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A prevalence of dynamo-generated magnetic fields in the cores of intermediate-mass stars

机译：中等质量恒星核心中发电机产生的磁场的普遍性

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摘要

Magnetic fields play a part in almost all stages of stellar evolution(1). Most low-mass stars, including the Sun, show surface fields that are generated by dynamo processes in their convective envelopes(2,3). Intermediate-mass stars do not have deep convective envelopes(4), although 10 per cent exhibit strong surface fields that are presumed to be residuals from the star formation process(5). These stars do have convective cores that might produce internal magnetic fields(6), and these fields might survive into later stages of stellar evolution, but information has been limited by our inability to measure the fields below the stellar surface(7). Here we report the strength of dipolar oscillation modes for a sample of 3,600 red giant stars. About 20 per cent of our sample show mode suppression, by strong magnetic fields in the cores(8), but this fraction is a strong function of mass. Strong core fields occur only in red giants heavier than 1.1 solar masses, and the occurrence rate is at least 50 per cent for intermediate-mass stars (1.6-2.0 solar masses), indicating that powerful dynamos were very common in the previously convective cores of these stars.
机译：磁场几乎在恒星演化的所有阶段都起着作用（1）。大多数低质量恒星，包括太阳，在对流包层中都显示出由发电机过程产生的地表场（2,3）。中等质量恒星没有较深的对流包络线（4），尽管有10％的恒星表面场强，据推测是恒星形成过程的残余物（5）。这些恒星确实具有可能产生内部磁场的对流核（6），并且这些场可能幸存到恒星演化的后期阶段，但是由于我们无法测量恒星表面以下的场（7），信息受到了限制。在这里，我们报告了3,600个红色巨星样本的偶极子振荡模式的强度。我们的样本中约有20％会受到铁心中的强磁场的抑制（8），但这部分是质量的强大函数。强核心场仅在重于1.1太阳质量的红色巨星中发生，中等质量恒星（1.6-2.0太阳质量）的发生率至少为50％，这表明强对流子在以前的对流核中非常普遍。这些星星。

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  • 来源
    《Nature》 |2016年第7586期|364-367|共4页
  • 作者

    Stello Dennis; Cantiello Matteo; Fuller Jim; Huber Daniel; Garcia Rafael A.; Bedding Timothy R.; Bildsten Lars; Aguirre Victor Silva;

  • 作者单位

    Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia|Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark;

    Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA;

    Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA|CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA;

    Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia|Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark|SETI Inst, Mountain View, CA 94043 USA;

    Univ Paris Diderot, IRFU, SAp Ctr Saclay, Lab AIM,CEA,DSM,CNRS, F-91191 Gif Sur Yvette, France;

    Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia|Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark;

    Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA|Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA;

    Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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