Measuring the properties of f−mode oscillations of a protoneutron star by third-generation gravitational-wave detectors
Measuring the properties of f−mode oscillations of a protoneutron star by third-generation gravitational-wave detectors
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DOI：
10.1103/physrevd.107.123005
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发表时间：
2023-04
影响因子：
5
通讯作者：
Chaitanya Afle;S. Kundu;Jenna Cammerino;E. Coughlin;Duncan A. Brown;D. Vartanyan;A. Burrows
中科院分区：
文献类型：
--
作者：
Chaitanya Afle;S. Kundu;Jenna Cammerino;E. Coughlin;Duncan A. Brown;D. Vartanyan;A. Burrows
核心坍缩超新星是可以被第三代引力波探测器探测到的引力波的天体物理来源之一。在这里，我们分析的引力波应变信号从二维和三维模拟的核心塌陷超新星产生的代码F{\sc{ornax}}。二维模拟的子集在芯反弹处具有非零芯旋转。时变四极矩的一个主要来源是原中子星星的l=2基模振荡。从引力波应变的时频频谱图中我们可以看到，从地核反弹后400毫秒开始，大部分的能量位于一个狭窄的轨道内，代表了f-模振荡的频率演化。从质子中子星星的角平均轮廓的线性微扰分析得到的f-模频率证实了我们在引力波信号的频谱图中观察到的。利用第三代引力波探测器观测到的超新星信号，研究了质子中子星星的$f-$模频率演化的可测性。对频率演化的测量可以揭示原中子星的质量、半径和密度等信息。我们发现，如果第三代探测器在10千秒差距内观测到超新星，我们可以测量这些频率的精度在90%以内。我们还可以使用应变信号的频谱图数据来测量基$f-$模式中发射的能量。我们发现，在$f-$模式的能量可以测量到的信号的宇宙探测器使用模拟与成功的爆炸，假设源的距离在10千秒差距内的误差在20%以内。
Core-collapse supernovae are among the astrophysical sources of gravitational waves that could be detected by third-generation gravitational-wave detectors. Here, we analyze the gravitational-wave strain signals from two- and three-dimensional simulations of core-collapse supernovae generated using the code F{\sc{ornax}}. A subset of the two-dimensional simulations has non-zero core rotation at the core bounce. A dominant source of time changing quadrupole moment is the $l=2$ fundamental mode ($f-$ mode) oscillation of the proto-neutron star. From the time-frequency spectrogram of the gravitational-wave strain we see that, starting $\sim 400$ ms after the core bounce, most of the power lies within a narrow track that represents the frequency evolution of the $f-$mode oscillations. The $f-$mode frequencies obtained from linear perturbation analysis of the angle-averaged profile of the protoneutron star corroborate what we observe in the spectrograms of the gravitational-wave signal. We explore the measurability of the $f-$mode frequency evolution of protoneutron star for a supernova signal observed in the third-generation gravitational-wave detectors. Measurement of the frequency evolution can reveal information about the masses, radii, and densities of the proto-neutron stars. We find that if the third generation detectors observe a supernova within 10 kpc, we can measure these frequencies to within $\sim$90\% accuracy. We can also measure the energy emitted in the fundamental $f-$mode using the spectrogram data of the strain signal. We find that the energy in the $f-$mode can be measured to within 20\% error for signals observed by Cosmic Explorer using simulations with successful explosion, assuming source distances within 10 kpc.