WHY ARE THE SECONDARY STARS IN POLARS SO NORMAL?

THOMAS E. HARRISON; STEVE B. HOWELL; PAULA SZKODY; FRANCE A. CORDOVA

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WHY ARE THE SECONDARY STARS IN POLARS SO NORMAL?

机译：极地的次级星为什么如此正常？

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We have used NIRSPEC on Keck II to obtain K-band spectroscopy of several magnetic cataclysmic variables. These data reveal that the secondary stars in these binary systems have spectra that are consistent with normal, late-type dwarfs in both their atomic and molecular line strengths, as well as in the slopes of their continua. This result is in stark contrast to the infrared spectra of their nonmagnetic cousins, nearly all of which show peculiar abundances, especially of CNO species and their isotopes. It appears that the evolutionary path taken by the secondary stars in magnetic systems differs from that for the nonmagnetic systems. We discuss the implications of this result.

机译：我们已经在Keck II上使用NIRSPEC来获得几个磁催化变量的K波段光谱。这些数据表明，这些双星系统中的次要恒星在原子和分子谱线强度以及连续谱的斜率方面均具有与正常的晚型矮星一致的光谱。这一结果与其非磁性表亲的红外光谱形成了鲜明的对比，它们几乎全部显示出奇特的丰度，尤其是CNO物种及其同位素。看来，次级恒星在磁系统中所采取的演化路径与非磁系统中的演化路径不同。我们讨论此结果的含义。

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《The Astrophysical journal》 |2005年第2pt2期|p.L123-L126|共4页
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THOMAS E. HARRISON; STEVE B. HOWELL; PAULA SZKODY; FRANCE A. CORDOVA;
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1. WHY ARE THE SECONDARY STARS IN POLARS SO NORMAL? [J] . THOMAS E. HARRISON, STEVE B. HOWELL, PAULA SZKODY, The Astrophysical journal . 2005,第2Pt2期

机译：极地的次级星为什么如此正常？
2. Observations of the Polar ST Leonis Minoris during an Extreme Low State: Identification of the Secondary Star [J] . David R. Ciardi, Steve B. Howell, V. S. Dhillon, Publications of the Astronomical Society of the Pacific . 1998,第751期

机译：极低状态下极地ST Leonis Minoris的观测：次级恒星的识别
3. On the fluorine nucleosynthesis in AGB stars in the light of the $^{19} F {(p, α)}^{16}$ O and $^{19} F {(α, p)}^{22}$ Ne reaction rate measured via THM [J] . S. Palmerini, G. D’Agata, M. La Cognata, International Journal of Modern Physics: Conference Series . 2019,第a期

机译：在AGB恒星中的氟核结核鉴于<！ - $ {MATHJAX TEX-AMS-MML_HTMLORMML} - > $19F（p ，α）16o和<！ - $ {mathjax tex-ams-mml_htmlormml} - >19f < mo class =“mathclass-open”弹力=“假”>（ α，p ）22通过THM测量的NE反应速率$
4. Chemical composition of secondary stars in LMXBs: implications on the progenitors of black holes and neutron stars [C] . Jonay I. Gonzalez Hernandez Conference on Interacting binaries:accretion, evolution, outcomes . 2005

机译：LMXBS中次生恒星的化学成分：对黑洞和中子恒星祖的影响
5. Abundance analysis of normal and mercury-manganase type late-B stars from optical spectra. [D] . Allen, Caroline Sarah. 1998

机译：从光谱中正常和汞锰酶型晚B星的丰度分析。
6. Protocol: a fast comprehensive and reproducible one-step extraction method for the rapid preparation of polar and semi-polar metabolites lipids proteins starch and cell wall polymers from a single sample [O] . Mohamed A. Salem, Jessica Jüppner, Krzysztof Bajdzienko, 2016

机译：方案：一种快速全面且可重现的一步提取方法用于从单个样品中快速制备极性和半极性代谢物脂质蛋白质淀粉和细胞壁聚合物
7. Why Are The Secondary Stars in Polars So Normal? [O] . Harrison, T E, Howell, S B, Szkody, P, 2005

机译：为什么极地中的次级恒星如此正常？
8. Ross Sea Oceanographic Data, 1983-1987: USCGC GLACIER, January-February 1983; USCGC POLAR SEA, January-February 1984; USCGC POLAR STAR, February 1984; USCGC POLAR SEA, February 1987 [R] . Jacobs, S. S., Haines, W. E., Ardai, J. L., 1989

机译：罗斯海洋海洋学数据，1983-1987：UsCGC GLaCIER，1983年1月至2月; UsCGC pOLaR sEa，1984年1月至2月; UsCGC pOLaR sTaR，1984年2月; UsCGC pOLaR sEa，1987年2月

WHY ARE THE SECONDARY STARS IN POLARS SO NORMAL?

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