轨道周期 (天) |
離心率 | 傾角 | 半径 |
|---|---|---|---|---|---|---|
| 原行星盤 | 0 — 120[15] AU | 30[14]° | — | |||
變異性
由於不穩定的吸積而產生強烈的耀斑，與恆星磁場控制，使金牛座BP有著不同的亮度[5]。光變曲線週期在 6.1 至 7.6 天之間變化，並且已知也有沒有變化的靜止週期[16]。
參考資料
- ^ MAST: Barbara A. Mikulski Archive for Space Telescopes. Space Telescope Science Institute. [8 December 2021]. （原始内容存档于2023-03-27）.
- ^ 2.0 2.1 V* BP Tau. SIMBAD. 斯特拉斯堡天文資料中心.
- ^ 3.0 3.1 3.2 3.3 Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533
. doi:10.1051/0004-6361/202039657 . 已忽略未知参数|collaboration=(帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR. - ^ 4.0 4.1 Simon, M.; Dutrey, A.; Guilloteau, S., Dynamical Masses of T Tauri Stars and Calibration of Pre–Main‐Sequence Evolution, The Astrophysical Journal, 2000, 545 (2): 1034–1043, Bibcode:2000ApJ...545.1034S, S2CID 18064837, arXiv:astro-ph/0008370 , doi:10.1086/317838
- ^ 5.0 5.1 5.2 5.3 Errico, L.; Lamzin, S. A.; Vittone, A. A., UV spectra of T Tauri stars from the HST and IUE satellites: BP Tau, Astronomy & Astrophysics, 2001, 377 (2): 557–565, Bibcode:2001A&A...377..557E, doi:10.1051/0004-6361:20011108
- ^ 6.0 6.1 6.2 6.3 Flores, C.; Connelley, M. S.; Reipurth, B.; Boogert, A., Measuring the Magnetic Field of Young Stars Using iSHELL Observations: BP Tau and V347 Aur, The Astrophysical Journal, 2019, 882 (2): 75, Bibcode:2019ApJ...882...75F, S2CID 201645503, arXiv:1908.08583 , doi:10.3847/1538-4357/ab35d4
- ^ Long, M.; Romanova, M. M.; Kulkarni, A. K.; Donati, J.-F., Global 3D simulations of disc accretion on to the classical T Tauri star BP Tauri, Monthly Notices of the Royal Astronomical Society, 2010, 413 (2): 1061–1071, S2CID 55134816, arXiv:1009.3300 , doi:10.1111/j.1365-2966.2010.18193.x
- ^ Schmitt, J. H. M. M.; Robrade, J.; Ness, J.-U.; Favata, F.; Stelzer, B., X-rays from accretion shocks in T Tauri stars: The case of BP Tau, Astronomy & Astrophysics, 2005, 432 (2): L35–L38, Bibcode:2005A&A...432L..35S, S2CID 2457531, arXiv:astro-ph/0503144 , doi:10.1051/0004-6361:200500014
- ^ Ireland, Lewis G.; Zanni, Claudio; Matt, Sean P.; Pantolmos, George, Magnetic Braking of Accreting T Tauri Stars: Effects of Mass Accretion Rate, Rotation, and Dipolar Field Strength, The Astrophysical Journal, 2020, 906: 4, S2CID 226236865, arXiv:2011.01087 , doi:10.3847/1538-4357/abc828
- ^ Long, Min; Romanova, Marina M.; Lamb, Frederick K., Accretion onto stars with octupole magnetic fields: Matter flow, hot spots and phase shifts, New Astronomy, 2009, 17 (2): 232–245, Bibcode:2012NewA...17..232L, S2CID 119113916, arXiv:0911.5455 , doi:10.1016/j.newast.2011.08.001
- ^ Itoh, Yoichi; Tamura, Motohide; Hayashi, Masahiko; Oasa, Yumiko; Hayashi, Saeko S.; Fukagawa, Misato; Kudo, Tomoyuki; Mayama, Satoshi; Ishii, Miki; Pyo, Tae-Soo; Yamashita, Takuya; Morino, Junichi. Near-Infrared Spectroscopy of Faint Companions around Young Stellar Objects Associated with the Taurus Molecular Cloud. Publications of the Astronomical Society of Japan. 2008, 60 (2): 209–218. Bibcode:2008PASJ...60..209I. doi:10.1093/pasj/60.2.209 .
- ^ Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533 . doi:10.1051/0004-6361/202039657 . 已忽略未知参数
|collaboration=(帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR. - ^ Brown, A. G. A.; et al. Gaia Early Data Release 3: Summary of the contents and survey properties. Astronomy & Astrophysics. 2021, 649: A1. Bibcode:2021A&A...649A...1G. S2CID 227254300. arXiv:2012.01533 . doi:10.1051/0004-6361/202039657 . 已忽略未知参数
|collaboration=(帮助) (勘误: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR. - ^ 14.0 14.1 Kama, M.; Bruderer, S.; Carney, M.; Hogerheijde, M.; Van Dishoeck, E. F.; Fedele, D.; Baryshev, A.; Boland, W.; Güsten, R.; Aikutalp, A.; Choi, Y.; Endo, A.; Frieswijk, W.; Karska, A.; Klaassen, P.; Koumpia, E.; Kristensen, L.; Leurini, S.; Nagy, Z.; Perez Beaupuits, J. -P.; Risacher, C.; Van Der Marel, N.; Van Kempen, T. A.; Van Weeren, R. J.; Wyrowski, F.; Yıldız, U. A. Observations and modelling of CO and [C I] in protoplanetary disks. First detections of [C I] and constraints on the carbon abundance. Astronomy and Astrophysics. 2016, 588: 588. Bibcode:2016A&A...588A.108K. S2CID 53941444. arXiv:1601.01449 . doi:10.1051/0004-6361/201526791.
- ^ Dutrey, A.; Guilloteau, S.; Simon, M. The BP Tau disk: A missing link between Class II and III objects?. Astronomy and Astrophysics. 2003, 402 (3): 1003. Bibcode:2003A&A...402.1003D. doi:10.1051/0004-6361:20030317 .
- ^ Simon, Theodore; Vrba, Frederick J.; Herbst, William. The Ultraviolet and Visible Light Variability of BP Tauri: Possible Clues for the Origin of T Tauri Star Activity. The Astronomical Journal. 1990, 100: 1957. Bibcode:1990AJ....100.1957S. doi:10.1086/115651.