天囷增廿一
天囷增廿一（HR 1099）是位于黄道星座金牛座的一个三合星系统，位置在恒星天囷增十五（金牛座10）以北11′[15]。该系统有变星名称金牛座V711，而HR 1099是“亮星星表”中的恒星识别字。它的视星等亮度组合范围从5.71到5.94[6]，其亮度用肉眼隐约可见。基于视差量测，到该系统的距离为96.6光年[1]，但它正在以大约−15 km/s的径向速度向接近太阳系的方向漂移。
  | |
| 观测数据 历元 J2000 分点 J2000 | |
|---|---|
| 星座 | 金牛座 |
| A | |
| 赤经 | 03h 36m 47.291s[1] |
| 赤纬 | 00° 35′ 15.94″[1] |
| 视星等 (V) | 5.91[2] |
| B | |
| 赤经 | 03h 36m 46.844s[3] |
| 赤纬 | 00° 35′ 15.93″[3] |
| 视星等 (V) | 8.79[2] |
| 特性 | |
| 光谱分类 | K2:Vnk[4] (K1 IV + G5 V + K3 V)[5] |
| 变星类型 | RS CVn[6] |
| 天体测定 | |
| A | |
| 径向速度 (Rv) | −21.24+6.62 −[1] km/s |
| 自行 (μ) | 赤经：−32.894 mas/yr 赤纬：−161.772 mas/yr |
| 视差 (π) | 33.7528 ± 0.0866[1] mas |
| 距离 | 96.6 ± 0.2 ly (29.63 ± 0.08 pc) |
| 绝对星等 (MV) | 3.6[2] |
| B | |
| 径向速度 (Rv) | −15.34±0.18[3] km/s |
| 自行 (μ) | 赤经：−34.359 mas/yr 赤纬：−138.137 mas/yr |
| 视差 (π) | 33.8664 ± 0.0226[3] mas |
| 距离 | 96.3 ± 0.2 ly (29.53 ± 0.02 pc) |
| 绝对星等 (MV) | 6.5[2] |
| 轨道[7] | |
| 绕行周期 (P) | 2.83774 d |
| 半长轴 (a) | 10.3 R☉[8] |
| 偏心率 (e) | 0.00 (assumed) |
| 倾斜角 (i) | 38[9]° |
| 近心点 历元 (T) | 2,442,767.4 HJD |
| 近心点幅角 (ω) (secondary) | 0.00 (assumed)° |
| 半振幅 (K1) (primary) | 52.6 km/s |
| 半振幅 (K2) (secondary) | 64.1 km/s |
| 详细资料 | |
| 成员 Aa | |
| 质量 | 1.0[8] M☉ |
| 半径 | 3.7[8] R☉ |
| 表面重力 (log g) | 3.30[5] |
| 温度 | 4,750[5] K |
| 金属量 [Fe/H] | −0.16[10] dex |
| 自转速度 (v sin i) | 39[9] km/s |
| 成员 Ab | |
| 质量 | 0.8[8] M☉ |
| 半径 | 1.1[8] R☉ |
| 表面重力 (log g) | 4.26[5] |
| 温度 | 5,500[5] K |
| 成员 B | |
| 质量 | 0.78[11] M☉ |
| 半径 | 0.78[11] R☉ |
| 表面重力 (log g) | 4.55[11] |
| 亮度 | 0.30[11] L☉ |
| 温度 | 4,829[11] K |
| 金属量 [Fe/H] | +0.10[10] dex |
| 自转速度 (v sin i) | 4.1[12] km/s |
| 年龄 | 2.2[3] Gyr |
| 其他命名 | |
| 参考资料库 | |
| SIMBAD | 资料 |
1822年，弗里德里希·冯·斯特鲁维发现该系统是一颗双星，其中A和B分量的角距离为5.4″。（2016年测量的角距离为6.7″。）[16]。拉尔夫·埃尔默·威尔逊在1953年确定，这对中较亮的成员A，具有可变的径向速度。1963年，奥林·查多克·威尔逊指出，相同的成员在钙H和K吸收线中显示出非常高的发射核[17]。奥林·查多克·威尔逊在1964年的后续观察表明，成员A的氢-α线完全处于发射状态，并且由于旋转而显示出适度的加宽。他发现成员B的恒星光谱分类为K3V，与一颗普通的K型主序星相匹配[18]。
