普瑞茲畢爾斯基星
普瑞兹毕尔斯基星,又称HD 101065或半人马座V816,是一种快速振荡Ap星,距离太阳 355光年(109秒差距),位于半人马座的南天球。
历史
1961年,波兰-澳大利亚天文学家安东尼·普瑞兹毕尔斯基发现这个恒星有不适用于恒星分类标准框架的特殊光谱。[13][14]普瑞兹毕尔斯基发现观测表明这个恒星的光谱中的铁和镍含量异常低,但如锶、钬、铌、钪、钇、铯、钕、镨、钍、镱和铀等不寻常元素的含量更高。事实上,起初普瑞兹毕尔斯基根本怀疑光谱中是否存在铁。现代研究表明,普瑞兹毕尔斯基星中的铁系元素丰度略低于正常水平,但镧系元素和其它不寻常的元素非常丰富。[6]
普瑞兹毕尔斯基星中也检测到如锕、镤、镎、钚、镅、锔、锫、锎和锿等多种短寿命的锕系元素,其中锿的最长寿同位素的半衰期只有472天。该恒星中也有放射性元素锝和钷的存在。[15]
相较于邻近的恒星,HD 101065的本动速度较高,为23.8 ± 1.9 km/s。[8]
假设
由于普瑞兹毕尔斯基星的性质特殊,对于为什么会发生这些奇怪的性质有许多假设。一个理论称这个恒星含有某些位于稳定岛的长寿命核素(例如298Fl),而这些检测到的短寿命锕系元素是这些核素的衰变产物,与它们的母同位素存在长期平衡。[16][17]
性质
HD 101065是快速振荡Ap星(roAP)这一类恒星的原型。1978年,人们发现它会以12.15分钟的周期光度脉动。[18]
人们还发现了普瑞兹毕尔斯基星的一个潜在伴星,是一个距离它8角秒的14等星(红外线波段)。这可能意味着这两个恒星的距离只有7014149597870700000♠1,000 AU(0.02光年)。[19]然而,盖亚任务表明虽然这两个恒星在我们看来非常近,但我们与第二个恒星之间的实际距离是7002890000000000000♠890±90光年,这意味着我们与它的距离比我们离普瑞兹毕尔斯基星的距离还要远两倍以上。[20]
参见
参考资料
- ^ Kurtz, Don; Wegner, Gary. The nature of Przybylski's star: an Ap star model inferred from the light variations and temperature. The Astrophysical Journal. September 1979, 232: 510–519 [2021-12-04]. doi:10.1086/157310. (原始内容存档于2021-12-04).
- ^ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H. J.; et al. Gaia Data Release 2. Summary of the contents and survey properties. Astronomy & Astrophysics. 2018. Bibcode:2018A&A...616A...1G. arXiv:1804.09365
. doi:10.1051/0004-6361/201833051. VizieR中此天体在盖亚望远镜第二批数据发布的5372587514128271232 记录
- ^ 3.0 3.1 Samus, N. N.; Durlevich, O. V.; et al. VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013). VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 2009, 1: B/gcvs. Bibcode:2009yCat....102025S.
- ^ Renson, P.; Manfroid, J. Catalogue of Ap, Hg Mn and Am stars. Astronomy and Astrophysics. 2009, 498 (3): 961. Bibcode:2009A&A...498..961R. doi:10.1051/0004-6361/200810788
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- ^ 5.0 5.1 Wegner, G. On the reddening and the effective temperature of HD 101065. Monthly Notices of the Royal Astronomical Society. 1976, 177: 99–108. Bibcode:1976MNRAS.177...99W. doi:10.1093/mnras/177.1.99
.
- ^ 6.0 6.1 Hubrig, S.; Järvinen, S. P.; Madej, J.; Bychkov, V. D.; Ilyin, I.; Schöller, M.; Bychkova, L. V. Magnetic and pulsational variability of Przybylski's star (HD 101065). Monthly Notices of the Royal Astronomical Society. 2018, 477 (3): 3791. Bibcode:2018MNRAS.477.3791H. S2CID 55698015. arXiv:1804.07260
. doi:10.1093/mnras/sty889.
