Corrections of rotation of the galaxy to measuredP of pulsars

Rong, Jianxiang; Xiao, Ni; Liu, Tan

doi:10.1007/bf02874265

Cited by 4 publications

(3 citation statements)

References 5 publications

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“…Finally, we note that the observed spin-down rates could be biased by other factors than GWs such as the Shklovskii effect (Shklovskii 1970), the Galactic differential rotation (Damour & Taylor 1991;Rong & Tan 1999) and acceleration toward the Galactic disk (Nice & Taylor 1995). Although the biases from the Galactic differential rotation and acceleration toward the disk would have spatial correlations in the sky, these effects are less significant (∆( p/p) 10 −19 for MSPs at 10 kpc) (Nice & Taylor 1995) and will be removed if the distance to MSPs is measured precisely in the future.…”

Section: Discussionmentioning

confidence: 92%

Constraints on ultra-low-frequency gravitational waves with statistics of pulsar spin-down rates

Kumamoto

Imasato

Yonemaru

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We probe ultra-low-frequency gravitational waves (GWs) with statistics of spin-down rates of milli-second pulsars (thereafter MSPs) by a method proposed in our prevous work (Yonemaru et al. 2016). The considered frequency range is 10 −12 Hz f GW 10 −10 Hz . The effect of such low-frequency GWs appears as a bias to spin-down rates which has a quadrupole pattern in the sky. We use the skewness of the spin-down rate distribution and the number of MSPs with negative spin-down rates to search for the bias induced by GWs. Applying this method to 149 MSPs selected from the ATNF pulsar catalog, we derive upper bounds on the time derivative of the GW amplitudes of h < 6.2 × 10 −18 sec −1 and h < 8.1 × 10 −18 sec −1 in the directions of the Galactic Center and M87, respectively. Approximating the GW amplitude as h ∼ 2π f GW h, the bounds translate into h < 3 × 10 −8 and h < 4 × 10 −8 , respectively, for f GW = 1/(1000 yr). Finally, we give the implications to possible super-massive black hole binaries at these sites.

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Section: Discussionmentioning

confidence: 92%

Constraints on ultra-low-frequency gravitational waves with statistics of pulsar spin-down rates

Kumamoto

Imasato

Yonemaru

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…We can see that the value of log 10 p/p [sec −1 ] ranges from −18.5 to −16 for "normal" MSPs. Here, we note that the observed spin-down rates are biased by various factors other than GWs: the Shklovskii effect (Shklovskii 1970), acceleration along the line of sight by gravity inside a globular cluster (Phinney 1993) and the Galactic differential rotation (Damour & Taylor 1991;Rong et al 1999), acceleration toward the Galactic disk (Nice & Taylor 1995) and low-frequency components of "pulsar timing noise" (or "red noise") often approximated as a power law of the form S( f ) ∝ f −λ , where λ 1 is the noise index (Kopeikin 1999;Kopeikin & Potapov 2004). Although the biases from the Galactic differential rotation and acceleration toward the disk could have spatial correlations in the sky, these effects are less significant (∆( p/p) 10 −19 for MSPs at 10 kpc) (Nice & Taylor 1995) and will be removed if the distance to MSPs is measured precisely in the future.…”

Section: Detection Principlementioning

confidence: 89%

Sensitivity of new detection method for ultra-low frequency gravitational waves with pulsar spin-down rate statistics

Yonemaru,

Kumamoto,

Takahashi

et al. 2017

Preprint

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A new detection method for ultra-low frequency gravitational waves (GWs) with a frequency much lower than the observational range of pulsar timing arrays (PTAs) was suggested in Yonemaru et al. (2016). In the PTA analysis, ultra-low frequency GWs ( 10 −10 Hz) which evolve just linearly during the observation time span are absorbed by the pulsar spin-down rates since both have the same effect on the pulse arrival time. Therefore, such GWs cannot be detected by the conventional method of PTAs. However, the bias on the observed spin-down rates depends on relative direction of a pulsar and GW source and shows a quadrupole pattern in the sky. Thus, if we divide the pulsars according to the position in the sky and see the difference in the statistics of the spin-down rates, ultra-low frequency GWs from a single source can be detected. In this paper, we evaluate the potential of this method by Monte-Carlo simulations and estimate the sensitivity, considering only the "Earth term" while the "pulsar term" acts like random noise for GW frequencies 10 −13 − 10 −10 Hz. We find that with 3,000 milli-second pulsars, which are expected to be discovered by a future survey with the Square Kilometre Array, GWs with the derivative of amplitude of about 3 × 10 −19 s −1 can in principle be detected. Implications for possible supermassive binary black holes in Sgr * and M87 are also given.

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“…Here, MSPs in globular clusters are excluded because they are biased significantly by the gravitational potential and complicated dynamics inside the cluster. Further, the observed spin-down rates are affected by Shklovskii effect (Shkloviskii 1970) and acceleration along the sight by the Galactic differential rotation (Damour & Taylor 1991;Rong et al 1999) other than GWs. However, such effects do not have spatial correlations in the sky and do not affect our analysis below.…”

Section: Detection Principlementioning

confidence: 99%

Detailed study of detection method for ultralow frequency gravitational waves with pulsar spin-down rate statistics

Hisano

Yonemaru

Kumamoto

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A new detection method for gravitational waves (GWs) with ultra-low frequencies ( f GW 10 −10 Hz), which is much lower than the range of pulsar timing arrays (PTAs), was proposed in Yonemaru et al. (2016). This method utilizes the statistical properties of spin-down rates of milli-second pulsars (MSPs) and the sensitivity was evaluated in Yonemaru et al. (2018). There, some simplifying assumptions, such as neglect of the "pulsar term" and spatially uniform distribution of MSPs, were adopted and the sensitivity on the time derivative of GW amplitude was estimated to be 10 −19 s −1 independent of the direction, polarization and frequency of GWs. In this paper, extending the previous analysis, realistic simulations are performed to evaluate the sensitivity more reasonably. We adopt a model of 3-dimensional pulsar distribution in our Galaxy and take the pulsar term into account. As a result, we obtain expected sensitivity as a function of the direction, polarization and frequency of GWs. The dependence on GW frequency is particularly significant and the sensitivity becomes worse by a few orders for < 10 −12 Hz compared to the previous estimates.

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Corrections of rotation of the galaxy to measuredP of pulsars

Cited by 4 publications

References 5 publications

Constraints on ultra-low-frequency gravitational waves with statistics of pulsar spin-down rates

Constraints on ultra-low-frequency gravitational waves with statistics of pulsar spin-down rates

Sensitivity of new detection method for ultra-low frequency gravitational waves with pulsar spin-down rate statistics

Detailed study of detection method for ultralow frequency gravitational waves with pulsar spin-down rate statistics

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