1974年至1975年的观测表明，成员A是猎犬座RS型变星类的光谱联星恒星系统。考虑到它的平均星等约为5.9，它是这类已知较亮的变星之一[20]。没有观测到食，但确定了2.838天的轨道周期。大部分发射被发现来自这对中质量较大的成员[21]。1976年，弗雷泽·纳尔逊·欧文探测到了该联星的电波发射[22]。1978年使用HEAO1卫星证明它是软X射线源[23]。
这个双线光谱联星系统由一颗演化中的K型次巨星和一颗普通的G型主序星组成。这两颗恒星的轨道距离如此之近，以至于它们的潮汐效应使它们呈椭圆形。该次巨星正在填充其洛希瓣的大约80%[5]。次巨星的色球层是已知的最活跃的磁活动之一，有一个很深的对流区为磁发电机供电[24][4]。G型伴星不太活跃，有一个浅对流区[5]。
1980年，在一些与表面温度有关的光谱特征中发现了显著的变化，表明存在星斑[25]。都卜勒成像证实这些多少与K型次巨星有关（它是第一颗对其表面进行都卜勒成像的低温恒星[26]。）。证据表明，这些斑点首先出现在低纬度地区，然后向两极迁移[20]。这些斑点比太阳上的要大得多[5]，大约70%的斑点是在纬度高于50°的地方观测到的，尤其是在极地地区[9][24]。一个极地斑点已经存在了至少二十年[5]。
减去星斑的影响后，这两颗恒星的基线视星等分别为5.80和7.20[5]。长期监测表明，次巨星有两个活动周期，类似于11年的太阳周期。一个5.3±0.1 年周期与半球之间斑点区域的对称翻转有关。较长的15-16年周期是总斑点面积的周期性变化。恒星的整体磁场可能是相对于自转轴的进动[26]。
相关条目
编辑参考资料
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. doi:10.1051/0004-6361/202243940 . 已忽略未知参数|collaboration=(帮助) Gaia DR3 record for this source at VizieR. - ^ 2.0 2.1 2.2 2.3 Freund, S.; Robrade, J.; Schneider, P. C.; Schmitt, J. H. M. M., The stellar content of the XMM-Newton slew survey, Astronomy and Astrophysics, 2018, 614: A125, Bibcode:2018A&A...614A.125F, S2CID 59396964, arXiv:1712.07410 , doi:10.1051/0004-6361/201732009.
- ^ 3.0 3.1 3.2 3.3 3.4 Vallenari, A.; et al. Gaia Data Release 3. Summary of the content and survey properties. Astronomy & Astrophysics. 2022. arXiv:2208.00211 . doi:10.1051/0004-6361/202243940 . 已忽略未知参数
|collaboration=(帮助) Gaia DR3 record for this source at VizieR. - ^ 4.0 4.1 Gray, R. O.; et al, Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc—The Southern Sample, The Astronomical Journal, July 2006, 132 (1): 161–170, Bibcode:2006AJ....132..161G, S2CID 119476992, arXiv:astro-ph/0603770 , doi:10.1086/504637.
- ^ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 Lanza, A. F.; et al, Long-term starspot evolution, activity cycle, and orbital period variation of V711 Tauri (HR 1099), Astronomy and Astrophysics, August 2006, 455 (2): 595–606, Bibcode:2006A&A...455..595L, doi:10.1051/0004-6361:20064847.
