脉冲星中的Maia变量和其他异常现象

IF 2.6 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Frontiers in Astronomy and Space Sciences Pub Date : 2023-09-14 DOI:10.3389/fspas.2023.1266750
L. A. Balona
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引用次数: 2

摘要

来自TESS的高精度光度测量已经发现了500多颗恒星,它们位于δ Scuti和β造父变星不稳定带之间,这些不稳定带的频率很高。模型无法预测这些恒星的高脉动频率。这些异常变量可以与历史“Maia”变量相识别。结果表明,在相同的有效温度范围内,Maia变星的旋转速率与主序星和SPB变星的旋转速率没有差异。一些玛亚星的脉动频率与罗普星相似。这表明Maia星应该被认为是δ Scuti变量的延伸,其有效温度高达18000 K,而不是作为一个单独的类别。TESS的数据显示了一个连续的低频脉动恒星序列,连接着剑鱼座γ和SPB变量,这是模型无法预测的。事实上,在上层主序星中根本没有明确定义的不稳定带,这意味着需要任意选择有效温度和频率范围,以便分配特定的变异性类别。似乎存在一种混合的驱动机制,其中对流可能起着非常重要的作用。
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Maia variables and other anomalies among pulsating stars
High-precision photometry from TESS has revealed over 500 stars, located between the δ Scuti and β Cephei instability strips, which pulsate with high frequencies. Models do not predict high pulsation frequencies in these stars. These anomalous variables may be identified with the historical “Maia” variables. From the projected rotational velocities, it is shown that the rotation rates of Maia variables are no different from main sequence or SPB stars in the same effective temperature range. Some Maia stars pulsate at frequencies typical of roAp stars. It is shown that Maia stars should be considered an extension of δ Scuti variables to effective temperatures as high as 18,000 K, rather than as a separate class. The TESS data show a continuous sequence of low-frequency pulsating stars linking the γ Doradus and SPB variables, which is not predicted by the models. There are, in fact, no well-defined instability strips at all among upper main sequence stars, which means that arbitrary choices of effective temperature and frequency ranges need to be made in order to assign a particular variability class. It seems that a mixture of driving mechanisms is present in which convection may play a very important role.
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来源期刊
Frontiers in Astronomy and Space Sciences
Frontiers in Astronomy and Space Sciences ASTRONOMY & ASTROPHYSICS-
CiteScore
3.40
自引率
13.30%
发文量
363
审稿时长
14 weeks
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