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arXiv 1105.3072astro-ph.SRastro-ph.HE
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UCXB 4U 0614 +09中的快速光学和X射线可变性

Fast Optical and X-ray Variability in the UCXB 4U0614+09

Pasi Hakala, Phil Charles, Panu Muhli

备注：
6 pages, 4 figures, accepted for publication in MNRAS
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摘要：

本文介绍了对4U 0614 +091（猎户座V1055）的几年快速光学测光结果，4U 0614 + 091是一个候选的超紧凑X射线双星，很可能由一颗中子星和一颗简并次级星组成。我们发现了强吸积驱动的变化在所有时代的证据，表现为红噪音。这种闪烁在15-65分钟周期范围内在观察到的功率谱中产生瞬态峰值。只有在我们的12个光学数据集中的一个数据集中，我们才能看到使用红噪声模型无法重现的证据。这个51分钟的周期与Shahbaz等人（2008年）探测到的最强周期相吻合，因此可以作为该系统轨道周期的主要候选者。此外，我们还利用我们的数据和RXTE/ASM的全天X射线监测数据，为Machin等人（1990）发现的X射线与光通量的关系找到了一些初步的证据。我们提出，4U 0614 +09的复杂时间序列行为是吸积盘几何/结构在从几小时到几天的时间尺度上发生剧烈变化的结果。最后，我们要提请注意的解释，特别是吸积，来源的功率谱中的中等强度的峰值。许多这样的“周期”可能归因于数据中存在红噪声（即相关事件）。

英文摘要：

We present results from several years of fast optical photometry of 4U0614+091 (V1055 Orionis), a candidate ultracompact X-ray binary most likely consisting of a neutron star and a degenerate secondary. We find evidence for strong accretion-driven variability at all epochs, that manifests itself as red noise. This flickering produces transient peaks in the observed power spectrum in the 15-65 min period range. Only in one of our 12 optical datasets can we see evidence for a period that cannot be reproduced using the red noise model. This period of 51 minutes coincides with the strongest period detected by Shahbaz et al. (2008) and can thus be taken as the prime candidate for the orbital period of the system. Furthermore, we find some tentative evidence for the X-ray vs. optical flux anticorrelation discovered by Machin et al. (1990) using our data together with the all-sky X-ray monitoring data from RXTE/ASM. We propose that the complex time series behaviour of 4U0614+09 is a result of drastic changes in the accretion disc geometry/structure on time scales from hours to days. Finally we want to draw attention to the interpretation of moderately strong peaks in the power spectra of, especially accreting, sources. Many of such "periods" can probably be attributed to the presence of red noise (i.e. correlated events) in the data.

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