- ^ 6.0 6.1 Samus, N. N.; et al, General Catalogue of Variable Stars, Astronomy Reports, 5.1, 2017, 61 (1): 80–88, Bibcode:2017ARep...61...80S, S2CID 125853869, doi:10.1134/S1063772917010085.
- ^ Strassmeier, K. G.; Bartus, J., Doppler imaging of stellar surface structure. XII. Rapid spot changes on the RS CVn binary V711 Tauri = HR 1099, Astronomy and Astrophysics, February 2000, 354: 537–550, Bibcode:2000A&A...354..537S.
- ^ 8.0 8.1 8.2 8.3 8.4 Donati, J. -F., Magnetic cycles of HR 1099 and LQ Hydrae, Monthly Notices of the Royal Astronomical Society, January 1999, 302 (3): 457–481, Bibcode:1999MNRAS.302..457D, doi:10.1046/j.1365-8711.1999.02096.x .
- ^ 9.0 9.1 9.2 Donati, J. -F.; et al, Dynamo processes and activity cycles of the active stars AB Doradus, LQ Hydrae and HR 1099, Monthly Notices of the Royal Astronomical Society, November 2003, 345 (4): 1145–1186, Bibcode:2003MNRAS.345.1145D, doi:10.1046/j.1365-2966.2003.07031.x .
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- ^ 11.0 11.1 11.2 11.3 11.4 Stassun K.G.; et al, The revised TESS Input Catalog and Candidate Target List, The Astronomical Journal, October 2019, 158 (4): 138, Bibcode:2019AJ....158..138S, S2CID 166227927, arXiv:1905.10694 , doi:10.3847/1538-3881/ab3467.
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进阶读物
编辑- Perdelwitz, V.; et al, Long-term variations in the X-ray activity of HR 1099, Astronomy & Astrophysics, August 2018, 616: A161, Bibcode:2018A&A...616A.161P, S2CID 55130058, arXiv:1806.03033 , doi:10.1051/0004-6361/201732222, A161.
- Osten, Rachel A.; et al, A Multiwavelength Perspective of Flares on HR 1099: 4 Years of Coordinated Campaigns, Astrophysical Journal Supplement Series, July 2004, 153 (1): 317–362, Bibcode:2004ApJS..153..317O, S2CID 119522693, arXiv:astro-ph/0402613 , doi:10.1086/420770.
- 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 .
- Ayres, Thomas R.; et al, Chandra, EUVE, HST, and VLA Multiwavelength Campaign on HR 1099: Instrumental Capabilities, Data Reduction, and Initial Results, Astrophysical Journal, March 2001, 549 (1): 554–577, Bibcode:2001ApJ...549..554A, S2CID 15938906, doi:10.1086/319051 .
- Brinkman, A. C.; et al, First light measurements with the XMM-Newton reflection grating spectrometers: Evidence for an inverse first ionisation potential effect and anomalous Ne abundance in the Coronae of HR 1099, Astronomy and Astrophysics, January 2001, 365: L324–L328, Bibcode:2001A&A...365L.324B, S2CID 15848464, arXiv:astro-ph/0011018 , doi:10.1051/0004-6361:20000047.
- Audard, M.; et al, The XMM-Newton view of stellar coronae: Flare heating in the coronae of HR 1099, Astronomy and Astrophysics, January 2001, 365: L318–L323, Bibcode:2001A&A...365L.318A, doi:10.1051/0004-6361:20000085.
- Vogt, Steven S.; et al, Doppler Imagery of the Spotted RS CVn Star HR 1099 (= V711 Tau) from 1981 - 1992, Astrophysical Journal Supplement Series, April 1997, 121: 547, Bibcode:1997astro.ph..4191V, S2CID 119515171, arXiv:astro-ph/9704191 , doi:10.1086/313195.
- Trigilio, C.; et al, VLBI observations of a strong radio flare in HR 1099, Monthly Notices of the Royal Astronomical Society, February 1993, 260 (4): 903–907, Bibcode:1993MNRAS.260..903T, doi:10.1093/mnras/260.4.903 .
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