arXiv 1406.36032014-06-13astro-ph.SR

从分离的白矮星双星的引力波数据和食定时测量潮汐和双星参数

Measuring tides and binary parameters from gravitational wave data and eclipsing timings of detached white dwarf binaries

Sweta Shah, Gijs Nelemans

备注：: 10 pages, 3 figures, Accepted for publication in ApJ
DOI：: 10.1088/0004-637X/791/2/76

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摘要：

本文从探测白矮星潮汐效应的角度讨论了最致密的分离白矮星（WD）双星SDSS J065133.33+284423.3的发现。该系统也是天基引力波探测器、改进型激光干涉仪空间天线（eLISA）的验证源，后者将观测具有$P_{orb}\lesssim 5$小时的短周期致密银河双星。我们解决的前景做潮汐研究使用eLISA二进制显示的轨道衰变率和衰变率的分数不确定性，$\dot{f}, \ddot{f}$预期从GW和EM数据的一些高$f$二进制。我们发现，$\dot{f}$和$\ddot{f}$可以测量使用GW数据，只有在高频率观测到的最大规模的WD二进制文件。通过对$\sim 10$年日食的计时，我们发现J 0651年的$\dot{f}$可以被$\sim 0.1% $所知。我们发现，仅从GW数据，测量潮汐的影响，在二进制是（几乎）不可能的。我们还调查了改进的知识的二进制参数结合GW振幅和倾角与EM数据有和没有$\dot{f}$。在我们以前的工作中，我们发现，距离上的EM数据约束2- $σ$的啁啾质量的不确定性$15-25%$，而添加$\dot{f}$减少到$0.11%$。$\dot{f}$上的EM数据也限制了2- $σ$与$35%-19%$之间距离的不确定性。关于主质量的EM数据将次质量$m_2$限制为$\sim40%$的2倍，而添加$\dot{f}$将其减少为$25%$。最后使用单线光谱将$m_2, d$中的2- $σ$不确定性约束为2至$\sim 40%$的因子。在$\dot{f}$上添加EM数据可分别减少$\leq 25%$和$6%-19%$的这些2- $σ$不确定性。因此，我们发现，电磁测量的$\dot{f}$和径向速度将是有价值的约束二元参数。

英文摘要：

The discovery of the most compact detached white dwarf (WD) binary SDSS J065133.33+284423.3 has been discussed in terms of probing the tidal effects in white dwarfs. This system is also a verification source for the space-based gravitational wave (GW) detector, evolved Laser Interferometer Space Antenna (eLISA) which will observe short-period compact Galactic binaries with $P_{orb}\lesssim 5$ hrs. We address the prospects of doing tidal studies using eLISA binaries by showing the fractional uncertainties in the orbital decay rate and the rate of that decay, $\dot{f}, \ddot{f}$ expected from both the GW and EM data for some of the high-$f$ binaries. We find that $\dot{f}$ and $\ddot{f}$ can be measured using GW data only for the most massive WD binaries observed at high-frequencies. Form timing the eclipses for $\sim 10$ years, we find that $\dot{f}$ can be known to $\sim 0.1% $ for J0651. We find that from GW data alone, measuring the effects of tides in binaries is (almost) impossible. We also investigate the improvement in the knowledge of the binary parameters by combining GW amplitude and inclination with EM data with and without $\dot{f}$. In our previous work we found that EM data on distance constrained 2-$σ$ uncertainty in chirp mass to $15-25%$ whereas adding $\dot{f}$ reduces it to $0.11%$. EM data on $\dot{f}$ also constrains 2-$σ$ uncertainty in distance to $35%-19%$. EM data on primary mass constrains the secondary mass $m_2$ to factors of 2 to $\sim40%$ whereas adding $\dot{f}$ reduces this to $25%$. And finally using single-line spectroscopic constrains 2-$σ$ uncertainties in both the $m_2, d$ to factors of 2 to $\sim 40%$. Adding EM data on $\dot{f}$ reduces these 2-$σ$ uncertainties to $\leq 25%$ and $6%-19%$ respectively. Thus we find that EM measurements of $\dot{f}$ and radial velocity will be valuable in constraining binary parameters.

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