- ^ Gontcharov, G. A. Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system. Astronomy Letters. 2006, 32 (11): 759–771. Bibcode:2006AstL...32..759G. S2CID 119231169. arXiv:1606.08053
. doi:10.1134/S1063773706110065.
- ^ 8.0 8.1 8.2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M., A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun, Monthly Notices of the Royal Astronomical Society, January 2011, 410 (1): 190–200, Bibcode:2011MNRAS.410..190T, S2CID 118629873, arXiv:1007.4883
, doi:10.1111/j.1365-2966.2010.17434.x
- ^ Shulyak, D.; Ryabchikova, T.; Kildiyarova, R.; Kochukhov, O. Realistic model atmosphere and revised abundances of the coolest Ap star HD 101065. Astronomy and Astrophysics. 2010, 520: A88. Bibcode:2010A&A...520A..88S. S2CID 53538833. arXiv:1004.0246
. doi:10.1051/0004-6361/200913750.
- ^ 10.0 10.1 Cowley, C. R.; Ryabchikova, T.; Kupka, F.; Bord, D. J.; Mathys, G.; Bidelman, W. P. Abundances in Przybylski's star (PDF). Monthly Notices of the Royal Astronomical Society. 2000, 317 (2): 299–309. Bibcode:2000MNRAS.317..299C. doi:10.1046/j.1365-8711.2000.03578.x
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- ^ Przybylski, A. Is iron present in the atmosphere of HD 101065. Monthly Notices of the Royal Astronomical Society. January 1977, 178 (2): 71–84. Bibcode:1977MNRAS.178...71P. doi:10.1093/mnras/178.2.71
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- ^ [ V* V816 Cen]. SIMBAD. 斯特拉斯堡天文資料中心.
- ^ Przybylski, A.; Kennedy, P. Morris. The Spectrum of HD 101065. Publications of the Astronomical Society of the Pacific. August 1963, 75 (445): 349–353. Bibcode:1963PASP...75..349P. doi:10.1086/127965
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- ^ Powell, C. S.; Wright, J. The Strangest (and Second-Strangest) Star in the Galaxy. Discover. 2017-06-30 [2017-09-10]. (原始内容存档于2019-11-05).
- ^ Gopka, V. F.; Yushchenko, A. V.; Yushchenko, V. A.; Panov, I. V.; Kim, Ch. Identification of absorption lines of short half-life actinides in the spectrum of Przybylski's star (HD 101065). Kinematics and Physics of Celestial Bodies. 2008-05-15, 24 (2): 89–98. Bibcode:2008KPCB...24...89G. S2CID 120526363. doi:10.3103/S0884591308020049.
- ^ Jason Wright. Przybylski's Star III: Neutron Stars, Unbinilium, and aliens. 2017-03-16 [2018-07-31]. (原始内容存档于2021-12-12).
- ^ V. A. Dzuba; V. V. Flambaum; J. K. Webb. Isotope shift and search for metastable superheavy elements in astrophysical data. Physical Review A. 2017, 95 (6): 062515. Bibcode:2017PhRvA..95f2515D. S2CID 118956691. arXiv:1703.04250
. doi:10.1103/PhysRevA.95.062515.
- ^ Kurtz, D. W. 12.15 Minute Light Variations in Przybylski's Star, HD 101065. Information Bulletin on Variable Stars. 1978, 1436: 1. Bibcode:1978IBVS.1436....1K.
- ^ Schöller, M.; Correia, S.; Hubrig, S.; Kurtz, D. W. Multiplicity of rapidly oscillating Ap stars. Astronomy & Astrophysics. 2012, 545: A38. Bibcode:2012A&A...545A..38S. S2CID 119311263. arXiv:1208.0480
. doi:10.1051/0004-6361/201118538.
- ^ Brown, A. G. A.; Vallenari, A.; Prusti, T.; de Bruijne, J. H. J.; et al. Gaia Data Release 2. Summary of the contents and survey properties. Astronomy & Astrophysics. 2018. Bibcode:2018A&A...616A...1G. arXiv:1804.09365
. doi:10.1051/0004-6361/201833051. VizieR中此天体在盖亚望远镜第二批数据发布的5372587509831616384 记录
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