论文标题
8.8分钟的轨道时期黯然失色的双白色矮人二进制
An 8.8 minute orbital period eclipsing detached double white dwarf binary
论文作者
论文摘要
我们报告了ZTF J2243+5242的发现，这是一种黯然失色的双白矮人二进制，轨道时期仅为$ 8.8 $分钟，这是第二个已知的eclips二进制二进制，轨道时期少于十分钟。该系统可能由两个低质量的白色矮人组成，并将在大约400，000年内合并，形成一个孤立的热分布或R Coronae Borealis Star。就像它的$ 6.91 \，\ rm min $对应物一样，ZTF J1539+5027，ZTF J2243+5242将是可通过太空引力波检测器检测到的最强的引力波源之一，激光空间空间扰动计（LISA）是强度频率的频率，因为它的重力频率降低了lisa的峰值。基于其$ d = 2120^{+131} _ { - 115} \，\ rm PC $的估计距离，Lisa应在操作的前几个月内检测到源，并应达到四年后的信噪比为87美元\ pm5 $。我们发现$ m_a = 0.349^{+0.093} _ { - 0.074} \，m_ \ odot $和$ m_b = 0.384^{+0.114} _ { - 0.074} $ r_a = 0.0308^{+0.0026} _ { - 0.0025} \，r_ \ odot $和$ r_b = 0.0291^{+0.0032} _ { - 0.0024} $ t_a = 22200^{+1800} _ { - 1600} \，\ rm k $和$ t_b = 16200^{+1200} _ { - 1000} \，\ rm k $。我们仅使用光度测量值确定了所有这些属性，以及与该系统的距离，证明了一种可行的方法来估算大量的光学微弱（$> 21 \，m _ {\ rm ab} $）重力 - 重力源，即Vera Rubin observatoration（Vro）和LISA应识别。
We report the discovery of ZTF J2243+5242, an eclipsing double white dwarf binary with an orbital period of just $8.8$ minutes, the second known eclipsing binary with an orbital period less than ten minutes. The system likely consists of two low-mass white dwarfs, and will merge in approximately 400,000 years to form either an isolated hot subdwarf or an R Coronae Borealis star. Like its $6.91\, \rm min$ counterpart, ZTF J1539+5027, ZTF J2243+5242 will be among the strongest gravitational wave sources detectable by the space-based gravitational-wave detector The Laser Space Interferometer Antenna (LISA) because its gravitational-wave frequency falls near the peak of LISA's sensitivity. Based on its estimated distance of $d=2120^{+131}_{-115}\,\rm pc$, LISA should detect the source within its first few months of operation, and should achieve a signal-to-noise ratio of $87\pm5$ after four years. We find component masses of $M_A= 0.349^{+0.093}_{-0.074}\,M_\odot$ and $M_B=0.384^{+0.114}_{-0.074}\,M_\odot$, radii of $R_A=0.0308^{+0.0026}_{-0.0025}\,R_\odot$ and $R_B = 0.0291^{+0.0032}_{-0.0024}\,R_\odot$, and effective temperatures of $T_A=22200^{+1800}_{-1600}\,\rm K$ and $T_B=16200^{+1200}_{-1000}\,\rm K$. We determined all of these properties, and the distance to this system, using only photometric measurements, demonstrating a feasible way to estimate parameters for the large population of optically faint ($r>21 \, m_{\rm AB}$) gravitational-wave sources which the Vera Rubin Observatory (VRO) and LISA should identify.
